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EXCLUSIVE: UBS Works on Employee Overpayment ErrorsPayroll processing company ADP says it erred in administering a “recurring loans program” at UBS Wealth Management U.S.A., and has reached a resolution with the firm.
UBS Brokers Reunite at Baird with Teammate Discharged over Client MailingFour brokers had worked together at UBS and predecessor firms before one was discharged from UBS in February over allegations of an unapproved mailing to clients.
JPMorgan’s Wealth Target: 6,500 Advisors by Year-EndBank CEO Jamie Dimon writes in annual report that the bank will add advisors across private banking, brokerage and mass-affluent channels to gain market share.
Most-read articles from July 9 through 14.
Most-read articles from May 14 to 19.


text: Find AFS2, 3138, GGG-B-001222-TY1CL2, B107-10M, 1680002P1 by aircraft manufacturer Gray Forgings And Stampings Ltd of CAGE Code 08486. We provide aviation parts from top-class manufacturers. Visit now!

industry_corpus2: Aerospace


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The veneration of Our Lady leaves its mark on every aspect of Carmelite life, since the very first hermits of our Order dedicated to her their little chapel on Mt. Carmel. The Order of Carmel considers Our Lady as its Patroness and its Queen. It is “the Order of the Virgin, our houses belong to her.” They are the “dovecotes of the Virgin.” The motherly presence of Our Lady among us penetrates all of our Carmelite vocation. This Marian dependence is expressed in a general manner of living, more or less accented according to the graces given to each, as well as in various community and personal devotions.
Mary is taken as a model of the contemplative life, especially in her hidden and meditative aspects, her faith, her charity and her loving participation in the mystery of Redemption. She is the perfect realization of our ideal. She illumines our steps and is the eminent example of our communal life in the Church.
“Always moved by the Holy Spirit,” she is the sure way to arrive at mystical union and marks with a particular stamp our sisterly communion and our whole life.
Like Our Blessed Lady in the Upper Room, who, by her prayerful presence, kept in her heart the origins of the Church, we want to carry in our loving hearts and in our praying hands the journey of the Church.

industry_corpus2: Others


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Duke University announced on Aug. 6 that it will acquire the papers of Rabbi Abraham Joshua Heschel.
Heschel was a highly visible and charismatic leader in the civil rights and anti-Vietnam War movements. He co-founded Clergy Concerned About Vietnam and served as a Jewish liaison with the Vatican during the Second Vatican Council, also known as Vatican II.
The collection, which has never before been available to scholars, consists of manuscripts, correspondence, publications, documents and photographs spanning five decades and at least four languages. Included among the papers are notes and drafts for nearly all of Heschel’s published works, as well as intimate and extensive correspondence with some of the leading religious figures of his time, including Martin Buber, Thomas Merton, Eugen Rosenstock-Huessy and Reinhold Niebuhr.
The papers also contain extensive documentation on Heschel’s life-long commitment to social justice, including planning documents, correspondence with organizers, speeches and even hate mail.
The archive will open for research after conservation review and archival processing are complete. The opening will be announced on the websites of the David M. Rubenstein Rare Book & Manuscript Library and the Center for Jewish Studies at Duke, which are partnering to acquire the papers.
“The acquisition of the Heschel papers assures scholars that the legacy of social activism, human rights and the highest standards of Judaic scholarship will be central to the pursuit of Jewish studies at Duke and many other places,” said Eric Meyers, the Bernice & Morton Lerner professor of religion and director of the Duke Center for Jewish Studies.
Rabbi Marshall Meyer, whose papers are already placed at the archive, was a student of Heschel’s and credited him with profoundly influencing his human rights work in Argentina.
“Together, these two collections represent almost a century of social justice thought and action and provide an important connection between the civil rights and human rights movements,” said Patrick Stawski, human rights archivist at the Rubenstein Library.
Heschel’s theological works include “The Sabbath” (1951), “Man is Not Alone” (1951) and “God in Search of Man” (1955). His writings continue to influence contemporary discussions of religion and social justice.

industry_corpus2: Subject Education


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Frank Festen is the country manager for Germany, Austria and Switzerland at Content Stadium. For ‘FUSSBALL BUSINESS‘ he speaks about social media in sports: the importance of it, the perfect strategy, the right content and more.
How important is social media for clubs and leagues – and why are they important?
Social media is the closest fans can get to the team and the players, after attending live games and events. Therefore social media plays a significant role in the overall sports branding experience. The demand from the fans is high and increasing fast. The clubs and other sports organisation have the challenging opportunity to fulfil this need. Some organisations even go beyond these fan-expectations and deliver a full fan-experience via social media. In comparison, TV-reach is still significant, but there is no interaction; you can not instantly like or share your favourite goal, player, trick or quote with your friends. Social media is taking over fast.
Which social media channel would you recommend clubs to use?
This depends on how big your team and reach is. What we see is that there is a big difference in focus between clubs, even at more prominent sports organisations. With a smaller social media team, you should focus on the three leading networks. And prioritise these on your fanbase (target audience). If these channels are well taken care of, you can include more channels in the mix. Maybe even try new ones. New networks and communities are being built every day, so always keep an eye open for innovation.
What are you offering to make the work easier?
Our product is a software as a service platform. We empower editorial teams of sports organisations to instantly create and publish sports visuals, animations and videos for social media. So, we support the social media teams in generating better, branded, visual content, in less time. This means that the same group of people can produce more engaging content.
What are fans and followers expecting from social media profiles of clubs and leagues?
Like I mentioned before; demand is high, and fans are expecting a lot. They expect to be taken seriously, also on social media. Nowadays fans wait to get all kinds of information in their feed from the clubs and leagues that they follow. Not only nice pictures but live coverage, statistics, behind-the-scenes-footage as well as other entertaining content. As a club, you want to make sure that you’re the first to communicate any update, news-flash or additional information about your club. Social Media fans do not wait for tomorrows newspaper; they want to consume content real-time!
In sports, that is easy to define: a good social profile puts fans first. No matter if you have a big budget or no budget at all, this is something everyone can do. Yes, maybe you want more traffic to your website, perhaps you want to sell more shirts online, all that is possible, but the experience of the fan should be the primary focus, throughout your channels. On the other hand, you have the sponsors, who are also expecting more from your social media channels. Branding, continuity and cross-channel posts are essential here, for the visibility of your sponsor.
I would say you must have a long-term-strategy but also need to be able to react quickly to trends and things that happened recently. Is this the basic requirement for good social media work?
Yes, of course, you need a strategy. Social media is too big to go with the flow. The strategy is your foundation and can differ per channel. Secondly, you need to make sure that you are preparing for what is coming next, that includes; live coverage, news, trends and virality (remember the cat at FC Bayern?). Look at it like this, you don’t know if your team will score a goal, but when they do, you have your social-team and tech-set-up ready to communicate it with your fans, as soon as possible, in any language needed and in such a way that fans feel invited for interaction and engagement.
What content is the “most valuable” on Facebook, Instagram and others?
From a sports business perspective, content with the highest engagement-ratio is the most valuable. These are the likes, the comments, the shares, the times that videos are viewed and the interactions on your shared content. These things count for social media algorithms. The more your content is shared, the more fans will start following your pages. Video content is the primary driver for growth. Already in 2016 Facebook announced that within five years they would mostly be a video-network. Video content has 1200% more shares, so it’s about time to start investing in qualitative videos that make your club stand out from the crowd, without losing your identity and branding. Because, since you own your social media pages, all these engaging fans are a tremendous and very valuable asset to your company.
You have the insights: which of your content gets the most attention/interaction?
It’s good to clarify that Content Stadium doesn’t own any content, the clubs do. We design and build templates, which your social media team can use on our platform – without a frequency cap and 24/7 access – to create content. We see a lot of different content getting a lot of interaction. Sports is emotion. Therefore a regular post, with a match result, for example, can double or triple in engagement due to an unexpected big-win (or loss). Of course, some graphics always tend to get more interaction than others. We help our clubs and companies with identifying this potential when we define the right templates for their social media strategy.
This interview first appeared in the newsletter of ‘FUSSBALL BUSINESS Magazin’. Click here to read it.
FUSSBALL BUSINESS is a magazine for football and business for the German-speaking countries. The magazine is addressed to deciders and opinion leaders in football-business and football-near business as well as to deciders in companies, agencies, associations and also to sports marketing students. Besides the magazine, FUSSBALL BUSINESS is publishing a weekly football-business-newsletter and organizes football-business-events, like the Big Data in Football-Conference in Graz, Austria.

industry_corpus2: Sports


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City is the administrative center of Oryol Oblast. . Total area of the city is 127.8 km2 . It has a population of 317,747 people.
It is the 57th largest city in terms of population. City is located near Oka River. It is nearly 226 miles distant from Moscow city.
The city was officially founded in 1566. The old city fortress was built in early 12th century. By 15th century, people started to move here. Soon, it became one of the important grain producing city of Russia.
This city has temperate climatic conditions. The summers become as hot as the peak temperature reaches to 40 C in the month of July. And even reaches to -38C in the peak winter season of December and January.
Oryol State University and Orel State Technical University are the main educational institutes of the city.
Machine and metal industry is the backbone of economy of this city. The area is also known for its productions of different agricultural products like wheat, oats , potatoes, barleys and many other grains. It is among the largest milk producing cities of Russia.
The city will amaze you with lot of its catchy sights. Place like Catherine's Cathedral, Orlik River, Duchy Park , Turgenev State Memorial and Nature Museum Preserve are very famous among the tourists.
City is famous because of its beautiful buildings, city structure and old churches.

industry_corpus2: Agriculture & Fisheries


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The U.S. Department of Justice has repealed a policy seen as being lax on antitrust violations, signaling a more aggressive approach toward antitrust enforcement under the administration of U.S. President Barack Obama.
The DOJ's Antitrust Division has withdrawn a September report that "raised too many hurdles to government antitrust enforcement and favored extreme caution" toward antitrust enforcement action, the DOJ said. The change in policy could mean that the DOJ looks harder at the actions of technology vendors such as Google, Oracle and IBM, as detractors have raised antitrust concerns about all three in recent months.
Christine Varney, assistant attorney general in charge of the Antitrust Division, said her comments, made during a speech Monday, weren't directed at any one company. She did say, however, that the DOJ should take close looks at the high-tech and Internet industries and new ways of measuring antitrust activity there. Varney also said the DOJ would look hard at mergers and their impact on competition.
"Withdrawing the ... report is a shift in philosophy and the clearest way to let everyone know that the Antitrust Division will be aggressively pursuing cases where monopolists try to use their dominance in the marketplace to stifle competition and harm consumers," Varney said during a speech. "The division will return to tried-and-true case law and Supreme Court precedent in enforcing the antitrust laws."
Spokesmen with Google and Intel declined to comment on the change in policy. The U.S. Federal Trade Commission has an open antitrust investigation of Intel and the DOJ's change in policy wouldn't affect that.
In recent months, several detractors have raised concerns that Google has a near monopoly in online search advertising. In late 2008, the DOJ's concerns over a proposed advertising partnership between Google and Yahoo killed the deal.
Google recently has been meeting with lawmakers, journalists and others in an effort to explain its positions on business competition. Google's main message has been that competition with the search giant is "one click away."
"As Google has grown, the company has naturally faced more scrutiny about our business principles and practices," Adam Kovacevich, senior manager for Google's global communications and public affairs, wrote on the Google public policy blog Friday. "We believe that Google promotes competition and openness online, but we haven't always done a good job telling our story."
An antitrust expert at Boston University questioned the DOJ's decision. It's no surprise that the Obama administration would take a different approach than former President George Bush's administration, said antitrust expert Professor Keith Hylton.
Varney talked about cartels and price-fixing and praised the DOJ for working hard on those types of issues. There are a handful of industries where cartels still exist because of "powerful interest groups," and new actions against those industries would be welcome, Hylton said.
But in most industries, a more aggressive approach may not be needed, he said. "Opening up the doors (or opening the doors wider) of the Department of Justice to complaints from firms against their rivals will encourage a different form of interest-group politics," he wrote in an e-mail.
The change in policy may mean that tech companies will have to look hard at mergers before going through with them, added Bruce McDonald, a lawyer with the Jones Day law firm, and former deputy assistant attorney general in the DOJ's Antitrust Division. High-tech and other companies may be more reluctant to go through with mergers, even though only a handful of merger cases ever lead to DOJ enforcement actions, he said.
With Varney signaling that the DOJ will look at new ways to measure antitrust behavior in tech industries, the DOJ will be a "little less predictable," McDonald said.
"You very likely will see new enforcement actions," he added.
Varney's decision could mostly shift antitrust enforcement back to standards that were long recognized before the Bush administration's changes late last year, added Steve Newborn, an antitrust lawyer with the Weil, Gotshal & Manges law firm. But companies with dominant positions in their markets, including Google, should be careful as they watch the new policies play out, he said.
"The rules have changed," he said.
The Computer & Communications Industry Association, a trade group that supports stronger antitrust enforcement, praised the policy shift. "It's clear we have a new sheriff in town," said Ed Black, the group's president and CEO. "There's so much that was left ignored by the last administration, so a main job will be catching up."
Varney's announcement suggests the U.S. intends to return to the "main track" of antitrust enforcement and operate in parallel with the European Union, Black said in an e-mail. It appears as if the DOJ is "going to be aggressive, but careful, and I think that's going to be an appropriate balance," he said.

industry_corpus2: Law & Justice


text: We are excited to offer this 2019 Honda CR-V. Want more room? Want more style? This Honda CR-V is the vehicle for you. Save money at the pump with this fuel-sipping Honda CR-V. You can finally stop searching... You've found the one you've been looking for. You've found the one you've been looking for. Your dream car. We look forward to seeing you soon! Please call us for more information.

industry_corpus2: Automobiles


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Get your prefabricated houses in bogota (casas prefabricadas en bogota).
It is no secret that currently Prefabricated houses (casas prefabricadas) any quite desirable alternative to conventional houses, this is a industry that has been several years in development and also in fact, prefabricated houses in bogota (casas prefabricadas en bogota) it is likely that in the particular not too distant future these types of will reach completely alter the style and even the lifestyles of the people who make use of it.
So why are they gaining such popularity? Well consider the prices, the Prefabricated houses (casas prefabricadas) can usually be much cheaper than the original houses, besides the moment that you would help save when creating them, that’s, the simplest types of these houses can arrive being built in merely 3 months, for you to never use a traditional residence, unless you have large sums of cash to pay development and labor costs. This type of houses also allow a better file format, since these tend to be modular models can always be added more should you desire, and especially the most important, security, these houses are at the mercy of many more regulations than standard houses so that you will have got far much less problems to concern yourself with.
If you want to help make your own prefabricated nation houses (casas prefabricadas campestres) you can key in https: //abcasalista.com and acquire in touch using the relevant group to perform this work. Here you can find the best Prefabricated houses (casas prefabricadas) as well as anywhere in the country if you wish, In Abdominal Casalista have a wide selection of models and also prefabricated housing programs that will be your complete fingertips.
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industry_corpus2: Real Estate & Construction


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For London HulaFit classes please read below for information & booking. Please go to our ‘Instructor’ page for other classes provided by our teachers around London. Hoops are provided at class. All abilities are welcome!
Hoops Provided. All abilities Welcome.
Participation in a HulaFit class is taken at the individuals own risk of injury or loss. If you are pregnant or you have any medical concerns regarding hula hooping for fitness, please contact a medical professional prior to attending a class. We do use weighted hoops which can cause bruising, this is not permanent or internally damaging but may cause some discomfort to the individual. Classes are suitable for ages 16yrs and older.
Every attendee will receive a loyalty card which, after 10 classes you will receive a FREE class. To claim your free class, please contact us at hulafituk@gmail.com and we can add your name to your chosen class.
The information provided by this website is based on experiences of current and past instructors and class participants. This is not saying everyone will benefit from the same results. There are many factors that can affect weight loss and fitness results. We can make no guarantee that individuals attending HulaFit classes will achieve the same results. The views and opinions in the testimonials on the website are solely of those clients. Your experience with HulaFit may be different.
Every effort is made to keep the website up and running smoothly. However, HulaFit, takes no responsibility for, and will not be liable for, the website being temporarily unavailable due to technical issues beyond our control.


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Icy cold Snowcones and tantalising fairy floss are favourite treat for many kids, and our freshly made hot popcorn is so popular with any child young or old. For all your soft serve ice cream requirements which include the traditional choc tops, sprinkle cones, sherbert cones and our very popular nut sundaes with your favourite toppings. We also have waffle cones, milk shakes and thick shakes. We are available for School fetes, Street fairs, Bithday parties, Xmas parties in fact any type of event, large or small.
Delights for every occasion! Makers of traditional continental cakes, biscuits, gelati, foccacia & pizzettes. From birthday tortes to fantastic wedding cakes. Just give us a ring!
Best Gelati & Sorbets in South Australia. All Gluten-free. Pure Authentic Gelati & Sorbets made with real ingredients, not artificial stuff. Vegan and Dairy-free Sorbet. Certified by the Dairy Authority of South Australia. Wholesale. Supply schools and events. Free home delivery of take away packs.
FRITZ GELATO is award winning, organic, Italian style ice cream. Our gelato is based on traditional recipes with modern influences. We pride ourselves on using the best fresh quality ingredients, eliminating the need for artificial flavours and colours.
GELATO MANIA is award winning,authentic Italian ice cream & sorbets. Our gelato is based on traditional recipes with modern influences. We pride ourselves on using the best fresh quality ingredients, eliminating the need for artificial flavours and colours.
Lick Me is a premium consumer brand of ice cream produced by the Gourmet Ice Cream Factory in Camberwell, Victoria.
Lick Me represents the essence of a traditional European ice cream recipe that has been nurtured by three generations. This cultural inheritance has resulted in the creation of the most natural and exclusive ice cream in Australia.
Lick Me ice cream has won many gold medals at the Dairy Industry Association National Awards as well as Dairy Australia's grand dairy Awards.
With a commitment to all natural products (no artificial colours or artificial flavours) and the use of only the freshest ingredients, The Gourmet Ice Cream Factory is proud to promote Lick Me Ice Cream.
We are now delivering ice cream cakes and our premium brand, gold medal winning Lick Me Ice Cream. You can choose your cake from many different flavours with various designs and characters available. These cakes can also be personalized.
Delivery of our premium brand Lick Me ice cream in tubs has never been so easy!
We have SoftServe, Gelato, Juices, Smoothies, Fairy Floss. We Cater For ALL EVENTS: Corporate Events, Private Parties, Xmas Parties, Schools, Fetes, Fundraising, Childrens Parties, Shows, Festivals, Sporting Events, Markets.

industry_corpus2: Hospitality & Catering


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Ernesto Paz, director of the Miss Peru Organization has chosen the country's official representative for Miss Universe and Miss World 2012 pageants. The beauty queens were crowned at the Santiago de Surco's Parque de la Amistad in Lima.
Giuliana Myriam Zevallos Roncagliolo was chosen as Miss Peru Mundo or Miss Peru World. She will compete in Miss World 2012 contest to be held on August 18 in Ordos, Inner Mongolia in China.
23 year old Giuliana Myriam Zevallos Roncagliolo from Lima stands 1.80m tall.
Nicole Faveron Vasquez was selected as Miss Peru Universo or Miss Peru Universe. She will enter the Miss Universe 2012 pageant later this year.
22 year old Nicole Faveron Vasquez from Iquitos stands 1.83m tall.

industry_corpus2: Film & Entertainment


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Here’s the latest news about women in theater and film.
The Good News: Pulitzer Prize winning playwrights Paula Vogel (left) and Lynn Nottage (right) bow on Broadway with Indecent and Sweat, respectively. Read the full article at Playbill.com. The Bad News: Only three 2016-2017 Broadway plays, including these two, were written by women.
Terrific Read: Leah Nanako Winkler spoke to the Los Angeles Times about her play Kentucky, “the angry playwright label” and the intersection of race, class and gender.
ICYMI, Part 1: Guardian article features Dame Harriet Walter’s plea for better roles for women on stage.
ICYMI, Part 2: Scott Mendelson wrote a searing article in Forbes about women film directors needing opportunity. The best way to address the dearth of female-directed feature films: hire women. Simple as that.
Opportunity: “BRIClab is a commissioning and residency development program for Brooklyn and New York City-based artists to explore and expand the possibilities of their work in music, dance, theater and multi-disciplinary performance.” Application Deadline: January 17, 2017. Apply at BRIC’s website.
This entry was posted on December 6, 2016 by worksbywomen in Broadway, Film, Theater, Women and tagged briclab, dame harriet walter, Forbes, leah nanako winkler, Lynn Nottage, Paula Vogel.


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It is by now a familiar story: while traders are experiencing some of the toughest ever conditions on the high street, online sales are growing exponentially. As the penetration of high-speed broadband continues at a pace across the world, the online shopping experience is growing in sophistication and being boosted by the massive popularity in smartphone and tablet devices. It is little surprise, therefore, that analysts are predicting a boom for online retail. Forrester, one of the leading analyst houses, has forecast that there will be 190 million Europeans shopping online by 2014, up on the 141 million we see today. It seems clearer than ever that the future of retail will be founded on the online world.
However, what is also becoming clear is that there will not be a simple dichotomy between online and offline retail. The fact of the matter is that consumers are increasingly opting for a multichannel approach to retail. The devices they use to shop online will vary. One day they might sit at their laptop and buy from an online marketplace; then next they may surf a reviews site on their mobile before making a purchase; on another day they may visit a bricks-and-mortar retail outlet to redeem a gift voucher they received online. Today’s shopping environment is one that increasingly crosses the boundaries between the off and online worlds, and also one that consumers want to access 24/7. This new approach to shopping has presented retailers with a range of new channels for communicating with customers, ones that have a global reach and if used effectively will help them win business and build brand loyalty.
Before the high street came to prominence in the 19th century, shopping took place in the local marketplaces that dotted the towns and villages of the world. Today we are seeing a return to the marketplace, but unlike its predecessors today’s marketplaces are global and digital. In 2011, Rakuten conducted a survey which threw into sharp relief just how popular online global marketplaces have become. Shoppers in Brazil were the fondest of the international marketplace model, with 81 per cent of consumers keen to shop on different online markets. Indonesia (77%), Thailand (74%), China (69%) and Spain (66%) were close behind, and demonstrated that the online marketplace is appealing to consumers regardless of the cultural and political environments they come from.
These results were also significant as they have provided retailers with a route into new and emerging markets, demonstrating that online marketplaces and affiliate marketing models represent a simple means of targeting a truly global audience. At a stroke, retailers can globalise without needing to invest in the capital expenditures usually associated with internationalisation, such as establishing local delivery models or buying local storage facilities. Instead, retailers will be able to establish a presence through local marketplaces, and easily scale their presence according to demand.
The penetration of smartphones has sparked a revolution in ecommerce, providing retailers with a web-enabled platform that reaches to the consumer with greater immediacy than any other channel. Over the course of 2010 and 2011, marketers started looking at the full potential that mobile devices could offer, and new services such as location-based marketing and QR codes began to come into play. This is just the beginning however. While browsing on smartphones has increased month by month, the sales conversion rate has lagged behind. As we move into the second half of 2012, we expect to see more of a push from retailers to change this state of affairs. Key to this will be innovation in the mobile payments space. The easier and more secure it is to buy goods over the mobile, the greater sales conversion will become. All the evidence from this year’s Mobile World Congress suggests that we are on the verge of solving the problem of mobile payments, and when this happens we expect to see the mobile become one of the most important sales channels.
Any mobile strategy today cannot be limited to smartphones, however. Tablets provide an engaging visual browsing and buying experience for consumers, and great importance should be placed on developing a strong t-commerce strategy. The rich functionality of the tablet shifts the traditionally transactional and bargain hunting online experience into a virtual store experience. Given the convenience and quality browsing experience delivered by tablets, we expect to see e-commerce growth driven by tablet devices. To make the most of the tactile nature of the tablet, marketers and retailers must look to optimise their web pages for use on these devices, and ensure that all content is as engaging as possible. After all, the more time a consumer spends on your site, the more likely they are to buy something.
Many people treat offline shopping as a highly social experience, taking their friends and family with them to advise on good buys and provide recommendations. We are now seeing this being replicated in the online world. Instead of bringing a few friends shopping, however, consumers are increasingly able to call on their entire social network for retail advice. Social media can offer much more than this, however, delivering retailers with tools for product development and customer service. For a marketplace to be truly social, they need to enable members to be able to invite friends to view products and live chat while looking at the website. This will deliver the social element of shopping that is such an important part of the traditional offline markets.
The great changes that are taking place in how consumers shop cannot be overstated. We are moving towards a multichannel environment where consumers will interact with brands and ultimately make a purchase from a variety of platforms. The marketplace will play an increasingly important role in this change, offering retailers with an easy way to create feature-rich multi-platform strategies across whichever markets they wish to operate in. Before long, we will have an online market where shopping is a communal and social experience, and brands are marketed to individuals in a highly personalised and relevant manner.

industry_corpus2: Computing & Telecommunications


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It was the world's first fully Arabic-themed browser-based massively multiplayer online (MMO) game and now, with its debut in the App Store, "Knights of Glory" has also become the first Arabic MMO app available for the iPhone.
Available to download as a paid app, Knights of Glory substitutes some of the now clichéd character types and historical settings familiar to MMO gaming fans with warring sultans in command of medieval armies all set against a historically accurate Middle Eastern backdrop.
Produced by Falafel Games, the browser version has proven a massive hit since its launch in 2011 and won the Readers' Award for the Best Arabic Browser Game of 2012 by ArabMMO.
The game's creators say that their decision to create the original version of "Knights of Glory" was a direct response to what they saw as a lack of existing games aimed at the Arabic world. The release for mobile is solely based on user demand. Before they were inundated with requests, they couldn't see any potential in MMO games optimized for smartphones or tablets.
So, if you're a gamer who prefers role play to single person shooters and is tired of playing the character of an elf or a pixie or an Arthurian knight, then "Knights of Glory" could be for you. Although it is a premium title, Falafel Games is offering a try before you buy service for early adopters.

industry_corpus2: Gaming


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Blue stragglers (BS) are usually defined as objects brighter and bluer than the main-sequence turn-off point of their host cluster (Sandage 1953). In the color−magnitude diagram (CMD) they occupy an extension of the main sequence (MS), from which all normal stars at the age of the cluster would have evolved billions of years ago. In other words, they indeed seem to lag in time, or straggle, behind the bulk of the cluster (Shara et al. 1997). Their location in the CMD suggests typical masses of 1.0−1.5 M⊙− significantly larger than those of normal stars in globular clusters (GC). Because of this, BSs are thought to have increased their mass during their evolution. Two basic ideas have been proposed to explain the origin of these objects: direct stellar collisions (Hills & Day 1976), and mass transfer between or coalescence of the components of binary systems (McCrea 1964; Chen & Han 2008, and references therein) forming, respectively, collisional and evolutionary BSs. The role of each of these scenarios in producing the observed BS populations is still debated (Ferraro et al. 2012, and references therein; Chatterjee et al. 2013; Perets 2015). It is conceivable that different intracluster environments could be responsible for different origins of BSs: in less dense clusters they would preferentially form as evolutionary mergers of, or owing to mass transfer in close binaries while, in high-density ones, from collisions during dynamical encounters between binaries and/or single stars (Chatterjee et al. 2013; Hypki & Giersz 2013).
BSs are not rare objects: every GC has been observed as hosting them, and each GC can contain from a not many up to a few hundred of them. The resulting straggler fractions range from a few times 10-5 to 10-4 (Piotto et al. 2004), however their presence in a cluster is far from insignificant. They result from the fascinating interplay between stellar evolution and stellar dynamics which drives cluster evolution (Cannon 2015) and, as such, they represent a crucial link between standard stellar evolution and internal dynamics of GCs (Ferraro et al. 2015). Thus, by studying them, the dynamical history of a cluster can be constructed, and important constraints obtained on the role played by cluster dynamics on the evolution of cluster members. BS statistics can also provide constraints on the initial distribution of binary systems (Hypki & Giersz 2013). All these factors explain why, within the last twenty years, BSs have evolved from a marginal oddity into an attractive subject of interest for at least three astronomical specialties: observers, cluster evolution modelers, and stellar/binary evolution modelers.
Observational data on which our paper is based have been collected within the Cluster AgeS Experiment (CASE) project. The main aim of CASE is to determine the basic stellar parameters (masses, luminosities, and radii) of the components of GC binaries to a precision better than 1% to measure ages and distances of their parent clusters, and to test stellar evolution models (Kaluzny et al. 2005). The best-suited objects for this type of survey are well-detached binaries so evolutionarily advanced that at least one component is about to leave (or has just left) the main sequence. A by-product of the systematic search for such systems is a wealth of cluster variables. Among the latter about 20 binary BSs have been found (Kaluzny et al. 2013a,b, 2014, 2015a, 2016) which strongly supports the mass transfer option. The aim of the present paper is to verify if a consistent evolutionary scenario can be obtained for these type of objects based on the available data.
To the best of our knowledge, the four stragglers whose evolutionary history we attempt to reconstruct are the only ones in GCs whose parameters are accurately (or at least reasonably accurately) known. In Sect. 2 we discuss their properties together with observational limits on their chemical composition and age. Section 3 briefly introduces the evolutionary code employed to follow their evolution. Section 4 presents results of the search for their progenitors. The results are discussed in Sect. 5, and the paper is summarized in Sect. 6.
The subject of the present investigation is binary blue stragglers V209/ω Cen, V60/M 55, V228/47 Tuc, and V8/NGC 6752 (hereafter: V209, V60, V228 and V8, respectively). The parameters of all the four systems (orbital period P, semi-major axis of the orbit a, component masses M1 and M2, component radii R1 and R2, effective temperatures of the components T1 and T2) are collected in Table 1, together with ages and chemical compositions or their parent clusters. We note that the quoted temperature uncertainties include the spread of color-temperature calibrations used but, accounting for discrepancies among the various calibrations, they might be increased to 250−300 K for V60 (a synthetic calibration was employed; see Rozyczka et al. 2013, for a justification) and V228 (T1 was found iteratively, and its error was difficult to estimate, see Kaluzny et al. 2007b).
V209 was discovered by Kaluzny et al. (1996) during a search for variable stars in the field of ω Centauri. The light curve exhibits total eclipses and is nearly flat between the minima, indicating a detached system. A detailed account from photometric and spectroscopic observations can be found in Kaluzny et al. (2007a), who also derive absolute parameters of the components. On the CMD of the cluster (their Fig. 8), the primary component is located at the tip of the BS region, while the much fainter (ΔV ≈ 1.5 mag) secondary approaches the hot subdwarf (sdB) domain.
In the evolutionary scenario proposed by Kaluzny et al. (2007a), V209 evolved through the common envelope (CE) phase when its original primary ascended the giant branch (RGB). The resulting angular momentum loss transformed it into a close binary with the orbital period of ~1 d, composed of a white dwarf and a main-sequence companion. The second episode of mass transfer and/or loss began once the companion entered the Hertzsprung gap. During that episode it lost most of its envelope, failing to ascend the RGB and ignite helium. Instead, it started to move nearly horizontally across the CMD toward the sdB domain. At the same time the primary accreted enough mass to ignite hydrogen in a shell. Its envelope expanded, and the former white dwarf is currently seen as the more massive and more luminous component of V209 Cen. Its companion, which consists of a helium core surrounded by a thin hydrogen shell, is now seen as the less massive and hotter component of the binary. Kaluzny et al. (2007a) admit that the chances of observing this evolutionary phase are rather low, since the primary should evolve very rapidly across the CMD, but they do not provide any alternative scenario.
V60 was discovered by Kaluzny et al. (2010). The system is a semidetached Algol with eclipses of a very different depth (ΔV ≈ 1.5 mag) whose period lengthens at a rate of 3.0 × 10-9. On the CMD, it occupies a position between the RGB and the extension of the main sequence (Fig. 5 of Kaluzny et al. 2010). Rozyczka et al. (2013) give a detailed account from photometric and spectroscopic observations, and derive absolute parameters of the components. They conclude that the present state of V60 is a result of rapid but conservative mass exchange, which the binary is still undergoing.
V228 was discovered by Kaluzny et al. (1998). The system is a semidetached Algol with partial eclipses of a significantly different depth (ΔV ≈ 0.3 mag). Kaluzny et al. (2007b) give a detailed account from photometric and spectroscopic observations, and derive absolute parameters of the components. On the CMD of 47 Tuc (their Fig. 5), the primary component is located slightly blueward of the tip of the BS region, while its companion resides close to the main sequence about ~0.5 mag above the turnoff. According to Kaluzny et al. (2007b), the secondary of V228 is burning hydrogen in a shell that surrounds a degenerate helium core, and transfers mass to the primary on a nuclear time-scale. This means that the resulting rate of period lengthening should be very low, and, indeed, their observations with a time base of 11 yr failed to reveal any change of the orbital period.
V8 was discovered by Thompson et al. (1999). The system has a W UMa-type light curve with a total secondary eclipse. Spectroscopic data were not obtained, but the duration of totality together with the amplitude of light variation enabled constraints to be imposed on mass ratio q and orbital inclination i. An account from observations is given by Kaluzny et al. (2009), who also perform a detailed analysis of the light curve. On the CMD (their Fig. 5), the primary of V8 resides at the extension of the normal main sequence, while the secondary is located far to the blue of the main-sequence (the temperatures of both components are very similar). Kaluzny et al. (2009) conclude that the present configuration of V8 resulted from a substantial mass exchange between the components. Most likely, the present secondary lost nearly all matter from its original envelope and is burning hydrogen in a shell.
We adopted the best-fitting model from among the radiative solutions of Kaluzny et al. (2009), and calculated absolute parameters of V8 based on apparent magnitude of the primary (V = 17.43 mag) and distance modulus to NGC 6752 (μV = 13.13 mag; Harris 1996, 2010 edition). Their values are only approximate.
Ages of the clusters together with their uncertainties are taken from Marín-Franch et al. (2009) and Forbes & Bridges (2010). Ages of 47 Tuc and NGC 6752 were more recently discussed by Roediger et al. (2014); however their values remained unchanged. The Z-values in Table 1 were derived from [Fe/H] and [α/ Fe] indices quoted below using the XYZ calculator of G. Worthey1.
In ω Cen, which has been long known for its inhomogeneity, a broad range of Y and [Fe/H] is observed. According to a recent survey by Fraix-Burnet & Davoust (2015), the cluster contains seven subpopulations with 0.25 <Y< 0.4, −2.0 < [Fe/H] < −0.5, 0.2 < [α/ Fe] < 0.6, which also differ from each other in spatial distribution and kinematical properties. As a result, we are free in choosing [Fe/H], [α/ Fe] , and Y for evolutionary calculations of V209 (under the condition, of course, that they conform to the limits Fraix-Burnet & Davoust 2015, set for a given subpopulation). In particular, the subpopulation OC3c, on which we focus for reasons explained in Sect. 4, has 0.25 <Y< 0.4 and −1.75 < [Fe/H] < −0.5. We note that the spectra of Kaluzny et al. (2007a) were not good enough to derive abundances, and they adopted [Fe/H] = −1.7, which represents the peak of the metallicity distribution in the cluster.
The RGB of M 55 is split on the ultraviolet CMD, suggesting the presence of two subpopulations (Piotto et al. 2015). However, spectroscopic evidence speaks rather for chemical homogeneity (Kayser et al. 2006; Pancino et al. 2010). We adopt [Fe/H] = −1.94 (Harris 1996, 2010 edition), Y = 0.25, and a range 0.2−0.4 for [α/ Fe].
There is no doubt that 47 Tuc hosts more than one subpopulation of stars although, compared to ω Cen, it may be regarded as nearly homogeneous. While all the subpopulations have [Fe/H] = −0.72 ± 0.01, at least one of them may be enriched in He up to Y = 0.28 (Marino et al. 2016). We adopt −0.73 ≤ [Fe/H] ≤ −0.71, and 0.2 ≤ [α/ Fe] ≤ 0.4.
In the case of NGC 6752 the problem of homogeneity is still discussed (see e.g. Lapenna et al. 2016, and references therein). The latter authors argue for the presence of three stellar subpopulations with Y = 0.24, 0.25 and 0.26. [Fe/H] values they quote range from −1.80 (based on FeI lines) to −1.50 (based on FeII lines). We adopt [Fe/H] = −1.54Harris (1996), Y = 0.25, and (as for the other GCs) 0.2 ≤ [α/ Fe] ≤ 0.4.
The following search for progenitors of the investigated binaries is based on a model developed by one of us (Stȩpień 2006a; Gazeas & Stȩpień 2008; Stȩpień 2009; Stȩpień & Kiraga 2015). It describes the evolution of a cool close binary from the zero-age main sequence (ZAMS) until a stage preceding the merger of the components.
where (3)and Here M = M1 + M2 is the total mass of the binary, Htot, Hspin, and Horb are total, rotational and orbital AM, and are the (nondimensional) gyration radii of the components, r1 and r2 are the sizes of the inner Roche lobes, and q = M1/M2 is the mass ratio. Mass, radius, and semi-major axis are given in solar units, period in days, and AM in cgs units.
We assume that orbital and rotational motions are fully synchronized throughout the whole evolution, i.e. that the rotational period of each component is always equal to the orbital period P. This assumption is very well founded for close binaries based on both observations and theoretical considerations: systems with P< 10 are fully synchronized (Abt 2002), and synchronization time for periods shorter than 2−3 d is of the order of 104−105 yr (Zahn 1989).
Here Ṁ is in solar masses per year and dHtot/ dt is in g cm2 s-1 per year. The formulae are calibrated by the observational data of the rotation of single, magnetically active stars of different age, and empirically determined mass-loss rates of single, solar-type stars. Both formulae apply in a limiting case of a rapidly rotating star in the saturated regime. We note that they do not contain any free adjustable parameters. The constant in Eq. (7) is uncertain within a factor of 2 and that in Eq. (8) is uncertain to ±30% (Stȩpień 2006b; Wood et al. 2002). The model ignores any interaction between winds from the two components.
The evolutionary calculations are divided into three phases: from ZAMS to the Roche lobe overflow (RLOF) by the initially more massive component (henceforth donor), rapid, conservative mass exchange from the more to less massive component (henceforth accretor), and the last phase of a slow mass exchange resulting from nuclear evolution of the donor.
The present computations follow those described in Stȩpień & Kiraga (2015, please refer to that paper for additional details, assumptions etc.). However, a couple of modifications were introduced to increase accuracy and computational efficiency of the code. In particular, upon approaching the final evolutionary state, the time step was substantially shortened to avoid nonphysical period oscillations observed in some cases by Stȩpień & Kiraga (2015). Instead of Padova models (Girardi et al. 2000), the newer PARSEC models2 (Bressan et al. 2012) were used, which include up-to-date physics and cover a broader range of metallicities. Finally, for modeling of V209 and V228, we calculated our own evolutionary tracks using a procedure outlined in Sect. 4.1.
Equations from the previous section do not contain any free adjustable parameters, so after specifying helium (Y) and metal (Z) content, the initial masses of both components and the initial orbital period, the evolution of the binary is fully determined. Our task is to examine the initial parameters space until a model binary that fits observations is found. We note that the result of the search is not unique if the physical parameters of the observed binary, i.e. chemical composition, orbital period, masses, sizes, and luminosities of the components are only used for matching (Stȩpień 2011). Several model binaries with different values of the initial parameters can reproduce the observed values, but in each case a different time is needed to reach the agreement with the observations.
To demonstrate the nonuniqueness of the solution in a broader context, we computed three sets of models with initial mass ratios qinit = 0.94, 0.82, and 0.72; all of them with initial total mass Minit = 1.55 M⊙, and low metallicity Z = 0.001 characteristic of globular clusters (Minit was kept fixed, assuming that a progenitor of an exemplary binary with the final total mass close to 1.4 M⊙ was searched for). Each set contained 16 binaries with initial orbital periods of between 1.5 d and 3 d. In Set 1, the initial component masses were equal to (0.8, 0.75) M⊙; in Sets 2 and 3 − to (0.85, 0.7) and (0.9, 0.65) M⊙, respectively. We note that accounting for mass loss owing to the wind, the MS-lifetime of a 0.8 M⊙ star exceeds the age of the Universe, while that of 0.85 M⊙ and 0.9 M⊙ is shorter than the age of most GCs.
As it is seen in Fig. 1, the 0.8 M⊙ star fills its inner Roche lobe only in binaries with initial orbital periods shorter than 2.1 d. The orbits of these binaries are then so compact that soon afterwards both the components overfill the outer critical Roche surface and merge together. For periods equal to, or longer than 2.1 d, RLOF never occurs and the binaries stay detached. Set 1 models can only reproduce observed contact or near-contact binaries with parameters from a restricted range M1 ≲ 0.9 M⊙, M2 ≳ 0.55 M⊙ and P ≲ 0.4 d.
The situation changes a lot when we consider Set 2 binaries with M1 = 0.85 M⊙ (Fig. 2). An M1 = 0.85 M⊙ primary fills the Roche lobe during the MS evolutionary phase only in binaries with the four shortest periods. For all other periods, it leaves the main sequence while being detached from its Roche lobe, but the ensuing expansion quickly leads to the RLOF. A rapid mass exchange occurs, after which the orbital period increases and the mass ratio decreases. Set 2 models can reproduce observed binaries with parameters from a broad range M1 ≲ 1.25 M⊙,M2 ≳ 0.2 M⊙, and P from a fraction of a day up to a few days. Their final ages are concentrated around 11 Gyr. Figure 3 shows the evolution of Set 3 models with M1 = 0.9 M⊙. It is very similar to Fig. 2, except that the final ages are concentrated around 9 Gyr.
Time evolution of Set 1 models with initial component masses of 0.8 and 0.75 M⊙ (broken lines, left axis) and initial periods of 1.5−3.0 d (solid lines, right axis). Only the six shortest-period binaries reach the RLOF phase within the age of the Universe, enabling the mass exchange between their components. All other binaries stay detached.
Same as in Fig. 1 but for Set 2 models with initial component masses of 0.85 and 0.70 M⊙. Only the four shortest-period binaries enter the RLOF phase when the primary component is still on the main sequence. For all other binaries, RLOF occurs when the primary is past the main sequence i.e. at an age of ~11 Gyr.
Same as in Fig. 1 but for Set 3 models with initial component masses equal to 0.90 and 0.65 M⊙. Only the three shortest-period binaries enter the RLOF phase when the primary component is still on the main sequence. For all other binaries, RLOF occurs when the primary is past MS, i.e. at an age of ~9 Gyr.
As we see, the final age of the model crucially depends on the initial mass of the primary, M1. Changing Z has a similar, but weaker effect to changing M1 (see Fig. 4). Knowledge of age and metallicity of the observed binary lifts the indeterminacy of the initial parameters. Fortunately, for GC members these parameters are known with a reasonable accuracy, even in clusters containing multiple subpopulations (Roediger et al. 2014).
Figures 1−3 may be regarded as an illustration of a coarse search of the parameter space. To reproduce the observed binary parameters more accurately, all three initial parameters have to be varied within a narrow range around the values resulting from the coarse search. This also includes the total initial mass because different component masses result in somewhat different mass losses. Examples of such fine search in period are shown in Figs. 5−8, which are related to the four actual binaries discussed below.
Data on observed and model binaries.
To select the best-fitting models, we applied the following procedure: first, we adopted the Y and Z parameters, in agreement with the observations of the parent clusters. Then, we evolved the model binary until the orbital period was to the third decimal place equal to that listed in Table 1, and, simultaneously, the observed component masses were reproduced within the observed uncertainties. This accuracy of period-fitting proved high enough for the resulting uncertainty of progenitor parameters to be negligible compared to the overall uncertainty dominated by sources discussed in the following sections. Finally, of all models meeting these criteria, the one with the age closest to the cluster age was selected. Radii, effective temperatures and luminosities of the components resulted automatically from the evolutionary sequences. The exception, discussed in detail in Sect. 4.1, were extremely low-mass stars (M< 0.2 M⊙) with helium cores and extended hydrogen envelopes, which we could not model reliably enough.
The basic data for the best-fitting models are given in Table 2. For each star, the left column contains the age of the parent cluster and the observed values of stellar parameters. The age of the model is given in the first row of the middle column and then all other parameters, as obtained from the model. For the secondary components of V209 and V8, no data on temperature and luminosity are given because we were not able to model extremely low-mass stars with a substantial helium core. A well known relation exists that connects the mass of the helium core with the stellar radius and luminosity, but it only applies to red giants with a sufficiently high total and core mass (Iben & Livio 1993; Eggleton 2009). Stars that are less massive than about 1 M⊙ with the helium core mass lower than about 0.2 M⊙ obey individual core mass-luminosity relation (see Fig. 2.9 in Eggleton 2009), as well as core mass-radius relation (Muslimov & Sarna 1996), depending on the total stellar mass. The right column gives for each star relative differences Δ(obs. − mod.) expressed in per cent.
Relation between metallicity and life-time on the MS for stars with different masses, based on PARSEC models. Indicated are the four clusters discussed in the present paper. Vertical and horizontal line segments give for each cluster uncertainties of both coordinates (see Table 1).
The ages of V209 and V8 are close to the adopted ages of the hosting clusters ω Cen and NGC 6752, but a serious mismatch occurs in the remaining two cases, in which the best-fitting models are significantly younger than the corresponding clusters. The discrepancy is of a fundamental nature, as Fig. 4 shows. Here we plotted the MS lifetime of stars with different masses and metallicity. The lines of constant mass are shown with solid lines and labels. We also plotted the positions of all four clusters according to their age and metallicity. The positions give the maximum mass of a star which just reached TAMS in each cluster. This mass is close to, but not identical with, the turn-off mass. Specifically, the turn-off mass, defined as a hottest MS star on the isochrone corresponding to a given cluster, is lower by 0.01−0.02 M⊙ than the plotted maximum mass. Doubling this mass gives a good approximation of the maximum total mass of a close binary, which can still be found in the blue straggler region of the cluster (assuming a strictly conservative evolution, i.e. no mass loss from the system and no close interactions with other members of the cluster). The read-off values of the maximum mass are: 0.78 ± 0.01 M⊙ for M 55, 0.8−0.9 M⊙ for ω Cen, 0.80 ± 0.01 M⊙ for NGC 6752 and 0.81 ± 0.01 M⊙ for 47 Tuc. While the observed total masses of the analyzed binaries in ω Cen and NGC 6752 are lower than these limits, they are higher in two other clusters: 1.586 versus 1.56 M⊙ for M 55, and 1.712 versus 1.62 M⊙ for 47 Tuc. Moreover, the evolutionary model includes the mass loss of several percent during the binary evolution (mostly during the longest first phase), so the initial component masses must be even higher than the measured ones (see Table 2). In effect, no model binary can be found that reproduces the observed total mass and age of V60 and V228 (assuming, of course, that their ages are equal to the ages of their parent clusters).
Time variations of orbital period (solid lines, right axis) and component masses (broken lines, left axis) of the best fitting model of V209 (see Table 2 for its initial parameters). Also shown are two models with the same initial component masses, and periods differing by ±0.02 d from the best-fitting one. The observed parameters of V209 are indicated by a filled circle (period) and diamonds (masses). Vertical sizes of the diamonds correspond to observational errors.
ω Cen is the most massive but also the most unusual GC in our Galaxy. It shows a very complex structure with a very broad MS, suggestive of a combination of a few independent sequences, multiple horizontal, subgiant and red giant branches, and a large spread in heavy element content (Norris et al. 1997; Johnson et al. 2010; Piotto et al. 2005; Joo & Lee 2013; Fraix-Burnet & Davoust 2015, and references therein). As a result, several (up to seven) different subpopulations have been identified with different chemical compositions and ages. In particular, an enhanced helium abundance was suggested for two subpopulations (Joo & Lee 2013; Fraix-Burnet & Davoust 2015).
To find a progenitor of V209, we first used PARSEC models in a search for desirable initial binary parameters. It quickly turned out that at the helium abundance Y = 0.25−0.27 the primary of V209 is far too hot for its mass, independently of metal content and age varying within the observed values. It is known, however, that evolutionary tracks of the helium enriched models are shifted towards higher temperatures (and higher luminosities) in the CMD, compared to normal helium abundance models (Glebbeek et al. 2010). Based on the suggestion that a significant subpopulation of cluster members may have helium content Y ≈ 0.40 (Joo & Lee 2013; Fraix-Burnet & Davoust 2015), we generated our own grid of evolutionary tracks for helium-enriched stars.
The tracks were computed using the Warsaw-New Jersey evolution code, which is an updated version of B. Paczyński’s code (Paczyński 1969, 1970). The computations were performed starting from chemically uniform models on the ZAMS. The input parameters for evolutionary model sequences are total mass, M, initial value for helium abundance, Y0, and heavy element abundance, Z. We computed two series of models with masses from 0.50 to 1.60 M⊙, with a step size of 0.05 M⊙. In one series of the computations, we assumed Y0 = 0.40,Z = 0.0004, in the second one, −Y0 = 0.27,Z = 0.003. For chemical elements heavier than helium, we adopted the solar element mixture of Asplund et al. (2009). For the opacities, we used the Opacity Project (OP) data (Seaton 1996, 2005) supplemented at log T< 3.95 with the low-temperature data of Ferguson et al. (2005). In all computations, the OPAL equation of state was used (Rogers et al. 1996, version OPAL EOS 2005). The nuclear reaction rates are the same as used by Bahcall & Pinsonneault (1995). In the stellar envelope, the standard mixing-length theory of convection with the mixing-length parameter α = 1.6 was used. The choice of the mixing-length parameter is important in our models because they are sufficiently cold to have an effective energy transfer by convection in the stellar envelope, namely in the regions of partial ionization of hydrogen and helium, and therefore will have an influence on the structure of the models and their position on the HR diagram. We used a value of α to be close to estimations for the Sun between 1.7 and 2.0 (Magic et al. 2015), as obtained from 3D computations and calibration to the solar radius.
Based on those models, we were able to find a progenitor of V209 (see Table 2). A binary with the initial orbital period of 1.66 d and the component masses of 0.65 and 0.55 M⊙ evolves after 11.34 Gyr (which is almost equal to the adopted age of ω Cen) into a binary with parameters close to V209, see Fig. 5. Tracks for two additional models are also plotted to illustrate the accuracy of the fine parameter search, in this case in period. The models have the same initial component masses as the best-fitting one, but their initial periods differ by ±0.02 d from the best-fitting one. The obs. − mod. differences are significantly larger for them: ΔP = 0.8% and 6.8%, ΔM1 = 3.7% and 0.1% and ΔM2 = 8% and 13% for the shorter and longer period model, respectively. A change of either component mass by, for example, 1% results in a similar worsening of the fit. We conclude that fitting the model to the observations with the assumed accuracy requires a really fine tuning of the initial parameters.
We note that, in our model, unlike in the scenario proposed by Kaluzny et al. (2007a), there is no need for the binary to experience two CE phases: just one mass transfer phase is sufficient to reproduce all the observed parameters of the primary (accretor) within the observational uncertainty. Unfortunately, in the case of the secondary (donor), we could only compute its mass and the mass of its helium core. We followed the evolution of the donor until its mass approached 0.2 M⊙, assuming that it still fills its Roche lobe. The helium core then reached a mass of about 0.13 M⊙. As the mass of the star decreases beyond 0.2 M⊙ , its radius shrinks rapidly, the star detaches from the Roche lobe, and loses mass via stellar wind and during the thermonuclear flashes that occur in the hydrogen burning shell (Sarna & De Greve 1996; Muslimov & Sarna 1996; Driebe et al. 1998; Althaus et al. 2013). Below about 0.18 M⊙, flashes disappear but the radius (and mass) continues to decrease as the star moves to the high temperature region in the HR diagram. These phases are not described by our model because of a lack of sufficiently dense grid of evolutionary models of these types of stars. Nevertheless, the precise fit of our model to the observed parameters of the primary component of V209, in particular an unusually high effective temperature for its mass, may be regarded as independent and strong evidence for the existence of a stellar subpopulation in ω Cen with the high helium content of Y = 0.40.
Same as in Fig. 5, but for V60 in M 55. The two additional models have initial periods differing by ±0.025 d from the best-fitting one.
This binary was already used by Stȩpień & Kiraga (2015) to demonstrate the potential of the method that was outlined in Sect. 3 in identifying progenitors of close binaries in GCs. Among models calculated in that paper, the one with Pinit = 1.9 d and component masses (M1,M2) = (0.89, 0.80) M⊙ reproduced the observed parameters of V60 fairly well. However, it could not be regarded as a solution to the present problem since its metallicity did not conform to the limits given in Table 2, and, moreover, the whole BS population of Stȩpień & Kiraga (2015) was generated without paying attention to the age of the models. Thus, a standard search of the parameter space was necessary. Once finished, we found that the model that best matches the present values P,M1, and M2 was over 2 Gyr younger than M 55. As argued at the beginning of Sect. 4, this discrepancy is a direct consequence of the doubled turn-off mass of M 55 being smaller than the total mass of V60. The results of the present fit are shown in Fig. 6.
The CMD of the cluster suggests a presence of subpopulations that differ in age and/or chemical composition (Piotto et al. 2015). An age discrepancy of 2 Gyr between them seems rather unlikely, but it can not be entirely excluded. On the other hand, the ages of M 55 and V60 could be reconciled if the metallicity of the straggler were significantly higher than the upper limit given in Table 2. Figure 4 shows that the present total mass of V60 can be reached for Z ≈ 0.005, i.e. about 15 times higher than obtained for the cluster (we note that M 55 is the most metal-poor of all the GCs discussed in this paper). If V60 belonged to a subpopulation younger by 1 Gyr than the cluster, the value of Z necessary for the turn-off mass to be equal to the total mass of the binary would decrease to 0.003, a value that is still much larger than observed. Clearly, more data and better models are needed to resolve the discrepancy.
This is another variable star for which a substantial discrepancy occurs between the adopted age of the cluster and the age of the best fitting model (Table 2 and Fig. 7). The PARSEC models with the metallicity of 0.003 are not available, so we decided to compute a special set of models with this value of Z and a helium content Y = 0.27. The best fitting model has the initial component masses equal to 0.95 and 0.94 M⊙, orbiting each other with the period of 2.129 d.
Same as in Fig. 5, but for V228 in 47 Tuc. The two additional models have initial periods differing by −0.02 and 0.04 d from the best-fitting one.
A binary with a total mass this large, and metallicity characteristic of 47 Tuc, should be past the red giant phase long before the age of the cluster. Here, the discrepancy between the cluster and model age is even larger than for M 55 (2.7 vs. 2.1 Gyr). Similar to other clusters, 47 Tuc also shows multiple subpopulations (Joo & Lee 2013; Piotto et al. 2015), but so far no data on the age spread are available. Alternatively, the age of the model binary can be brought to agreement with the cluster age if its components have metallicity 3−4 times higher than adopted for the cluster.
The secondary of V228 reached a mass of 0.2 M⊙ , but it still fills its Roche lobe and has characteristics of a subgiant with a helium core of 0.12−0.13 M⊙. The model reproduces the observed parameters quite well. We expect the star to detach soon from its Roche lobe and to move to the left in the HR diagram. The agreement of the model with the primary of V228 is somewhat poorer. In particular, the radius of the accretor is significantly larger than observed, and also the temperature is significantly higher. As a result, the luminosity of the model primary is too high by 0.19 dex, compared to the observations. The difference suggests that the real primary is less evolutionarily advanced than the model.
Same as in Fig. 5, but for V8 in NGC 6752. The two additional models have initial periods differing by ±0.025 d from the best-fitting one.
This is the most unusual binary system of all discussed in the present paper. It is a near contact binary with an extremely low mass secondary of 0.12 M⊙ , which possesses the radius of 0.45 R⊙ and fills its Roche lobe. A single star with this mass and a significant helium core has a much lower radius as the calculations by Muslimov & Sarna (1996) show. A similarly low radius results from the paper by Paczyński et al. (2007) who computed radii of several stars with masses between 0.18−0.14 M⊙ and different helium cores. The maximum stellar radius decreases from about 1.3 R⊙ for a 0.18 M⊙ star down to about 0.3 R⊙ for a 0.14 M⊙ star. An extrapolation of this trend to 0.12 M⊙ gives a maximum radius of about 0.15 R⊙, in good agreement with the paper by Muslimov & Sarna (1996). The observed large value of the radius must result from the interaction with the other component. V8 may remind us in this respect of AW UMa (Rucinski 2015), where the 0.13 M⊙ secondary possesses a massive helium core and is submerged in the matter flowing from the 1.3 M⊙ primary component. AW UMa looks like a typical contact system of W UMa-type with the secondary radius of about 0.5 R⊙, yet the detailed observations of this binary obtained by Rucinski (2015) indicate a much more complex geometry of the system, where both components do not actually fill their Roche lobes, but are surrounded by the equatorial flow extending up to the inner critical surface. The existence of this type of flow in contact and near contact binaries was predicted by Stȩpień (2009) and Stȩpień & Kiraga (2013). The flow redistributes energy between the components, resulting in an apparent equality of their effective temperatures, which we also see in V8 (see Table 2).
The observational parameters of V8 result from the solution of the light curve only. No radial velocity curve exists for the variable, which makes the solution rather uncertain. Fortunately, one of the eclipses is total so the range of likely parameter values is not too large. The best fitting model has the values of the main parameters satisfactorily close to the observed ones (see Table 2 and Fig. 8), but the radius and temperature of the accretor are significantly lower than observed. This results most likely from the fact that the donor transferred to the accretor not only its outer layers with the original hydrogen content, but also an amount of matter enriched in helium by the nuclear reactions. As a result, the accretor behaves like a more evolutionarily advanced star, compared to the model. Our simple modeling procedure does not take this into account. It assumes that all the transferred matter is hydrogen-rich so after the mass transfer the accretor has the hydrogen content very close to that of a zero age MS star.
The discrepancy is closely related to another caveat of the best fitting model. To satisfactorily reproduce the observed parameters, it was necessary to assume an initial mass ratio qinit = M1,init/M2,init = 4.47. During the rapid mass transfer after RLOF, the orbital period decreased to about 0.1 d, which resulted in the overflow of the outer critical Roche surface by the common stellar surface. The assumption of the conservative mass transfer very likely breaks down in this case. However, to allow for the nonconservative mass transfer, two additional free parameters describing the amount of mass and AM lost from the system would be necessary. Because we avoid this, the conservative mass transfer can be considered as a limiting case when all the matter from the CE ultimately returns to the stars. We note, that the model of V8 is the only one with such an extreme initial mass ratio.
We have reproduced the present configurations of the considered systems, assuming a conservative evolution of isolated binaries (apart from the mass and AM loss by stellar winds). Obviously, this result does not prove that V209, V60, V228, and V8 are formed in this way but just indicates such a possibility. Approximating the evolution of binary components with single star models only works well in case of V209. While, for the remaining three BSs, orbital periods and component masses also agree with observations, radii, and temperatures derived from modeling differ from the observed ones by several standard deviations. This points to the limitations of the simple evolutionary code employed in this paper. A sequence of evolutionary models of single stars correctly describes the evolution of close binary components only until the rapid mass exchange. Later on, the evolution of both components deviates increasingly from that of single stars, in particular when the accretor begins to receive nuclearly processed matter from the deeper layers of the donor. An obvious improvement would be to replace the present code with a binary evolution code, solving the equations of the internal structure of each component at every time step, and allowing for the mass transfer between the components. The next step would be to incorporate the dynamical processes that take place in close binaries, but are still poorly understood, like the rapid mass transfer following RLOF with an unknown amount of mass and AM lost from the system (Sarna & De Greve 1996), or the mass flow carrying thermal energy from the primary to secondary component in a contact binary (Stȩpień 2009; Rucinski 2015).
The BS progenitors identified in the present survey are close binaries. Below we argue that this result is calculationally robust, and physically feasible.
Uncertainties in the evolutionary modeling procedure outlined in Sect. 3 are discussed in detail by Stȩpień & Kiraga (2015). Here we only make use of their most important conclusions. The progenitors of V209, V60, V228, and V8 have lost, respectively, ΔM = 7.7%, 8.8%, 9.7% and 7.8%, and ΔAM = 67%, 53%, 72% and 71%. An increase of the mass loss rate by a factor of 2 entails an increase of M by ΔM, whereas its decrease by 50% entails a decrease of M by ΔM/2. Similarly, decreasing/increasing the AM loss rate by 30% requires a decrease/increase of the initial AM by the same percentage of ΔAM, which corresponds to initial orbital periods of 0.84 and 2.88 d for V209, 1.30 and 3.03 d for V60, 1.63 and 2.71 d for V228, and 2.82 and 3.71 d for V8 (calculated for M kept constant).
Thus, varying the coefficients in Eqs. (7) and (8) within observationally acceptable limits cannot cause the model progenitors to leave the short-period regime.
The next question to ask is: can close binaries be sufficiently abundant in a GC to account for the observed binary BSs? The efficient tightening of binaries in triple systems by the Kozai mechanism can be mentioned in this respect. The presence of a third body stimulates the so-called Kozai cycles which, together with the tidal energy dissipation, can shorten an orbital period of 1−2 weeks down to a couple of days within less than 108 yr (Eggleton & Kiseleva-Eggleton 2006; Fabrycky & Tremaine 2007; Naoz & Fabrycky 2014). If this is the principal source of close binaries in GCs, then a local maximum around 2−4 days may be expected in the period distribution of young cluster binaries, similar to that observed by Tokovinin & Smekhov (2002) among spectroscopic subsystems of visual multiple stars. Close binaries can also be formed due to so called hardening encounters with single or binary cluster members (see for example Leigh et al. 2015, and references therein). We note that the progenitors do not have to be formed as close binaries; it is sufficient for them to tighten shortly before the more massive component leaves the main sequence, so that there is ample time for the hardening to occur. However, the recent research of Hypki & Giersz (2016) suggests that most of the evolutionary BSs result from the unperturbed evolution of primordial binaries.
Whether primordial or hardened, all the four binaries considered here have experienced a rapid mass exchange with the mass-ratio reversal. Their present primaries are main-sequence objects substantially enriched in matter from the companion. An exception is V60, whose primary is still accreting, and may be quite far from thermal equilibrium (Rozyczka et al. 2013). The secondaries are evolutionarily advanced objects with considerable helium cores. Two of them are already heading towards the sdB domain, and the third one (in V228) should do it soon. The most probable scenario for the ultimate fate of all the four systems involves the CE phase beginning when the present primaries reach the RGB, and followed either by a merger (Tylenda et al. 2011; Stȩpień & Kiraga 2015) or the formation of a close binary with two degenerate stars.
The good agreement between the ages of V209 and V8 and the ages of their parent clusters does not exclude the possibility that they were formed after the bulk of the cluster. Assuming, for example, that V209 should belong to a younger subpopulation, it is possible to slightly increase the initial mass of the donor and to accordingly modify the mass of the other component together with the initial orbital period, so that the evolutionary time-scale of the binary will be shorter. Similarly, the age of model (4) describing V8 can be altered by an appropriate modification of the donor mass as is demonstrated in Figs. 1−3.
Binaries V60 and V228 are apparently younger than M 55 and 47 Tuc or, in other words, are overmassive for the ages of their parent clusters. While it is tempting to suggest that they are members of younger subpopulations, it would be premature to do so. First, it is conceivable that overmassive systems are products of multiple mergers or collisions (Sandquist et al. 2003; Leigh & Sills 2011). Second, as we argue in the following paragraphs, available stellar evolution models are simply not reliable enough to draw such far-reaching conclusions. In particular, an apparent age discrepancy may emerge whenever MS life-times of models applied to determine the age of the cluster differ from those of models applied to evolve individual binaries. We note, however, that the cases of V60 and V228 are not unique. Based consistently on Dartmouth evolutionary models, Kaluzny et al. (2015b) found that the detached main-sequence binaries V40 and V41 in NGC 6362 differ in age by 1.3 ± 0.4 Gyr, i.e. statistically significant at the 3σ level. In our opinion, all these discrepancies are vexing enough to be closely examined by more accurate observations and better modeling.
A broader context of our findings is origin and evolution of GCs. Obtaining the absolute age of a cluster involves many steps in transformation of observational data into theoretical parameters to which models can be fitted. Both the poor data and oversimplified theory may generate incoherent results or even paradoxes, like cluster ages significantly exceeding the Hubble time. The latter values were still being derived in the late 90 s, as emphasized by VandenBerg (2000), who thoroughly rediscussed the issue and obtained ages between 8 and 14 Gyr. While the basic paradox had been removed, the problem is far from settled. Although new methods of age determination have been introduced, in addition to the original isochrone fitting, all of them remain strongly model-dependent, be it sophisticated isochrone construction (Dotter 2016) or comparing absolute parameters of turn-off stars or detached binaries with the output of stellar evolution codes (Marín-Franch et al. 2009, project CASE, see Introduction). Moreover, in spite of constant progress in modeling significant differences exist among codes used by different authors. Important physical processes like convection, semiconvection, diffusion, mixing, or rotation are usually described by single-value parameters that are adopted individually in each code. Cool, solar-type stars generate winds induced by their magnetic activity, but the resulting mass and AM loss has been largely neglected when computing evolutionary tracks. Only very recently some codes, like MESA, have included such losses as an option.
Even Y and Z – the fundamental parameters describing the chemical composition of a star – do not always have a well-defined meaning, since the [Fe/H] index, which is often used as an input parameter, may relate to different values of Z⊙. Moreover, different transformations [Fe/H] → Z may be used, and different correlations between Z and Y may be assumed. No wonder that the resulting stellar parameters differ from one code to another. The codes are typically calibrated on the Sun, so they reproduce MS solar type stars in a consistent way. Yet, the most important parameter for the correct determination of GC ages, i.e. MS life-time can differ for some stars quite considerably. To give an example, the old Padova model of a 0.8 M⊙ star with Z = 0.001 has MS life time equal to 13.5 Gyr (Girardi et al. 2000), whereas the new PARSEC model of the same star only 11.95 Gyr (Bressan et al. 2012). Another example: recently published by Lagarde et al. (2012) 0.85 M⊙ model with Z = 0.0001 has the MS life of 11.14 Gyr, compared to 9 Gyr for the PARSEC model with the same Z. Differences in time-scales between models beyond the MS are still greater. This diversity recently concerned a number of authors who discuss the influence of several physical mechanisms on models produced by different codes and compare them to well calibrated observational data (Nataf et al. 2012; Martins & Palacios 2013; Ghezzi & Johnson 2015; Meynet et al. 2016; Stancliffe et al. 2015; Valle et al. 2016b,a). However, uncertainties of stellar evolution models still remain the primary factor that impedes the accurate determination of the absolute ages of globular clusters. Observational uncertainties will dramatically decrease when Gaia parallaxes become available (distances to many GCs will be known with an accuracy better than one per cent; Pancino et al. 2013). If the theory is to catch up with observations, much more effort in exposing and diagnosing its problems is needed. We believe that evolutionary simulations of binary blue stragglers is a very useful tool to achieve this goal.
The results of the present investigation demonstrate animportance of the close binary evolution in the formation of bluestragglers. In particular, it was shown that blue stragglers resultfrom rejuvenation of an initially less massive component that isfed by the hydrogen rich matter from its companion overflowingthe inner Roche lobe.
To reproduce the present parameters of V209 in ω Cen, it was necessary to adopt the increased helium content Y = 0.40 of this binary. This is further evidence in favour of the existence of the helium-rich subpopulation in this cluster.
The best fitting models of V60 in M 55 and V228 in 47 Tuc are too massive for the age of the parent cluster as it is currently estimated. Unless this is an apparent effect resulting from an inconsistency between models used for GC age determination and binary modeling, these systems may belong to younger subpopulations or may result from dynamical multibody interactions.
Different evolutionary codes produce mutually inconsistent stellar parameters. A better description of physical processes influencing the stellar evolution is urgently needed. Until this shortage is overcome, the absolute age determination of globular clusters will be plagued with substantial uncertainties.
Studying the evolution of binary BSs in GCs emerges as a new research tool that provides an independent insight into interactions between GC members and enables sensitive tests of stellar evolution codes.
This paper is dedicated to the memory of Janusz Kaluzny, founder and long-time leader of CASE, who prematurely passed away in March 2015. We thank an anonymous referee for very insightful remarks that significantly improved the final shape of the paper. A.A.P. acknowledges partial support from the Polish National Science Center (NCN) grant 2015/17/B/ST9/02082. M.R. was supported by the NCN grant DEC-2012/05/B/ST9/03931.

industry_corpus2: Technology & Research


text:
Westlink M7 values safety. To ensure that we maintain a safe environment for our customers, staff and contractors – and for efficient operation of the M7 motorway, please read the information, and follow steps below, for work or access to the M7 motorway corridor.
Contractors and companies planning work in the M7 corridor, or transport companies with oversize/overmass (*OSOM) heavy vehicles and loads travelling on the M7 motorway, are to register and apply for a work access permit (WAP) through our online system, Permitted.
A work authority permit is required for planned work activity on the M7 mainline and interchange ramps, in areas on or next to the M7 Shared Path, or on site at the Westlink M7 Eastern Creek Control Centre (ECCC).
Registering with Westlink M7 is easy, and one time only. Email the following details to access@m7.com.au.
Contractors - attach current Public Liability (min $20M) and Work Cover Certificates (*insurance documentation can be updated annually to remain registered).
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industry_corpus2: Transportation


text:
Do you love the challenge of selling?
It’s advertising in the theatre programme for Little Shop of Horrors ... and possibly a few special sponsorships.
What we’re after is a member of the production team who can recruit about $1000 worth of advertisers or sponsors over the coming two months. That would mean, for example, getting 10 ads at $100, or maybe a combination of 6 or 8 ads + a couple of $250 sponsorships.
We have good things to offer in return—a classy theatre programme that reaches 1500 people, mention in our publicity, complimentary ticket and such. We will provide a recruitment brochure which outlines the show in an appealing way, ad sizes & prices, and enticements.
Interested in the challenge? Get in touch with the show’s producer, Rob Thomson, at 902-628-6778, robthomson @ pei.sympatico.ca.


text:
"This is such a gold mine of strategy, tools, and the heart and purpose behind teaching leadership."
This is such a gold mine of strategy, tools, and the heart and purpose behind teaching leadership and the servant-leadership model. I valued every minute of the time today. I could keep listening, learning, and reflecting!


text:
Five former members of Pi Kappa Phi enter plea agreements for the death of fraternity pledge Andrew Coffey.
At the Leon County Courthouse Monday morning, five former members of Pi Kappa Phi plead guilty to two counts of a misdemeanor hazing in connection to the death of fraternity pledge Andrew Coffey.
The 20-year-old civil-engineering student was found unresponsive at an off-campus apartment off of High Road on Buena Vista Drive. After police arrived, Coffey received medical treatment, but he was pronounced dead on-scene.
The five sentenced–Kyle Bauer, Brett Birmingham, Christopher Hamlin, Conner Ravelo and John Ray–will not be allowed to drink alcohol and will be subjected to random testing. The sentence also requires the men to enroll in a hazing awareness course, speak on the dangers of binge drinking and hazing whenever asked and write an apology letter to the Coffey family.
Before the plea hearing, the parents of Andrew Coffey, Tom and Sandra, made a victim impact statement.
Coffey's parents talked about how their son had enrolled at TCC and transferred to FSU. He was thrilled to be a Seminole and planned to go join the Navy.
“An entire community is heartbroken because of the senseless tradition of ‘Big Brother Night,’” Coffey’s mother said. “He was simply the person everyone wanted to be around. Our family wakes up every day with a hole in our hearts and our lives…Andrew died alone in a room full of people and we will never be able to understand that. Last year, four young men died while pledging a fraternity. Fraternity hazing needs to stop.”.
Ravelo, who has been in jail for 22 days, was the first to come forward for sentencing. He was Coffey’s “big brother” in the fraternity. Of all five defendants heard, Ravelo received the shortest jail sentencing due to his cooperation since the beginning of the investigation. He will only serve eight more days in Leon County jail because he will get credit for time already served.
Ravelo explained that he had wanted to apologize earlier, but was told it was not appropriate by police and could not send an apology note for the funeral because of the ongoing investigation. The defendants believe that engaging in speaking engagements will help end hazing and binge drinking–something the Coffey parents explicitly referenced in their victim impact statement.
Bauer is sentenced to 60 days in jail and must turn himself to Leon County jail by this Friday at 5pm, or he would violate his probation. He will get credit for one day served.
Hamlin will also receive credit for one day served and plans to serve his sentence in Hillsborough County jail. The exact date he will turn himself in was not addressed.
Birmingham plans to turn himself in in the next few weeks, but he wants to serve in Santa Rosa or Wakulla counties. The judge urged Birmingham to complete his hazing awareness class prior to turning himself in.
Birmingham's attorney, Fred Cochran, spoke to the Tallahassee Democrat after the trial and questioned why FSU was not being held accountable. Cochran said that a felony charge was a deal breaker for his client and that they did not want to go trial.
Ray said he did not want to put the Coffey family through the trauma of trial. He plans to turn himself into Leon County jail by Monday, April 16 at 6pm.
All five of these individuals were initially charged with a third-degree felony, which could’ve brought a sentence of up to five years. However, they were charged with two misdemeanors because of the plea deal. Each misdemeanor has a maximum sentence of one year.
Afterwards, the Coffey family attorney, David Bianchi, discussed the upcoming trial in June for the other four defendants. Bianchi said it reminded him of a sexual assault case because the main defense is that it was the victim’s fault.
“I have yet to meet a college student who hasn’t drunk alcohol,” Bianchi said. He emphasized that their attempt to blame Coffey is disgusting.
In terms of the civil case against Pi Kappa Phi, Bianchi revealed that a similar case occurred 18 years ago at California State Chico, when Adrian Heideman was killed after a "Big Brother Night." Strippers were brought to both events and the pledges were encouraged to get as drunk as possible.
Bianchi emphasized that the adults running this fraternity should be held accountable for this behavior. Mark Timmis is currently the CEO of the Pi Kappa Phi and held the position at the time of both Heideman and Coffey's death.
The Coffey family is currently bringing a case against the fraternity as a whole, and there will be a case management meeting tomorrow.


text:
Vancouver’s Old Apple Tree is 190 years old! The City of Vancouver invites the public to come celebrate at the annual Old Apple Tree Festival from 11 a.m. to 3 p.m. on Saturday, Oct. 1. The free event takes places at the Old Apple Tree Park, 112 S.E. Columbia Way, directly east of the I-5 Bridge near the Fort Vancouver National Historic Site.
Bring your own clean apples and containers to participate in the free apple pressing. Also on tap at the family-friendly festival this year will be live music, tours of the Land Bridge, arts and crafts for kids and tree care workshops. Food will be available for purchase. The Urban Forestry Commission will also give away a limited number of tree cuttings from the Old Apple Tree.
Planted in 1826 at Fort Vancouver, Vancouver’s venerable Old Apple Tree is the oldest apple tree in the Pacific Northwest and is considered the matriarch of Washington State’s apple industry. Despite floods, winds, drought, ice and snow, the tree has survived and continues to produce some fruit.
The Old Apple Tree Festival is presented by Urban Forestry, Bartlett Tree Experts, and the National Park Service. For more information about the Old Apple Tree Festival, call the City’s Urban Forestry office at 360-487-8308 or visit www.cityofvancouver.us/urbanforestry.
Celebrate the Old Apple Tree’s amazing 189 years of life at Vancouver’s annual Old Apple Tree Festival, 11 a.m. to 3 p.m. Saturday, Oct. 3, at the Old Apple Tree Park, 112 S.E. Columbia Way, directly east of the Interstate 5 Bridge within the Fort Vancouver National Historic Site.
Planted in 1826 at Fort Vancouver, Vancouver’s venerable Old Apple Tree this is the oldest apple tree in the Northwest and considered the matriarch of Washington State’s apple industry. Despite floods, winds, drought, ice and snow, the tree lives on, standing tall to greet visitors.
The free festival features live music, food, tours of the Land Bridge, arts and crafts for kids, tree care workshops, and free apple cider pressing. To participate in the apple cider pressing, bring your own clean apples and clean containers to take home your freshly pressed cider. The Urban Forestry Commission will also give away a limited number of tree cuttings from the Old Apple Tree.
The Old Apple Tree Festival is presented by the Urban Forestry Commission in partnership with the City of Vancouver’s Urban Forestry, a Public Works Department program, Clark Public Utilities, Bartlett Tree Care, and the National Park Service. For more information about the Old Apple Tree Festival and Vancouver’s efforts to enhance the community’s trees and highlight the benefits they bring to residents and businesses, call Urban Forestry at 360-487-8308 or visit www.cityofvancouver.us/urbanforestry.
Celebrate the Old Apple Tree’s 188 years of life at Vancouver’s annual Old Apple Tree Festival, to be held from 11 a.m. to 3 p.m. on Saturday, Oct. 4, at the Old Apple Tree Park, 112 S.E. Columbia Way, directly east of the I-5 Bridge within the Fort Vancouver National Historic Site. This year, the free, family-friendly festival features live music by On a Lark, Another Shade of Bluegrass, and the Washington Old Time Fiddlers Association. There will also be fruit tree pruning demonstrations, arts and crafts for kids, ask-the-arborist sessions, Fort Vancouver Land Bridge tours and on-site food vendors.
To participate in the apple cider pressing, bring your own clean apples and clean containers to take home your freshly pressed cider. You can also get a free cutting to start your own piece of history. Each year during the festival, the Urban Forestry Commission gives away approximately 200 cuttings from the Old Apple Tree. While it’s challenging to successfully propagate these cuttings, it is possible. The commission would like to know how many people are able to successfully propagate their cutting, so if you’ve managed it, bring your story or a photo of your Old Apple Tree; a map will show where descendants of the Old Apple Tree live. For more details, call Urban Forestry at 360-487-8308 or visit www.cityofvancouver.us/urbanforestry.
In 1826, the U.S.A. celebrated its 50th birthday, the American Temperance Society was founded, Thomas Jefferson and John Adams died, and the oldest living apple tree in the Pacific Northwest was just a sprout. Planted in 1826, the noble Old Apple Tree is considered the matriarch of Washington State’s apple industry. It has withstood flood, wind, ice, snow, steady human encroachment and breakage of a major limb in 2009.
Celebrate the venerable tree’s 188 years of life at Vancouver’s annual Old Apple Tree Festival, to be held from 11 a.m. to 3 p.m. on Saturday, Oct. 4, at the Old Apple Tree Park, 112 S.E. Columbia Way, directly east of the I-5 Bridge within the Fort Vancouver National Historic Site. This year, the free, family-friendly festival features live music by On a Lark, Another Shade of Bluegrass, and the Washington Old Time Fiddlers Association. There will also be fruit tree pruning demonstrations, arts and crafts for kids, ask-the-arborist sessions, Fort Vancouver Land Bridge tours and on-site food vendors.
To participate in the apple cider pressing, bring your own clean apples and clean containers to take home your freshly pressed cider. You can also get a free cutting to start your own piece of history. Each year during the festival, the Urban Forestry Commission gives away approximately 200 cuttings from the Old Apple Tree. While it’s challenging to successfully propagate these cuttings, it is possible. The commission would like to know how many people are able to successfully propagate their cutting, so if you’ve managed it, bring your story or a photo of your Old Apple Tree; a map will show where descendants of the Old Apple Tree live.
For more details, call Urban Forestry at 360-487-8308 or visit www.cityofvancouver.us/urbanforestry.