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— сёнэн-манга авторства Мэгуму Окады. Выпускалась издательствами Fujimi Shobo и Kodansha и выходила в журнале Monthly Dragon Jr. с 1992 по 1998 года. По мотивам манги были выпущены несколько OVA-серий и аниме-сериал, который транслировался по телеканалу TV Tokyo с 2 июля по 24 декабря 1998 года.

Сюжет
Действие происходит в альтернативном мире, похожем на землю в эпоху начала нашей эры. Однако главное отличие заключается в том, что здесь существует магия, а сильнейшие волшебники и воины регулярно устраивают между собой поединки. Землями правят 4 разных государства, но самым могущественным считается королевство Курода, которое вот уже 2000 лет держит роль первенства. Курдианцы знамениты своей колоссальной физической силой и магическими способностями. По традиции сильнейший воин Куроды удостаивается звания Севаара, так впервые за всю историю королевства им становится женщина по имени Элле Рагу. Хотя со стороны она кажется легкомысленной и непринуждённой, на её плечи взвалено огромное бремя: она должна тренировать своего младшего брата Гау Бана, всё время сражаться с сильнейшими врагами государства и не проигрывать, в противном случае Эль опозорит честь Куроды, которая оставалась непобедимой вот уже 2000 лет.

Список персонажей

 Сэйю: Мэгуми Хаясибара
 Главная героиня истории, 59 воин-севаар королевства Куруды и первая женщина, удостоенная данного звания. Получила звание в 14 лет, за 3 года по основных событий и известна как «мастер теней». Её родители умерли от болезни, которой заразилась и сама Эль, и должна была рано или поздно умереть, но её старший брат принимал участие в самых опасных заданиях, чтобы раздобыть деньги на лекарство и в результате подорвал своё здоровье. Из-за этого Эль терзает сильное чувство вины, так как она осознаёт, что брат сам был достоин звания воина севаара, но перестал быть воином из-за неё. Известна также как королева долгов, так как бесконечно находится в больших долгах. Непринуждённая и недальновидная боевая дева, преисполненная чувством чести воина. Любит много пить, а потом буянить, в результате разрушая новое здания и увеличивая свои долги. Однако на поле битвы становится серьёзной. В OVA-сериях имеет жёлтые волосы, в сериале — рыжие.

 Сэйю: Акио Мацуока
 Приёмный брат Эль, курдианский воин. В детстве на его деревню напали бандиты и убили всех, включая родителей Гая. После этого он встретил Эль и решил следовать за ней. (В OVA-сериях после нападения бандитов Гау вёл против них партизанскую борьбу, и через год встретил Элле). Изначально он стал следовать за Элле, чтобы в удобный момент украсть её деньги, но увидев её силу, решил верно следовать за ней. В начале истории он значительно слабее Эль, но его сила быстро начинает возрастать, и к концу истории он становится наравне с Эль сильнейшим курдианским воином. Вступает в близкие отношения с Кюо Рю, но когда в девушку влюбляется Скриб, он объявляет себя соперником Гау, таким образом образовав любовный треугольник. По мере развития сюжета Гау становится центральным персонажем в сражениях.
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 Сэйю: Юко Мидзутани
 Спутница главных героев, дочь известного мага Суй Рэма, который был наставником Эль и погиб после сражения с ней. Изначально Фолли яростно ненавидела Эль и мечтала убить её, но после того, как та спасла её из пожара, у Фолли возникли противоречивые чувства, с одной стороны ненависть её не пропала, с другой стороны она благодарна ей за спасение и видела её тёплый и искренний характер. Позже они стали хорошими друзьями, их отношения сложились ближе к сестринским. Однако Фолли всё ещё не могла простить Эль за убийство и решила закончить с вопросом на честном поединке. Позже однако выясняется, что Эль вовсе не убивала Суй Рэма, а его убил другой ученик — Луи Франсиль, уже обессиленного после боя с Эль, чтобы стравить друг с другом Эль и Фолли и самому заполучить наследство и титул наставника. В манге показано, что до смерти отца она заключила брак в возрасте 15 лет. Среди главных героев самая мудрая и смышлёная. Имеет неплохой опыт в любовных отношениях. Физически слаба и в бою полностью полагается на магию.

 Сэйю: Икуэ Отани
 До начала событий входила в группу охотников-септий, которые убивали демонов. Её дед — Джин Столла был лидером Фантома и самым великим из известных септиев. Однажды фантом попытался заполучить могущественного демона, но они не знали, что это был царь луны, который в результате уничтожил всю деревню охотников. Позже присоединяется к главным героям. Очень добрая и наивная, плохо понимает что-либо в любви, в частности, когда Скриб стал присылать ей любовные письма, она в упор не понимала их смысл. Не обладает особыми боевыми навыками, но достаточно слабо знает технику поимки демона, которую ещё долгое время должна оттачивать. Позже она узнаёт, что король Куроды Иба Столла был братом покойного деда. Он лично посетил Кюю Рю, чтобы обещать ей, что будет защищать её, пока та не найдёт себе близкого человека, который будет готов любить и защищать её.

 Сэйю: Мицуру Миямото
 Старший брат Эль. Был одним из сильнейших курдианских воинов и главным кандидатом на звание сивальдца. Также был известен крайней жестокостью в борьбе с врагами, за что получил прозвище «Чёрное крыло». Когда его родители умерли от болезни, а младшая сестра Эль заболела той же болезнью, он решил во что бы то ни стало вылечить её и принимал участия в самых тяжёлых и опасных заданиях, чтобы раздобыть побольше денег на лекарство. Диаз сумел спасти свою сестру, однако его здоровье было настолько сильно подорвано, что он был вынужден отказаться от мечты стать сивальдцем и отойти от сражений. В результате 58 сивальдцем стал Каин Фаланги. Он решил остаться жить в родном городе Блорахане, где его периодически посещают Эль с Гау. Однако несмотря на спокойную жизнь, его самостояние продолжало ухудшаться и Диаз стал постепенно терять зрение. Несмотря на свои недуги, он остаются сильнейшим воином и в нужных ситуациях помогал главным героям. В борьбе с ангелом Даркнессом, он сумел победить, однако его раны были настолько велики, что Диаз умер, но при этом остался стаять на ногах. Даркнесс запечатал душу Диаза в своём глазу, пока Кай Шинкс не восстановит своё тело. В конце истории появляется в образе ангела, чтобы помочь Гау в сражении.

 Сэйю: Каппэй Ямагути
 57 севаар Куроды, сильнейший воин, известен также как Скарфейс (от англ. лицо со шрамом), стал севааром в возрасте 16 лет, когда одержал победу на 55-м севааром Эвой Строллом. Играет важную роль в развитии Гау, подталкивая его на совершенство и дальнейшие тренировки. Выступает в роли наблюдателя за главными героями.

 Сэйю: Каппэй Ямагути
 Ученик короля Куроды, является ровесником Гау. Плохо относится к Эль, так как считает её слишком грубой, утверждая, что девушки должны быть изящными и заниматься домашним хозяйством. Но когда сталкивается с Кюо, влюбляется в неё с первого взгляда и начинает каждый день присылать любовные письма, но когда узнаёт, что с ней рядом живёт Гау (который читал любовные письма), невзлюбил его и объявил соперником. На первом сражении они сражались половину суток, но в результате вышла ничья. На втором сражении Гау одержал уверенную победу, срубив Скриба с одного удара. В результате Скриб признал за собой поражение и подарил Гау свои красные серьги, прося, чтобы тот позаботился о Кюо.

 Сэйю: Кодзи Цудзитани
 58-й севаар-отступник. Известен как «J». Из-за своей колоссальной силы, потерял рассудок и решил уничтожить Куроду. Во время боя впадает в состояние безумия, сражаясь как берсерк. Позже выясняется, что он уже 3 года назад умер, но поддерживал жизнь за счёт тёмных печатей, чей срок рано и поздно должен был истечь, в результате его побеждает Гау, а сам Кайн рассыпается на печати. Некоторые из них забирает Гау, через которых дух Кайна поможет ему в финальном сражении.

Медиа
Манга выла создана Мэгуму Окадой и начала выпускаться с 1992 года. В 1995 году была выпущена OVA-серия длительностью в 52 минуты (здесь Ель имеет жёлтые волосы и сиреневый костюм). В 1995 году был выпущен короткий OVA-сериал в 3 серии длительностью по 25 минут; 3 серии иногда упоминаются как полнометражный фильм. В 1998 году был выпущен аниме-сериал под названием , который транслировался по телеканалу TV Tokyo с 2 июля по 24 декабря 1998 года. В 2003 году была создана ещё одна OVA-серия, выполненная в 3D-графике. Здесь у Ель снова жёлтые волосы.

Критика
По мнению представителей сайта Anime News Network, сериал в общем получился интересным, хотя явно видно, что сериал слабо сосредоточен на сюжете, делая перевес на боевые искусства. Таким образом его создавали изначально для поклонников жанра. Сам сериал получился интересным, но ему не хватает развития сюжета, которое необходимо для создания великолепного аниме.

Примечания

Ссылки


The social network is in experimentation mode as it tries to figure out the best way to alert its 1.19 billion members to what's trending now.
Facebook is showing some members stories that are "Trending Now" inside the News Feed of the desktop application.
The in-feed placement, as pictured above, complements Facebook's other Web and mobile trending-topic trials, which started running over the summer. The company is clearly in experimentation mode as it tries to figure out the best way to alert its 1.19 billion members to what people are buzzing about.
"This is just a small test that's been running for a while," a Facebook spokesperson said when reached for comment.
Facebook's campaign to challenge Twitter as the world's water cooler has been in full swing ever since it added support for hashtags in June. The social network has also encouraged people to start embedding public posts on their Web sites and blogs.
As Facebook becomes more Twitter-like, it's only fitting that Twitter take on some of Facebook's qualities. Last week, the soon-to-go-public social network started inserting photos and videos into members' timelines to increase engagement and appeal to the masses.


When we launched Eternal Throne Bolster increased everyones item rating up to 250 (which was 8 higher than the highest possible gear rating of 242 at the time). This meant that gear was irrelevant in PvP as Bolster made an equal playing field. However, it is our design intent that players in all gameplay have some form of gear progression and so in Game Update 5.1 we lowered the effect of Bolster in PvP to 232. To compensate for the launch of Tier 4 gear we increased Bolsters effect in PvP to item rating 238.
Bolster is equal to item rating 238. - This is how it works today, this effectively puts you slightly above Tier 2 gear.
Bolster is equal to item rating 240. This would place bolster equal to the start of Tier 3 gear. There would now be an 8 rating difference between Bolster and the highest tier of gear (248). For reference this is identical to the gap that existed for Bolster prior to 5.0.
Bolster is equal to item rating 242. This would place Bolster at the top end of Tier 3 gear, meaning only Tier 4 gear is above it.
Let us know what you think? Do you like Bolster where it is? Do you want to see it go up?


From their site: "Sunshine Tavern is that warm, playful and welcoming environment you would expect from a tavern. Most of all, it's fun. This is a bar, a clubhouse, a gathering place for family, friends and everyone in between. Come in for a drink, linger over dinner, or have a go at the 14-foot shuffleboard table or our vintage Ms. Pac Man and Donkey Kong games."


Bixby's annual NIGHT OF CHAMPIONS is tonight at Lee Snider Field at 8:15pm under the lights!
We are expecting 50-60 of our athletes to clean 225lbs+ and 3-5 be over 300lbs!!!
Total=2+4burpee T2B with my wife Heather. Good job babe!
13:24 rxd -took me to the pain cave.
Wod. Rx'd w/ Kevin O.
Wod with Shawn… what he said!
OMG Jessica..I was tired just reading your strength!!! You are a beast!!
Great job Chrissy, way to keep moving and never quit!
Thanks for letting me slow you down Jordan!
I ran and rowed. Max rowed and biked.
WOD with Nicole's dad Mike – great work today!


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See inside Gabrielle Union and Dwyane Wade's $29 million Miami mansion
The home also boasts sunset views from every room, according to the listing.
Want to live like you're at a private beach resort? You can if you buy this insanely gorgeous Miami Beach property that belongs to Dwyane Wade and Gabrielle Union.
Living here would make feel like being on vacation every day of the year!Elliman.com
The recently retired NBA star and his actress wife recently dropped the price of the 14,000-square-foot home from $32.5 million to $29 million. And, yes, even with the reduction, it's still a hefty price tag, but this mansion seems worth every penny.
Wade, who spent the majority of his basketball career playing for the Miami Heat, has owned this place since 2010. So it's no surprise that the property has its own basketball court.
It's likely the outdoor amenities made this house so enticing to the Hollywood power couple. It's like living at your own private resort or being on vacation 24/7.
There's a gorgeous pool overlooking Biscayne Bay, an outdoor kitchen and bar area, and plenty of places to sit and soak up that bright Florida sunshine.
Step inside this classic American manor.Elliman.com
Inside the main house, you'll find rich accents and classic details. The chef's kitchen features dark wood cabinets, while the dining room has massive windows looking out to the picturesque view. Plus, there are plenty of formal and informal living areas to entertain friends and family.
Many of the rooms have wood beams on the ceiling.Elliman.com
One of the many living areas in the homeElliman.com
There's also a casual indoor bar that could be a fun place to watch the game — or, you know, a cheerleading competition. And there's a professional home theater for movie nights with the family.
The home has a total of six bedrooms, including a master suite that has its own terrace and sitting area, plus a spa-like bathroom and a closet that looks like it could be the size of a small store.
Check out that view!Elliman.com
Another amazing feature? The home also boasts sunset views from every room, according to the listing.
Brett Harris of Douglas Elliman, the listing agent for the property, declined to comment.
See more pictures at Douglas Elliman.
Dr. Oz's favorite room: His amazing basement (with its own basketball court!)
This story was originally published September 20, 2019.

redpajama_set_name: RedPajamaCommonCrawl


It's a blend that checks all the boxes: Anti-Aging, Anti-Shriveling, Anti-Chafing, Anti-Dryness, Anti-Sagging, yet Botanically Bountiful.
The 'other' down-there products (powders, creams, wipes) for men are all about anti-wetness and anti-odor, leaving a strong, distinctive scent of artificial chemicals. TAME the BEAST® Multipurpose Anti-Chafe Nutt Butter is derived from ingredients such as Jojoba, Aloe, Comfrey Root, Calendula, Chamomile, Shea, Cocoa, Mango, Rosemary, Eucalyptus, Lavender, and Vitamin E, giving you a more natural and welcoming scent.


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Upcoming deadline on 31 March 2016 to comply with revised disclosure rules for significant shareholdings
Alexander Vogel
Samuel Ljubicic
As of 1 January 2016, revised regulations for the disclosure of significant shareholdings in listed companies and amendments to takeover regulations took effect. Pursuant to the transitory provisions, facts that occurred before 1 January 2016, but trigger a reporting obligation under the new law, must be reported by 31 March 2016.
On 19 June 2015, the Swiss Parliament finalized the new "Financial Market Infrastructure Act" (FMIA) which was enacted by the Federal Council together with the implementing regulation, the Financial Market Infrastructure Ordinance (FMIO), at the beginning of 2016. At the same time, FINMA issued its own ordinance on financial market infrastructure (FMIO-FINMA). The new regulatory framework regulates key market infrastructures in Switzerland, such as securities exchanges, trading platforms, central depositaries and payment systems as well as trading in derivatives. It also incorporates many former provisions of the Stock Exchange Act (SESTA), among others those on public takeovers and those relating to the disclosure of significant interests in listed companies. The implementing provisions on reporting requirements for securities trading, on clearing duties for derivatives, as well as the new rules on disclosure of significant interests in listed companies are contained in the FMIO-FINMA.
While in many aspects, the new regulatory framework took over the regulations of the SESTA and its former implementing provisions, it also brought some important changes not only with regard to the rules applicable to public offers, both in substance (see Act leads to amendments of public takeover law) and in form (see New rules for publication of documents relating to public tender offers), but also with regard to the rules on disclosure of significant interests in listed companies. The most important effect of these new disclosure rules is that on the one hand both the owners of significant interests in listed companies as well as the asset manager or other persons managing such interests may have to make certain disclosures and that persons authorized to exercise voting rights of listed companies in their discretion – based on an asset management agreement or otherwise – have to take such managed shares into account when determining their own disclosure obligations.
Also under the amended rules introduced by the FMIA, the main reporting obligation for any significant shareholding remains with the beneficial owner of such holding and the relevant thresholds (3, 5, 10, 15, 20, 25, 331/3, 50 and 662/3%) remain the same. Pursuant to the new provision in Section 10 FMIO-FINMA, a beneficial owner is defined as a person who controls the voting rights, i.e. who has the ultimate power to control the exercise of the voting rights in his or her sole discretion (including the power to authorize a third party to exercise the voting rights) and bears at the same time the economic risk of the relevant holdings. In addition to this reporting obligation of persons exercising voting rights of positions economically held for their own account, the FMIA introduced a reporting obligation of persons who, even though not qualifying as beneficial owners, have the de facto power to exercise voting rights in their sole discretion. This reporting obligation is broadly similar to an earlier provision contained in the former SESTO-FINMA, which was, however, qualified as overreaching for lack of sufficient basis in the SESTA by a decision of the Federal Supreme Court in mid 2013 and as a consequence thereof invalidated. The new rule only addresses holdings in voting securities and thus, derivatives on such voting securities are not captured by this regime.
As a consequence of this new rule, the individual or firm authorized to exercise the relevant voting rights has to add such voting rights to its own positions when determining the relevant total positions, i.e. when determining whether a relevant threshold has been reached or crossed. Conversely, financial intermediaries who only buy and sell equity positions for their clients but do not have the right to exercise the voting rights on a discretionary basis have no obligation to take such equity securities into account for disclosure purposes (unless in case of a direct involvement in the framework of a takeover offer for such equity securities, e.g. as bidder or friendly target).
Mainly affected by this new rules are, for instance asset managers (or in certain cases proxy advisors) authorized to exercise the voting rights or cause to have such voting rights be exercised in a particular way, e.g. by completing the relevant voting instructions. It is important to note that on the one hand the person granting the right to exercise voting rights on a discretionary basis is not released from including the relevant equity securities in its own disclosure reporting (if any) and the person obliged to report based on his or her authority to exercise voting rights on a discretionary basis (in addition to his or her own positions) has to disclose the number of the voting rights reported based on such authority. In case of a group of companies active in the financial sector, where e.g. one entity provides asset management services to clients and thus has the right to exercise voting rights on a discretionary basis, such equity securities need not to be reported separately by the asset management entity but have to be reported by the ultimate parent together with all other aggregated holdings of the group and in addition, the parent has to disclose the number of voting rights exercised by the asset management entity – but not held for its own account – separately.
Another important change relates to a simplified reporting regime in case of indirect share ownership, for instance in case of a group of companies. Under the previous disclosure regime in force up to the end of 2015, the entire chain of entities between the direct holder of the relevant position and the ultimate beneficial owner needed to be disclosed. Under the regime introduced by the FMIA and the FMIO-FINMA, the disclosure of the intermediate entities is not required any longer, but it is enough to report the direct holder and the ultimate beneficial owner. In addition entities of the same group of companies, i.e. under the control of the same parent company, do no longer qualify as parties acting in concert and thus have no longer a group reporting obligation, since all positions held by the group are deemed to be held indirectly by the parent company itself (or, if applicable by its beneficial owner(s)).
Further changes include the abolition of the former regime for the disclosure of usufruct – with the consequence that the granting of a usufruct does no longer qualify as a sale of the relevant shares, but such equity securities remain to be reported for disclosure purposes by the owner, while the beneficiary of the usufruct needs to report the relevant holdings (in addition to the owner) in case he or she is entitled to exercise the voting rights.
While the FMIA, the FMIO and the FMIO-FINMA entered into force, as mentioned above, on 1 January 2016, the transitory provisions provide that any facts dating back to the period before 31 December 2015 triggering under the new regime of the FMIA (e.g. an authority to exercise voting rights granted before 1 January 2016), such fact must be reported by 31 March 2016. To the extent no new reporting obligation is triggered, the notifications made under the former disclosure regime, i.e. before the end of 2015, will remain valid to the extent made in full compliance with such former rules until a new disclosure threshold has been reached or crossed or reported facts change. If a notification after 1 January 1 2016 was made in accordance with the old disclosure regime (which is permissible until 31 March 2016) an amended notification complying with the new rules needs to be submitted by 31 March 2016. As of 1 April 2016, all notifications will have to be made in compliance with the new rules.
Law Reform on Company Law – Aspects of Corporate Governance
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ESG & Compliance Update: Switzerland Enacts Non-Financial Reporting and Due Diligence Requirements
Switzerland has updated its legislation in 2021 and in 2022 to include transparency and non-financial reporting requirements, specifically on CO2 goals, social issues, employee-related issues, respect for human rights and combating corruption as well as due diligence and transparency duties in relation to minerals and metals from conflict-zones and child labour.
We have prepared user-friendly che…
LexCast: Happy New Year From the MLL NexGen Incubator – Find Out What 2022 Has in Store for You!


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Ryan Stringer Memorial Scholarships 2018
Alhambra POA hosted our fifth annual Ryan Stringer Memorial Scholarship Night on Wednesday, May 23. Out of a record-breaking number of applicants, five high school seniors were selected to each receive a $1,000 scholarship. They were chosen for their essays on what they learned about and from Ryan Stringer's legacy, as well as why they need a scholarship. We strive to keep Ryan's memory alive both within the department and community through generations with our scholarship approach and night of remembering him.
The evening began with welcome remarks by Alhambra Police Department Chief Vu. Scholarship Chairperson Corporal Grant Spencer then introduced the scholarship and Ryan's parents, Debbie and Sonny, to speak about their son and present a slideshow before recognizing the recipients. The five students that we honored were Kenneth Tiet, Valerie Montelon, Alejandro Salazar, Kimberly Pham, and Bliss Tafolla-Aguirre.
• Kenneth is a senior at Mark Keppel High School and will be attending Pasadena City College.
• Valerie is a senior at San Gabriel High School and will be attending Cal Poly Pomona to study mechanical engineering.
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text:
\section{Introduction}
\label{sec:intro}

Most stars appear to form in star clusters
\citep{lada03,lada09,portegies_zwart10} and so star formation is
inextricably linked with star cluster formation.  Recent advances in
observations and theory have allowed us to construct a basic picture
of cluster formation in which clusters form dynamically cool
(sub-virial), and highly substructured.

Clusters form in highly turbulent molecular clouds.  These clouds are
highly substructured, containing dense clumps and filaments
\citep{williams99,williams00,carpenter08} which are presumably formed
by the decay of supersonic turbulence
\citep{maclow04,ballesteros-paredes07}. Stars and small stellar groups
form in these dense regions and are unsurprisingly observed to have a
high degree of substructure when young
\citep{larson95,elmegreen00,testi00,cartwright04,gutermuth05,allen07,schmeja06,schmeja08},
clustering in young stellar groups has even been observed in the SMC
\citep{schmeja09} and LMC \citep{bastian09}.  The same behaviour is
seen in simulations of cluster formation
\citep{klessen00,klessen01,bate03,bonnell03,bate09,offner09},
including in comparison tests between AMR and SPH techniques
\citep{federrath10}.

Clusters are observed to lose their substructure as they evolve,
becoming smooth and roughly spherical
\citep{cartwright04,schmeja06,schmeja08}. \citet{goodwin04} have shown
that substructure can only be erased in clusters if the clusters are
initially cool (sub-virial) (see also Maschberger et al. 2010).
Both observations of pre-stellar cores
\citep{belloche01,andre02,walsh04,peretto06,kirk07} and stars
\citep{peretto06,proszkow09} show that they indeed appear to be
sub-virial, a property also found in simulations of cluster formation
(Klessen \& Burkert 2000; Offner et al. 2009; Maschberger et al. 2010).

Following Allison et al. (2009b) we conduct $N$-body simulations of a
large number of initially sub-virial, fractal star clusters.  In
Section~\ref{sec:init} we describe our simulations. In
Section~\ref{sec:results} we describe our main results, specifically
the early onset of dynamical mass segregation and interesting
`post-collapse' evolution. In Section~\ref{sec:disc} we discuss the
results, and we summarise and conclude in Section~\ref{sec:conc}.

\section{Initial Conditions}
\label{sec:init}

We perform 160 $N$-body simulations with 1000 stars each, in which the
initial conditions are cool and clumpy.  We vary the level of
substructure and initial virial ratio, and conduct ensembles of
simulations with the same initial conditions, varying only the initial
random number seed used to initialise the simulations.

To create initial substructure in our simulations we use a fractal
stellar distribution. Using a fractal distribution provides a
parameterisation of substructure using only a single number: the
fractal dimension.  (Note that we are not claiming that clusters are
actually initially fractal, although they may be
\citep{elmegreen01,cartwright04}, just that this provides a simple
descriptor of substructure that is easy to reproduce).

The fractal stellar distributions were generated following the
method of \citet{goodwin04}. The method begins by defining a cube
of side $N_{{\rm div}}$ (we use $N_{{\rm div}} = 2$ throughout),
inside of which the fractal will be built. A
first-generation parent is placed at the centre of the cube, from
which are spawned $N_{{\rm div}}^{3}$ sub-cubes, each containing a
first-generation child in its centre. The fractal is then built
by determining which of the children themselves become parents,
and spawn their own offspring. This is determined by the fractal
dimension, $D$, where the probability that a child becomes a
parent is $N_{\rm div}^{(D-3)}$. For a lower fractal dimension
less children will mature and so the final distribution will
contain more structure. Any children which do not become parents
in a given step are removed, along with all of their parents. A
small amount of noise is then added to the positions of the
remaining children, preventing the final cluster from having
a gridded appearance, and the children become parents of the next
generation. Each new parent then spawns $N_{\rm div}^{3}$
second-generation children in $N_{\rm div}^{3}$ sub-sub-cubes,
with each second-generation child having a $N_{\rm div}^{(D-3)}$
probability of becoming a second-generation parent. This process
is then repeated until there are substantially more children than
required. The children are pruned to produce a sphere from the
cube and are then randomly removed (so maintaining the fractal
dimension) until the required number of children are left. These
children then become the stars in the cluster.

To determine the velocity structure of the cloud, children inherit
their parent's velocity plus a random component that decreases with
each generation in the fractal.  The children of the first generation
are given random velocities from a Gaussian of mean zero\footnote{Here
  the variance is unimportant as the velocities are scaled to the
  desired virial ratio once the final spatial distribution is
  obtained, but the method can also be used to match the
  \citet{larson81} relations if desired
  \citep[see][]{goodwin04}.}. Each new generation then inherits their
parent's velocity plus an extra random component that becomes smaller
with each generation.  This results in a velocity structure in which
nearby stars have similar velocities, but distant stars can have very
different velocities.  Finally, the velocity of every star is scaled
to obtain the desired total virial ratio for the cluster.

\begin{center}
\begin{table}
  \begin{tabular}{|c|c|c|c|c|}
\hline
        &  \multicolumn{4}{|c|}{$D$} \\
$Q$     &  1.6        &  2.0        &  2.6        &  3.0  \\
\hline
0.3     &  a1.01--50  &  a2.01--10  &  a3.01--10  &  a4.01--10   \\
0.4     &  b1.01--10  &  b2.01--10  &  b3.01--10  &  b4.01--10   \\
0.5     &  c1.01--10  &  c2.01--10  &  c3.01--10  &  c4.01--10   \\
\hline
  \end{tabular}
\caption{Notation for run identification where $D$ is the initial
  fractal dimension, and $Q$ is the initial virial ratio of each
  simulation. The numbers 01--50 and 01--10 are the identifiers for
  each individual run.  Within each ensemble only the random number
  seed used to generate the initial conditions is
  changed. \label{tab:runs}}
\end{table}
\end{center}

The simulations contain 1000 stars, have an initial maximum radius of
1 pc, include no primordial binaries or gas and a three-part power law
is used to produce an initial mass function \citep[IMF,][]{kroupa02},

\begin{equation}
  N(M) \propto \left\{
  \begin{array}{r}
    M^{-0.3} \quad m_0 \leq M/\ensuremath{\textrm{ M}_{\odot}} < m_1, \\
    M^{-1.3} \quad m_1 \leq M/\ensuremath{\textrm{ M}_{\odot}} < m_2, \\
    M^{-2.3} \quad m_2 \leq M/\ensuremath{\textrm{ M}_{\odot}} < m_3, \\
  \end{array}
  \right.
\end{equation}

\noindent with $m_0=0.08\ensuremath{\textrm{ M}_{\odot}}$, $m_1=0.1\ensuremath{\textrm{ M}_{\odot}}$, $m_2=0.5 \ensuremath{\textrm{ M}_{\odot}}$ and
$m_3=50\ensuremath{\textrm{ M}_{\odot}}$. No stellar evolution is included because of the short
duration of the simulations ($\sim 4$ Myr).  We use the {\sc starlab}
$N$-body integrator {\sc kira} to run our simulations
\citep{portegies_zwart01}.

In this study we explore a range of fractal dimensions and virial
ratios. The fractal dimensions investigated are
$D=1.6,~2.0,~2.6~\textrm{and}~3.0$ (since these values correspond to
the number of maturing children, $N_{{\rm div}}^D \equiv 2^{D}$ ,
being an integer), where $D=1.6$ produces a large amount of structure,
and $D=3.0$ produces a uniform sphere. We investigate virial ratios of
$Q = 0.3,~0.4~\textrm{and}~0.5$, we define the virial ratio as
$Q=T/|\Omega|$ (where $T$ and $|\Omega|$ are the total kinetic and
total potential energy of the stars, respectively), hence virial
equilibrium is $Q=0.5$.

It is important to note that fractal initial conditions are inherently
stochastic: statistically identical fractals (i.e., the same fractal
dimension), can appear very different to the eye, and can evolve in
very different ways (see Section~\ref{ssec:stocasticity}).  Therefore,
it is vital to perform large ensembles of simulations with different
random number seeds.  We have therefore simulated 50 $D=1.6$, $Q=0.3$
(a1) clusters (as they have the most interesting evolution), and
restricted our analysis of all other combinations of $D$ and $Q$ to 10
clusters each.  The identifiers and initial conditions of each
ensemble are presented in table~\ref{tab:runs}.

To quantify mass segregation we use the minimum spanning tree (MST)
method \citep{allison09}. This method compares the MST of the $N$ most
massive stars with the average MSTs of $N$ randomly selected stars.
The ratio of these two MST lengths gives a quantitative measure of the
concentration of the massive stars and hence a value of the mass
segregation in the cluster,

\begin{equation}
\Lambda=\frac{\langle l_{\rm norm} \rangle}{l_{\rm massive}}\pm
\frac{\sigma_{\rm norm}}{l_{\rm massive}}
\end{equation}

\noindent where $\Lambda$ is the measure of mass segregation,
${\langle l_{\rm norm} \rangle}$ is the average length of the random
MSTs, $l_{\rm massive}$ is the length of the massive star MST and
$\sigma_{\rm norm}$ is the error in the random MST length. The value
$\sigma_{\rm norm}/l_{\rm massive}$ is the 1 $\sigma$ error in
$\Lambda$.

In this paper, mass segregation is calculated for the entire stellar
content (i.e. ejected stars are not removed from the simulation) in
all three dimensions. We note that an observer will see only two
dimensions, and may not identify all cluster members, in particular
low-mass stars and stars that have been ejected from the cluster.
Allison et al. (2009a) show that there is little difference between
the mass segregation measure in two and three dimensions when using
mass segregated Plummer spheres. However, as with all mass segregation
measures, if using the measure in two dimensions projection effects
may cause differences depending on orientation. Unfortunately, this is
unavoidable. Including all stars is useful theoretically, however it
does not allow a direct comparison with observational data.

\section{Results}
\label{sec:results}

\subsection{Rapid dynamical mass segregation}
\label{ssec:dyn_ms}

\begin{figure*}
  \begin{center}
    \setlength{\subfigcapskip}{10pt}
\subfigure[0 Myr]{\label{fig:a1.34.001}
\includegraphics[scale=0.5,angle=270]{faa11a034.dat.001.ps}}
\subfigure[0.8 Myr - Formation of core]{\label{fig:a1.34.081}
\includegraphics[scale=0.5,angle=270]{faa11a034.dat.081.ps}}
\subfigure[1 Myr - End of core]{\label{fig:a1.34.102}
\includegraphics[scale=0.5,angle=270]{faa11a034.dat.102.ps}}
  \end{center}
  \caption[bf]{Run a1.34 -- \textit{Top:} 2 dimensional stellar
    distributions at (a) 0 Myrs - the initial distribution, (b) 0.8
    Myrs - the formation of the dense core and (c) 1 Myr - the end of
    the dense core and initial dynamical mass segregation. Triangles
    indicate the positions of the 10 most massive
    stars. \textit{Bottom:} The evolution of $\Lambda$ with $N$ for
    (a), (b), (c); as described above. The error bars show $1\sigma$
    deviations.}
  \label{fig:a1.34}
\end{figure*}

In \citet[][hereafter Paper I]{allison09b} we showed that cool
($Q=0.3$), and clumpy ($D=1.6$) clusters can dynamically mass
segregate on a timescale close to the initial crossing time of the
system ($\sim 1$~Myr).  Figure~\ref{fig:a1.34} shows the early
evolution and onset of mass segregation in such a cluster. The top
panels show the spatial distributions of the cluster at times $\sim 0.01,
0.81$ and $1.02$~Myr (left to right), whilst the lower panels show the
mass segregation ratio $\Lambda$ for each of these snapshots -- the
higher the value of $\Lambda$, the greater the degree of mass
segregation.  As is clear from the figure, the cluster evolves from an
initially non-mass segregated and clumpy distribution, into a smooth
and mass segregated one.

In paper I we argued that this rapid dynamical mass segregation is due
to the collapse of the cool cluster forming a very dense, but
short-lived core (at $\sim 0.8$~Myr in the example shown in
Fig.~\ref{fig:a1.34}).  These dense cores (for $D=1.6$, $Q=0.3$) tend
to contain about half of the mass of the cluster, are roughly $0.1$ --
$0.2$~pc in radius, and survive for $0.1$ -- $0.2$~Myr ($10$ -- $20$
crossing times in the core).

\citet{spitzer69} showed that the timescale for mass segregation,
$t_{\rm seg}$, for a star of mass $M$ depends on how massive that star
is relative to the average mass of a star in a cluster, $\langle m
\rangle$,

\begin{equation}
t_{\rm seg }(M) \approx \frac{\langle m \rangle}{M} t_{\rm relax},
\label{eq:tseg}
\end{equation}

where $t_{\rm relax}$ is the relaxation time of the cluster, which is
related to its crossing time, $t_{\rm cross}$, by

\begin{equation}
t_{\rm relax }\approx \frac{N}{8\ln N} t_{\rm cross}.
\label{eq:trelax}
\end{equation}

Eq.~\ref{eq:tseg} can be rewritten as

\begin{equation}
t_{\rm seg } \approx \frac{\langle m \rangle}{M}
\frac{N}{8\ln{N}} t_{\rm cross }.
\label{eq:tdense.exp}
\end{equation}

For the $D=1.6$, $Q=0.3$ initial conditions used in paper I, typical
values for these parameters are $N \sim 300$ -- $500$, $t_{\rm cross }
\sim 0.01$ -- $0.2$~Myr, $\langle m \rangle \sim 0.4 \ensuremath{\textrm{ M}_{\odot}}$ (typical
for standard IMFs).  The core has a lifetime of $0.1$ -- $0.2$~Myr in
which it can mass segregate giving a mass to which the core can
segregate of $M \sim 2$ -- $4 \ensuremath{\textrm{ M}_{\odot}}$.  In Fig.~\ref{fig:a1.34} the
cluster is mass segregated to the 20th most massive star, which has a
mass of a few $\ensuremath{\textrm{ M}_{\odot}}$, in good agreement with our simple analytical
model.

The reason that a dense core can form is that the cluster is
both cool {\em and} clumpy: cool clusters will initially collapse, but
cool and clumpy clusters can collapse further.  The potential
energy, $\Omega$, of a cluster of mass $M_{\rm clus}$ and radius $R$ is

\begin{equation}
\Omega = - \eta \frac{GM_{\rm clus}^2}{R},
\end{equation}

\noindent where $\eta$ is a structure parameter whose value depends on
the choice of $R$ (e.g., is it the core radius or the half-mass
radius?), and the structure of the cluster (e.g., is it clumpy,
Plummer, or uniform density?) \citep[see also,][]{portegies_zwart10}.
For example, for a Plummer sphere, if $R$ is the Plummer radius then
$\eta \sim 0.3$.

If a cluster has an initial potential energy $\Omega_0$ (with radius
$R_0$ and structure parameter $\eta_0$), and an initial virial ratio
$Q_0$, then the initial total energy $E_0$ is

\[
E_0 = -\eta_0 \frac{GM_{\rm clus}^2}{R_0} (1 - Q_0).
\]

Whatever the initial conditions, a (bound) cluster will attempt to
reach virial equilibrium and a relaxed configuration (something like a
Plummer sphere, or King profile with a concentration
parameter\footnote{We define the concentration parameter as $c={\rm
    log}_{10}(r_{\rm virial}/r_{\rm core})$} $\approx 2-3$, for an a1
type cluster).  Therefore, the final energy $E_f$ of the cluster (with
potential energy $\Omega_f$, radius $R_f$, structure parameter
$\eta_f$, and virial ratio $Q_f=0.5$) will be

\[
E_f = -\eta_f \frac{1}{2} \frac{GM_{\rm clus}^2}{R_f}
\]

\noindent (assuming no mass is lost).  Equating these equations gives
the degree of collapse (or expansion if initially warm) of the cluster

\begin{equation}
\frac{R_0}{R_f} = \frac{\eta_0}{\eta_f} 2(1 - Q_0).
\end{equation}

Clearly, to induce dynamical mass segregation on a short timescale,
$R_0/R_f$ must be as large as possible to cause the maximum degree
of collapse.  This implies that both $\eta_0/\eta_f$ and $2(1 -
Q_0)$ need to be large.

Obviously, making $2(1 - Q_0)$ large means making $Q_0$ as small as
possible, but even with an initially static stellar distribution with
$Q_0 = 0$, $2(1 - Q_0)$ can never be greater than two (this is why
Bonnell \& Davis 1998 did not see rapid, early mass segregation).
Realistically, it is difficult to imagine $Q_0$ being much less than
$0.2$ or $0.3$ as the stars {\em must} initially have some relative
velocities.

As stated above, the cluster will not just relax into virial
equilibrium, it will also attempt to reach a basic statistical
equilibrium which is a smooth, centrally concentrated distribution
(like a Plummer sphere or King model if tidally truncated).  Therefore
the final structure parameter will be $\eta_f \sim 0.3$ when the
scale radius is the Plummer radius.

Numerical experiments we have carried out show that the structure
parameter for a fractal of dimension $D=1.6$ is $\eta_0 \sim 1.1 \pm
0.1$, for $D=2.0$, $\eta_0 \sim 0.8 \pm 0.1$ (note that different
realisations of $D=1.6$ and $D=2.0$ fractals have a large variation in
their structure parameters), for $D=2.6$, $\eta_0 \sim 0.7$, and for
$D=3.0$, $\eta_0 \sim 0.6$.  For each of these $\eta$ values the scale
radius is the total radius of the fractal.  Unfortunately, it is very
difficult to exactly compare the $\eta$ of a Plummer model and the
$\eta$ of a fractal as the radii are defined differently.  The
half-mass radius of fractal models varies quite significantly (and its
meaning is also rather unclear in a fractal) and so does not provide a
useful comparison radius either.

\subsection{Mass segregation in clusters with different $D$ and $Q$}
\label{ssec:DandQ}

The analysis above suggests that the initial virial ratio and the
initial fractal dimension of a cluster are the crucial parameters in
determining whether that cluster will be able to rapidly dynamically
mass segregate.  In particular, the warmer (higher-$Q$), and the
smoother (higher-$D$) a cluster is, the lower the maximum central
density, and hence less dynamical mass segregation will occur.

In Fig.~\ref{fig:DandQ} we show the typical evolution of $\Lambda$
with time for clusters with different initial virial ratios and
fractal dimensions for $N=10,20 {\rm ~and~} 50$, the full
version of this figure, showing the evolution of all of the
simulations, can be found in the supplementary data.  In the top left
is our canonical $Q=0.3$, $D=1.6$ cluster from paper I.  From left to
right, the initial virial ratio increases from $Q=0.3$ to 0.4 and 0.5
(virialised).  From top to bottom, the fractal dimension increases
from $D=1.6$ (very clumpy) to $2.0, 2.6$ and 3.0 (roughly a uniform
density sphere).

It would be expected from our earlier argument that lower-$Q$ and
lower-$D$ clusters will collapse to a denser state, and hence show
more rapid and more pronounced dynamical mass segregation.  This is
exactly what is seen in Fig.~\ref{fig:DandQ}: faster and more intense
mass segregation at the top left (cool and clumpy clusters), and no
appreciable mass segregation at all at the bottom right (virialised,
uniform density clusters). The trend in the typical evolution of
clusters in our parameter space shown in Fig.~\ref{fig:DandQ} is
exactly what we would expect to see following the theoretical argument
in Section~\ref{ssec:dyn_ms}.

Whilst the behaviour of `typical' clusters is exactly what is
expected, many individual clusters show unusual and unexpected
behaviour. Examination of each simulation (see the supplementary data)
shows that, whilst the general pattern of evolution with $D$ and $Q$
holds, there is a large degree of stochasticity due to each fractal
being different in detail to every other fractal.

\begin{figure*}
  \begin{center}
    \setlength{\subfigcapskip}{10pt}
\subfigure[$D=1.6; Q=0.3$ -- a1.21]{\label{fig:a1.21}
\includegraphics[scale=0.25,angle=270]{plot.faa11a021.dat.ps}}
\subfigure[$D=1.6; Q=0.4$ -- b1.05]{\label{fig:b1.05}
\includegraphics[scale=0.25,angle=270]{plot.fab11a005.dat.ps}}
\subfigure[$D=1.6; Q=0.5$ -- c1.06]{\label{fig:c1.06}
\includegraphics[scale=0.25,angle=270]{plot.fac11a006.dat.ps}}

\subfigure[$D=2.0; Q=0.3$ -- a2.08]{\label{fig:a2.08}
\includegraphics[scale=0.25,angle=270]{plot.faa21a008.dat.ps}}
\subfigure[$D=2.0; Q=0.4$ -- b2.08]{\label{fig:b2.08}
\includegraphics[scale=0.25,angle=270]{plot.fab21a008.dat.ps}}
\subfigure[$D=2.0; Q=0.5$ -- c2.06]{\label{fig:c2.06}
\includegraphics[scale=0.25,angle=270]{plot.fac21a006.dat.ps}}

\subfigure[$D=2.6; Q=0.3$ -- a3.04]{\label{fig:a3.04}
\includegraphics[scale=0.25,angle=270]{plot.faa31a004.dat.ps}}
\subfigure[$D=2.6; Q=0.4$ -- b3.02]{\label{fig:b3.02}
\includegraphics[scale=0.25,angle=270]{plot.fab31a002.dat.ps}}
\subfigure[$D=2.6; Q=0.5$ -- c3.09]{\label{fig:c3.09}
\includegraphics[scale=0.25,angle=270]{plot.fac31a009.dat.ps}}

\subfigure[$D=3.0; Q=0.3$ -- a4.02]{\label{fig:a4.02}
\includegraphics[scale=0.25,angle=270]{plot.faa41a002.dat.ps}}
\subfigure[$D=3.0; Q=0.4$ -- b4.03]{\label{fig:b4.03}
\includegraphics[scale=0.25,angle=270]{plot.fab41a003.dat.ps}}
\subfigure[$D=3.0; Q=0.5$ -- c4.03]{\label{fig:c4.03}
\includegraphics[scale=0.25,angle=270]{plot.fac41a003.dat.ps}}

  \end{center}
  \caption[bf]{Generic examples from the investigated $D$ and $Q$
    values. Plots show the evolution of mass segregation ($\Lambda$)
    with time for $N=10$ (\textit{solid}, includes error bars); $N=20$
    (\textit{dashed}); $N=50$ (\textit{dot-dash}). The red line
    indicates a $\Lambda$ of unity i.e. no mass segregation. The error
    bars show a 1$\sigma$ deviation. A movie showing the evolution of
    (a) a1.21 can be downloaded at
    http://www.astro.group.shef.ac.uk/stars.html}
  \label{fig:DandQ}
\end{figure*}

\subsection{Stochasticity}
\label{ssec:stocasticity}

The supplementary data shows that a number of simulations do not show
the behaviour that we might expect for their $D$ and $Q$ values.  The
evolution of fractal clusters depends significantly on the specific
initial conditions of the cluster. The systems are inherently chaotic
and so each new random number seed can deliver completely different
evolution. Phenomena which occur during the evolution of a cluster
(such as mass segregation) can also be very transient. In some
systems, $\Lambda$ may change by a large factor on short
timescales. In this section we have chosen a few examples which
demonstrate the stochasticity and transience in the evolution of cool,
clumpy clusters.

There are several $D=1.6, Q=0.3$ clusters which appear to have little
or no mass segregation, for example run a1.20 (see
Fig.~\ref{fig:faa11a020}). In this cluster there appears to be no
significant mass segregation at any time during the 4 Myr of the
simulation for $N=10,20 {\rm ~and~}
50$. Fig.~\ref{fig:faa11a020.ext} shows the evolution of $\Lambda$ for
run a1.20 in more detail than Fig.~\ref{fig:faa11a020.3}. In this plot
we show $\Lambda$ for $N=4, 6, 8, 10 {\rm ~and~} 12$. It is
now clear that the cluster {\em does} mass segregate, but only for
stars more massive than the 6\ensuremath{^{\rm th}}~most massive star. In fact, a
substantial multiple system consisting of the 4 most massive stars is
formed in this cluster. Mass segregation is only present for the
6\ensuremath{^{\rm th}}~most massive stars because the 7\ensuremath{^{\rm th}}~most massive star is
ejected early in the simulation, thereby enlarging the length of all
MSTs that include more than 7 stars. Mass segregation for $N=4$ occurs
at 0.8 Myr with $\Lambda = 3.4^{+1.8}_{-1.5}$, and by 2 Myr
$\Lambda$ for the four most massive stars has risen to
$50.9^{+22.0}_{-19.9}$, with a total MST length of 13000 AU (an
average separation of 3250 AU), $\Lambda$ is very high here because
many lower mass stars have been widely spread from the cluster, making
the random MSTs large. This also explains the large error values.
Fig.~\ref{fig:faa11a020.ext} illustrates the rapid variations in
$\Lambda$ for the small-$N$ system of the most massive stars, and the
fairly smooth variation for larger $N$.

Superficially, run c4.10 looks very similar to run a1.20, for $N=10,20
{\rm ~and~} 50$, in that it shows no evidence for mass segregation
throughout the simulation. When we investigate this cluster in detail,
we find that the two simulations are completely different as this
cluster does not undergo a dense collapse phase. It becomes only
slightly mass segregated at 3.2 Myr with $\Lambda$ for $N=4$ of $
3.1^{+1.5}_{-1.1}$.

\begin{figure}
  \begin{center}
    \setlength{\subfigcapskip}{10pt}
\subfigure[]{\label{fig:faa11a020.3}
\includegraphics[scale=0.3,angle=270]{plot.faa11a020.dat.ps}}
\subfigure[]{\label{fig:faa11a020.ext}
\includegraphics[scale=0.3,angle=270]{plot.faa11a020.dat.ext.ps}}
  \end{center}
  \caption[bf]{Evolution of $\Lambda$ with time for run
    a1.20. Top: $N=10,20 {\rm ~and~} 50$. Bottom: $N=4 {\rm~(solid~
      line)}, 6, 8, 10, {\rm ~and~}12$ (top to bottom) for run
    a1.20. Error bars have only been included for $N=4$ for clarity.
  \label{fig:faa11a020}}
\end{figure}

In runs a1.08 and a1.21 the stochasticity of runs with different
random number seeds is easily seen. Both simulations are initially
{\em statistically} the same, but in Fig.~\ref{fig:faa11a008} we show
the states of the clusters at $\approx 1.9$ Myr.  Run a1.08 shows no
evidence of mass segregation, whilst run a1.21 shows very significant
mass segregation out to $N = 20 - 25$ (in
Fig.~\ref{fig:faa11a021.191} the 10 most massive stars are very
closely clustered in the centre, and the symbols indicating their
positions overlap somewhat).

\begin{figure}
  \begin{center}
    \setlength{\subfigcapskip}{10pt}
\subfigure[]{\label{fig:faa11a008.190}
\includegraphics[scale=0.37,angle=270]{faa11a008.dat.190.ps}}
\subfigure[]{\label{fig:faa11a021.191}
\includegraphics[scale=0.37,angle=270]{faa11a021.dat.191.ps}}
  \end{center}
  \caption[bf]{Runs a1.08 (a) and a1.21 (b): $D=1.6,Q=0.3$. The ten
    most massive stars are depicted by triangles. The most massive
    stars are not always clearly seen because of close grouping.
  \label{fig:faa11a008}}
\end{figure}

It is important to note that the plots used in Fig.~\ref{fig:DandQ} do
not show all of the mass segregation information. They only show mass
segregation for the $N$ which is plotted (in this case $N=10,20{\rm
  ~and~} 50$).  This choice is rather arbitrary and fails to provide
all of the information.  We have chosen to plot these values for
clarity, but any detailed investigation of the evolution of cool,
clumpy clusters requires an analysis of a three dimensional
dataset including time, $N$, and $\Lambda$.

In run a1.04, the stochastic and transient nature of mass segregation
can be seen. Fig.~\ref{fig:faa11a004.212} shows that at 2.1 Myr the
twelve most massive stars in the cluster are in a heavily mass
segregated state. However, Fig.~\ref{fig:faa11a004.222}, shows that
only 0.1 Myr later the amount of observed mass segregation in the
cluster has been reduced from $\Lambda \approx 21$ to $\Lambda \approx
6$ because of the disruption of the massive multiple system at the core.

\begin{figure}
  \begin{center}
    \setlength{\subfigcapskip}{10pt}
\subfigure[]{\label{fig:faa11a004.212}
\includegraphics[scale=0.37,angle=270]{faa11a004.dat.212.ps}}
\subfigure[]{\label{fig:faa11a004.222}
\includegraphics[scale=0.37,angle=270]{faa11a004.dat.222.ps}}
  \end{center}
  \caption[bf]{Run a1.04: $D=1.6,Q=0.3$. The ten most massive stars
    are depicted by triangles. (a) At 2.1 Myr the cluster shows very
    high levels of mass segregation for the twelve most massive stars
    ($\Lambda\approx 21$). The ten most massive stars are tightly
    grouped in the centre of the the cluster, and cannot be seen
    clearly. (b) 0.1 Myr later, the amount of mass segregation present
    in the cluster has been vastly reduced ($\Lambda\approx 6$). There
    are two massive star-massive star binaries in the central region,
    causing symbols to overlap.
  \label{fig:faa11a004}}
\end{figure}

As observations are a snapshot of one time in a cluster's evolution,
they only provide two dimensions of $N$ and $\Lambda$.  This means
that observations miss the time evolution of the system which, as is
clear in many plots in the supplementary material, can vary extremely
rapidly.  Hence we stress that observations only provide a snapshot of
a young cluster. {\em Young clusters can evolve very rapidly} on a
timescale of $\sim$ 1 Myr. Therefore the instantaneous state of a
cluster (especially if it is based on two dimensional positions) may
provide no information on what the cluster was like in the recent
past, or to how it might evolve in the near future \citep[see
  also][]{goodwin06,bastian08,allison09b}.

\begin{figure}
  \begin{center}
    \setlength{\subfigcapskip}{10pt}
\subfigure[]{\label{fig:faa11a002.185}
\includegraphics[scale=0.3,angle=270]{faa11a002.dat.185.ps}}
\subfigure[]{\label{fig:faa11a002.250}
\includegraphics[scale=0.3,angle=270]{faa11a002.dat.250.ps}}
  \end{center}
  \caption[bf]{Run a1.02: $D=1.6,Q=0.3$. The ten most massive stars
    are depicted by triangles. (a) The cluster has evolved to form a
    centrally concentrated distribution. In the core there is a tight
    triple system consisting of 3 of the most massive stars, which
    cannot clearly be seen. (b) 0.7 Myr after (a), the cluster has
    been destroyed by the decay of the multiple system, and most of
    the 10 most massive stars have been ejected.
  \label{fig:faa11a002}}
\end{figure}

\subsection{Post-collapse evolution}
\label{ssec:post-collapse}

The collapse of clumpy clusters may not lead only to mass segregation,
but also to other interesting phenomena; most notably the formation of
`Trapezium-like' systems, the rapid ejection of massive stars, and the
disruption of the cluster itself.

\subsubsection{Formation of `Trapezium-like' systems}
\label{sssec:trapezium}

The Trapezium in the Orion Nebula Cluster (ONC) is a multiple system
consisting of four of the most massive stars in the ONC. For the
following discussion we shall use a simple definition of a
`Trapezium-like' system as a close group of massive stars (at least 3
with $M>8\ensuremath{\textrm{ M}_{\odot}}$) which are bound.  Under this criterion, 45 of the 50
$D=1.6,Q=0.3$ simulations formed a `Trapezium-like' system. These
simulations contained no primordial binaries, but were able to migrate
the most massive stars into very close proximity to each other on very
short timescales ($\sim$ 1 Myr) through dynamics alone \citep[see
  also,][]{allison09b}. In the 50 $D=1.6,Q=0.3$ simulations, the
average shortest separation reached by the four most massive stars was
0.04~pc (about 8000~AU), which occurs within the first 2 Myr. The
shortest separation between the four most massive stars in any
simulation was 0.0025~pc (500~AU). We would expect that with different
initial conditions (i.e., initial binaries, smaller $R_0$, etc) these
multiple systems could be made even more extreme. In fact, preliminary
investigations of simulations with an initial fractal radius of 0.5~pc
(half the size used in this paper) and only single stars found a
`Trapezium-like' system with the four most massive stars in a cluster
with an average separation of only 20~AU between them.

`Trapezium-like' systems form during the dense core phase as the most
massive stars loose kinetic energy through two-body encounters with
lower-mass stars.  As they mass segregate, the typical separations
between the most massive stars decrease and they form high-order
multiple systems.  We note that the dense core that forms at the peak
of the collapse is similar to the initial conditions used by
\citet{pflamm-altenburg06} to model the formation of the Trapezium in
the ONC.  It also has the extreme density required to explain
observations of $\eta$ Cham \citep{moraux07} and the ONC
\citep{parker09}.  We will examine the formation and evolution of
`Trapezium-like' systems in more detail in a subsequent paper
(R.~J.~Allison et al., in prep.). Hydrodynamical simulations also
  show the formation of trapezium-like systems in the gas-dominated
  phase of cluster formation
  \citep[see,][]{bonnell03,klessen09}. These systems are able to form
  due to the ability of gas to dissipate kinetic energy and
  redistribute angular momentum. Therefore, if the effects of gas were
  included in these simulations we would expect the trapezium systems
  which form in these simulations to appear earlier and to be even
  more extreme.

\subsubsection{Core collapse?}

Some simulations appear to show core collapse events.  Early mass
segregation can create a core-halo structure in the cluster, with a
dense core of massive stars, surrounded by a halo of lower-mass stars.
The dense core often forms a Trapezium-like system (see above).  The
lower-mass stars are typically on radial orbits, and may enter and
extract energy from the core causing it to shrink and the higher-order
massive multiples to harden.  This also causes the halo to heat up and
the cluster to start dissolving.  At some point, the massive multiples
may decay, ejecting high-mass stars at high velocity (see below) and
blowing the cluster apart.

In run a1.02, for example, the cluster collapses and forms a dense
core. The 4 most massive stars form a Trapezium-like system which very
rapidly decays and destroys the cluster. Fig.~\ref{fig:faa11a002.185}
shows the cluster during the `core phase', the massive star multiple
system is in the centre of the cluster (but the individual stars are
too close to resolve in this image).  Fig.~\ref{fig:faa11a002.250}
shows the cluster 0.7 Myr later. Most of the massive stars have been
ejected from the central 1 pc, and the cluster has been destroyed.
Prior to dissolution, the degree of mass segregation increases as the
central multiple hardens, and at around 1.9~Myr the central multiple
finally decays, ejecting the most massive stars and creating a hard
binary. This system contains two stars of mass 45.3 and 27.8\ensuremath{\textrm{ M}_{\odot}},
which had an initial separation of 800 AU before the ejection, and a
separation of $\sim 100$ AU after. This binary increases its binding
energy by around $1\times 10^{40}$ J, which is comparable to the
entire potential energy of the cluster of $\sim -6\times 10^{39}$
J. In this simulation the formation of the binary system alone is
  able to directly disrupt the cluster. It is also possible that the
  energy input comes from gradual interactions with massive star multiples
  which slowly disrupt the cluster and form a hard massive star binary.

\begin{center}
\begin{table}
  \begin{tabular}{|c|c|c|c|c|}
\hline
        &  \multicolumn{4}{|c|}{$D$}      \\
$Q$     &  1.6    &  2.0   &  2.6  &  3.0 \\
\hline
0.3     &  32/50  &  2/10  &  0    &  0   \\
0.4     &  6/10   &  2/10  &  0    &  0   \\
0.5     &  7/10   &  0     &  0    &  0   \\
\hline

  \end{tabular}
\caption{Fraction of clusters which become globally unbound with
varying initial virial ratio, $Q$, and fractal dimension, $D$.
\label{tab:disruption}}
\end{table}
\end{center}

Table~\ref{tab:disruption} shows the number of simulations for which
the final (4 Myr) virial ratio is greater than unity (i.e., the cluster is
unbound). Energy is conserved in the simulations, but an unbound
cluster may be formed from an initially sub-virial cluster through the
redistribution of energy in the core collapse phase.

Even if the cluster manages to survive for the 4~Myr of our
simulations, shortly after this the most massive stars will become
supernovae and the loss of the most bound portions of the cluster
should destroy the cluster.  Thus clusters can be destroyed
dynamically without the need for gas expulsion
\citep{goodwin06,goodwin09}.

\subsubsection{Massive star ejections}
\label{sssec:ejection}

\begin{figure}
  \begin{center}
    \setlength{\subfigcapskip}{10pt}
    \includegraphics[scale=0.35,angle=270]{ejec_speed.ps}
  \end{center}
  \caption[bf]{Distribution of final speeds of all stars from
  the 50 $D=1.6,Q=0.3$ simulations. The black region shows stars with
  $M>10\ensuremath{\textrm{ M}_{\odot}}$, and the dashed line shows the average escape speed
  ($v_{\textrm{esc}}\approx 2.5$ km s$^{-1}$).
  \label{fig:vel}}
\end{figure}

The ejection of massive stars from clusters can occur in three ways.
Firstly, Trapezium-like systems are inherently unstable and can
decay dynamically \citep{sterzik98}.  Secondly, other massive stars
can interact with Trapezium-like systems or with massive binaries and
be ejected.  Thirdly, the hardening of Trapezium-like systems in
core collapse processes may decrease its stability and cause it
to decay faster than it might otherwise have done.

Figure~\ref{fig:vel} shows the final (at 4 Myr) velocity distribution
of the 50 $D=1.6,Q=0.3$ simulations, for comparison the typical
velocity dispersion of a cluster is $\sim 1.9$~km~s$^{-1}$, and the
typical escape velocity is $\sim 2.5$~km~s$^{-1}$. The plot shows that
it is quite possible for the massive star ejections to reach
velocities in excess of 10 km s$^{-1}$. The simulations produce stars
with masses $>30\ensuremath{\textrm{ M}_{\odot}}$ having ejection velocities $>10$ km s$^{-1}$,
and in one case a 12\ensuremath{\textrm{ M}_{\odot}} star is ejected with a velocity of
25.9\ensuremath{\textrm{ km s}^{-1}}. In all, 13 per cent of stars $>10$\ensuremath{\textrm{ M}_{\odot}}~ were ejected with
velocities $> 5$\ensuremath{\textrm{ km s}^{-1}} ($\approx 5 {\rm~pc~Myr}^{-1}$).

\section{Discussion}
\label{sec:disc}

Many young clusters are observed to be `mass segregated', that is
their most massive stars are concentrated preferentially towards their
centres.  The ONC (2-3 Myr) is well known to be mass
segregated. \citet{hillenbrand98} find, using the cumulative
distribution of different mass groups, evidence of mass segregation
for stars more massive than 5\ensuremath{\textrm{ M}_{\odot}}, and a possibility that mass
segregation is present for stars $>$1-2\ensuremath{\textrm{ M}_{\odot}}. \citet{allison09} show,
using the minimum spanning tree method, that mass segregation in the
ONC is split into three `levels'. The first contains the four most
massive stars, the second stars $>5\ensuremath{\textrm{ M}_{\odot}}$, and the third is a decrease
towards no mass segregation below $5\ensuremath{\textrm{ M}_{\odot}}$.  Using the radial
variation of the IMF, \citet{harayama08} and \citet{sharma07} show
that NGC 3603 (2.5 Myr) and NGC 1893 (4 Myr) are mass segregated, but
that there is no evidence for mass segregation for stars $<1-2\ensuremath{\textrm{ M}_{\odot}}$
in either cluster.  \citet{raboud98} show, using the cumulative
distribution method, that NGC 6231 (4 Myr) is mass segregated. This
cluster, like the ONC, has different `levels' of mass segregation. The
most massive stars ($>16\ensuremath{\textrm{ M}_{\odot}}$) are clearly more mass segregated than
stars of lower mass, and stars with masses between $2.5 \textrm{ and }
16\ensuremath{\textrm{ M}_{\odot}}$ are spatially well mixed, but more mass segregated than stars
$<2.5\ensuremath{\textrm{ M}_{\odot}}$.  Also using the cumulative distribution method
\citet{jose08} find evidence for mass segregation in Stock 8 (1-5
Myr), and show that it is only apparent for stars $>1\ensuremath{\textrm{ M}_{\odot}}$.
  Using our method, \citet{sana10} find that the cluster Trumpler 14
  ($\sim$4 Myr) also shows mass segregation. There is significant mass
  segregation for stars more massive than $\approx$10\ensuremath{\textrm{ M}_{\odot}}, but no
  evidence for stars less massive than this.

Such observations are a strong indication that these clusters have
undergone an early dense phase. The mass segregation in these clusters
follows a similar profile -- mass segregation is present for the most
massive stars, and below some particular mass ceases to be observed --
this is what we observe in our simulations.

There are two important elements that are missing from our
simulations: binaries and gas.  Binaries have been neglected as we
wish to explore the basic gravitational physics which binaries would
confuse.  In future papers, we will introduce primordial binaries into
our simulations.  Gas has been ignored, as it is computationally
extremely expensive to include and because introducing gas introduces
a whole new set of parameters (the equation of state of the gas, the
Mach number and power spectrum of the turbulence, etc.).  But clearly
gas is a vital ingredient in very young star clusters. It is what the
stars form from, and it can be a significant contributor to the
background potential.

From our simulations, it is not clear if massive stars might form
directly in massive cores \citep[e.g.,][]{krumholz07}, through
fragment-induced starvation \citep{peters10} or due to competitive
accretion \citep[e.g.,][]{smith09}.  However, hydrodynamical
simulations indicate that gravoturbulent fragmentation leads to
subclustered and mass segregated clusters
\citep{maclow04,maschberger10}. Clearly, the ability of young clusters
to dynamically mass segregate on a very short timescale means that
massive stars do not {\em have} to form (or rather, build up their
mass) in the core of a young cluster.  Massive stars can form in
subclusters or in the outskirts of clusters and within a~Myr or so be
very mass segregated. However, not only stars, but also gas, will be
involved in the collapse of the cluster to a dense phase and so cool
collapse might enhance competitive accretion.  Indeed, it is difficult
to imagine that some competitive accretion will not occur during the
channelling of stars and gas into a very dense state.  Do massive
stars form in massive cores that are then dynamically mass segregated?
Does competitive accretion dominate, especially during the dense
collapse to form the massive stars?  Do fairly massive stars form in
the outskirts of clusters which are dynamically mass segregated and
then have their masses increased by competitive accretion in a hybrid
scenario (such a process may be occurring in simulations; see
Maschberger et al. 2010)?

\section{Conclusions}
\label{sec:conc}

Observations and theory both strongly suggest that the initial
conditions of star clusters are cool and clumpy.  Therefore, we have
conducted a large number of $N$-body simulations of the early
($< 4$~Myr) evolution of clusters with virial ratios of $Q = 0.3, 0.4$
and $0.5$ (where $0.5$ is virialised), and fractal dimensions of $D =
1.6, 2.0, 2.6$ and $3.0$ (where $3.0$ is roughly a uniform density
sphere) with radii of $1$~pc and $1000$ members (ie. total masses of $\sim
500$~M$_\odot$).   In our simulations, all  members were
initially single stars selected from a Kroupa IMF, and the simulations
lasted for 4~Myr (so not requiring stellar evolution to be included).

We study the evolution of the star clusters with a particular emphasis
on the level of mass segregation.  We measure mass segregation using a
minimum spanning tree to provide a quantitative measure of mass
segregation and which is not biased by clumpy underlying mass
distributions (Allison et al. 2009a).

This study follows that of Allison et al. (2009b), in which we showed
that clusters with $Q=0.3$ and $D=1.6$ (i.e., very cool and extremely
clumpy) undergo collapse to a short-lived but extremely dense core.
This core can dynamically mass segregate the most massive stars
down to a few M$_\odot$ via two-body encounters before re-expanding.
The re-expansion is partially driven by the increase in the velocity
dispersion of the low-mass stars caused by two-body encounters.

Our main results may be summarised as follows:

$\bullet$  The depth of the collapse, and so the degree of mass
segregation depend on both the initial virial ratio, $Q$, and the
degree of substructure, $D$.  Low-$Q$ and low-$D$ clusters can
collapse to a denser state and so mass segregate more than high-$Q$,
high-$D$ clusters.

$\bullet$ Whilst there is a general trend of increasing mass
segregation with lower-$Q$ and lower-$D$ the inherently stochastic
nature of fractals means that {\em statistically} identical clusters may
undergo very different evolution.

$\bullet$  Many features are extremely short-lived, and young clusters
can change rapidly and violently.  Observations only provide a
snapshot of the evolution of a cluster and it is dangerous to draw
conclusions about the past and future state of a cluster from a single
snapshot (see also Bastian et al. 2008).

$\bullet$ Young clusters can undergo core collapse.  Early
dynamical mass segregation establishes a core of massive stars (see
also Pflamm-Altenburg \& Kroupa 2006) and a halo of lower-mass stars.
Energy loss from the core to the halo can drive the formation of
massive, hard binaries and Trapezium-like multiple systems.  The
heating of the halo and the hardening and subsequent decay of the
central multiple systems can dynamically destroy a cluster within a
few~Myr.

$\bullet$  The interactions of massive stars in the core of a young
cluster can cause the ejection of even very massive stars at
velocities in excess of $20$~km~s$^{-1}$.  This may help explain
ejections from the ONC (see also Pflamm-Altenburg \& Kroupa 2006).

$\bullet$ The early evolution of cool, clumpy clusters is rapid,
violent, and extreme.  The densities of clusters (and hence their
crossing and relaxation times) can change by orders of magnitude
during the first few~Myr of their existence.  Thus the currently
observed properties of young clusters are just a snapshot in the life
of these clusters and extreme care must be taken in inferring the past
history or future evolution of clusters from a single snapshot (see
also Goodwin \& Bastian 2006; Bastian et al. 2008; Allison et
al. 2009b).

That young clusters are mass segregated down to a few M$_\odot$, but
not below, is due to the short-lived dynamical mass segregation phase
which is able to mass segregate only the most massive stars.  That the
ONC has an unstable high-order multiple containing four of the most
massive stars can be explained by its dynamical formation during the
dense phase.  The ejection of high-mass stars from clusters can occur
during the dense phase, or afterwards from the decay of higher-order
massive multiple systems.

\section*{Acknowledgements}

RJA and RJP acknowledge financial support from STFC. SPZ is grateful
for the support of the Netherlands Advanced School in Astrophysics
(NOVA), the LKBF and the Netherlands Organisation for Scientific
Research (NWO) (via grants \#643.200.503 and \#639.073.803). RdG
acknowledges financial support from the National Science Foundation of
China under grant 11043006. We acknowledge the support and hospitality
of the International Space Science Institute in Bern, Switzerland
where part of this work was done as part of a International Team
Programme. We would also like to thank the referee, Ralf Klessen, for
his interesting and useful comments.

\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


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On Sunday 11 May, the 2008 ISAF Mid-Year Meetings, hosted by the Chinese Yachting Association, concluded in Qingdao, China.
The location enabled the delegates to have a first hand look at the Qingdao Olympic Sailing Centre which will host the 2008 Olympic Sailing Competition in less than 100 days, with a tour of the venue on Sunday morning. The visit coincided with the first race day of the IFDS Qingdao International Regatta, which is being treated as the 'unofficial' test event for the Paralympic Games.
Deliberations then returned to the 2012 Olympic Sailing Competition (click here to read the report from Saturday on the Council's decision on the Olympic events). The ISAF Regulations require Council to make a list of equipment for the 2012 Olympic Sailing Competition at this meeting. It is from this list that in November 2008 Council will select the equipment for the 2012 Games. The regulations require that the list shall include all equipment proposed through a valid submission, whether or not there is an event on the programme suitable for the equipment proposed. Having reaffirmed at Saturday's opening meeting that the multihull would not be on the programme for the 2012 Olympic Sailing Competition, Council wished to ensure this requirement to make a list was not misleading in the context of the multihull event. Therefore, whilst submissions were received proposing multihull equipment for the dinghy events and multihull equipment is included on the following list, Council added the proviso that 'the selection of equipment for dinghy events for the 2012 Olympic Sailing Competition will not be open to multihulls*'.
Council went on to approve the recommendation from the Events Committee on the voting procedure Council will use to decide the equipment in November 2008. Each event will be voted for individually, with a simple majority determining the equipment selected. If there is a tied vote, a 'run off' will be held between those two securing the highest number of votes. In the event of being unable to break a tie, the President will have the casting vote.
The ISAF Advertising Code (ISAF Regulation 20 - www.sailing.org/regulations) has been reviewed over the past year by a working party including representatives from Member National Authorities, classes, sailors and event organizers. Whilst the fundamental principles will remain, the aim of the review has been to reword the existing Code in a format that is easier to understand, ensure the appropriate balance of advertising 'space' for each party, review the default advertising for classes and improve and broaden the advertising opportunities.
To ensure extensive consultation, the proposed changes will soon be published on the ISAF website for feedback by 30 June 2008. The final proposals will be submitted to the 2008 ISAF Annual Conference, with the new Advertising Code scheduled for implementation from 1 January 2009, to coincide with the next Olympic quadrennial.
At their meeting on Monday, the Executive Committee established a Multihull Commission who will work directly with the Executive Committee. 'It is essential the multihull community is represented directly within ISAF and the Executive Committee looks forward to working together to support the future of multihull sailing at all levels,' commented the ISAF President.
In closing the 2008 ISAF Mid-Year Meeting, the ISAF expressed thanks to the Chinese Yachting Association, Qingdao Municipal Government, Sports Bureau of Qingdao and the Sailing Sub-Committee of Qingdao.
Click here to read more on the ISAF Beppe Croce Trophy, presented at a gala dinner hosted by Sanpellegrino during the Mid-Year Meetings.


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We know you have many choices when choosing a dentist in The Villages area, so we have made requesting an appointment a simple process via our website. If, for any reason you cannot keep a scheduled appointment, or will be delayed, please call us as soon as possible.
We accept most PPO insurance plans, please contact our office to verify acceptance of your plan. We will be happy to process your insurance claims for you to make your experience as hassle free as possible.
CareCredit finance plans are available to help you pay for treatments and procedures your insurance does not cover. We offer interest free financing* or low minimum monthly payment options so you can get the treatment you need, when you want it. You can even use CareCredit financing for your family and favorite pet.
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This is the new Sheffield cafe where you will soon be able to enjoy afternoon tea with your dog
Fireworks hurled at police officers and firefighters in Halloween attacks in SheffieldÂ
Firefighters and police officers had fireworks hurled at them in a series of Halloween attacks in Sheffield. Â
South Yorkshire Police said officers had fireworks, eggs and stones hurled at them while responding to incidents in Firth Park and Burngreave last night.
CRIME: Man recovering after stabbing in Sheffield city centre And firefighters called out to a house blaze in Lifford Street, Tinsley, were also pelted with fireworks and eggs.
Sheffield's District Commander, Chief Superintendent Stuart Barton
Police officer attacked at domestic incident in Sheffield
The blaze broke out after a firework was hurled through a bedroom window.
Two men in the house at the time escaped unharmed.
POLICE: Cigarette packets and cash machines fitted with tracking devices after raids at Co-op stores in South Yorkshire
Police officers and firefighters targeted by yobs in the Halloween attacks avoided injury but South Yorkshire Police Inspector Chris Lewis, whose officers were attacked, slammed the '˜stupidity' of those involved.
He said he fears it '˜will only be a matter of time before these mindless acts result in serious injury to an officer or a member of the public'.
Sheffield's District Commander, Chief Superintendent Stuart Barton, has also condemned those involved.
'Last night the vast majority of people in Sheffield enjoyed themselves trick or treating and having fun but unfortunately there was a small minority who decided to target police officers,' he said.
'It was a small group but their actions could have caused catastrophic consequences for the police officers and their families.
'This foolish few did not think about the consequences of their actions and rest assured we will do all we can to identify and deal with them.
'We want people to enjoy this time of year and not to get involved in activities which will lead them to our custody suite and could have long term repercussions.'
Area Manager Tony Carlin, of South Yorkshire Fire and Rescue, said: 'We are absolutely appalled that our firefighters appear to have been targeted in this way.
'Attacks like this place the safety of our firefighters, and the people they are trying to protect, at risk. Thankfully, this type of incident is extremely rare in South Yorkshire and it is only a tiny minority of people who would ever consider acting in such an irresponsible and dangerous way.
'However, even one attack on a firefighter is completely unacceptable '" and we will work alongside the police to fully investigate any attacks and ensure that those responsible are brought to justice.'
The new Assaults on Emergency Services Workers (Offences) Act 2018Â is now in force.
Firefighters, police officers, prison officers and NHS staff are among those covered by the new law, which introduces tougher sentences for people who attack emergency services personnel.
Anyone with information on those involved in the attacks should call South Yorkshire Police on 101.


Runs and drives 455 V8 7.5L, Automatic, Interior is very nice shape and is all original. Everything works except the AC and the horn. Rear brake lines still need to be replaced. New battery, gas tank, gas sending uni, filters and fluid, plug wires, front brake calipers and all new front brake lines. Little rust on bottom corner of doors and on rear finders.1 owner car ordered in January 1976. Car is for sale locally so this add may end at my request. If you have any questions call or text me 765-265-6193.


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Mr. Basil Jones, Jr.
April 16, 1966 — August 9, 2021
Adams announces the passing of Mr. Basil Jones, Jr., 55, who transitioned on Monday, August 9, 2021 at St. Joseph's Hospital.
Adams announces funeral services of Mr. Basil Luther Jones, Jr. which will be held 2:00 PM, Sunday, August 22, 2021 in The Adams Chapel.
Viewing will be held from 12 PM - 2 PM, Sunday, August 22, 2021 in The Adams Chapel prior to the service.
We will live-streaming this service on our Facebook page beginning at 2:00 PM, Sunday, August 22, 2021 follow the link to our Facebook page to view the live-stream: www.facebook.com/adamsfuneralservices
Basil Luther Jones Jr. was born on April 16, 1966, in Kingston, Jamaica. Basil was the first child of Karen Dinnall and Basil Jones. As a baby, he spent two years in Jamaica and then migrated to the United States. Basil grew up in Brooklyn, New York. He went to Samuel J. Tilden High School and completed secondary school with his GED.
He moved with his mother and siblings to West Palm Beach, Florida, in 1989. Later he attended Atlantic Vocational Technical school and completed the Computer Service Technician program. He lived in Florida for 26 years and moved to Port Wentworth, Georgia, in 2016. He enjoyed watching television, reading, collecting comic books, and assembling model planes. He often worked construction with his brother-in-law. He was a peaceful, gentle, loving soul. He leaves behind his mother Karen Blake, father Basil Jones Sr., sister Osalami Omisoore (Nakia Blake), brother Winston Olise Blake, brother-in-law Awokoya Oyewole, two nieces, and one nephew.
To order memorial trees or send flowers to the family in memory of Mr. Basil Jones, Jr., please visit our flower store.
12:00 - 2:00pm (Eastern time)
The Adams Chapel


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subscriber appear in your tracking as bounced.
The 288 re-tries do not count as bounces. Instead, the full count of unsuccessful retries equate to one soft bounce. If the system attempts delivery 288 times and the message bounces each time, the subscriber's status is set to Bounced. If the email is delivered during the 288 tries and the subscriber opens the email, the subscriber's status is set to Active.
After Marketing Cloud receives the third soft bounce for a subscriber, their status is set to Held.
on the subscriber's current status. If the subscriber's status was already Active, their status now changes to Bounced.
the application treats the bounce differently.
re-tried in the next email send.
This table describes the causes of a technical bounce.
or the domain or IP address is found on a blacklist utilized by the receiving domain. A subscriber who receives a block bounce is re-tried in the next email send.
This table describes the causes of a block bounce.


A tool for quoting the Sacred Scriptures in the digital era.
If anyone tried to use the service or the applications yesterday August 27 and it wasn't responding, I did infact notice that there were some server downtimes, I had to reset it more than once. I think I may have found the possible cause, and I see that the server has been back up and working without any problems for half a day now. Sorry for the inconvenience and we hope it doesn't happen again!
← First 500 successful queries!
It happened again today, but now I've done further diagnostics and I believe I have patched the problem. Still sorry for the inconvenience and let's hope that now the problem won't present itself again.


Look like a Dartford based company - use an 01322 Dartford phone number and point it to your landline.
Want a Dartford phone number pointed to a mobile phone?
Want a Dartford phone number pointed for a fax to email service?


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Stop. Watch. Listen. Transform.
by Mardi-Ellen Hill
Thu, February 19, 2015
12:00 PM – 3:00 PM EST
The General Society Library
Stop Watch Listen Transform - is a launch event introducing the community to The Universe of MEND™ (Click Here for Trailer)
Presented by the New York Association of Realtors and Managers (NYARM), at the General Society Library, this event showcases executive producer Mardi-Ellen Hill in a Composer's Now Festival featured presentation and live demonstration of the epic tale's core mechanic - a musical encode / decode technology.
The live analog performance by violinist Marissa Licata will transport the audience into the digital mainframe, blurring the lines between fiction and reality, introducing the audience to a new epic adventure - the Universe of MEND™.
Following the performance will be a discussion with a panel of experts on the topics uncovered during the presentation.
Come for lunch. Unlock a thrilling puzzle for the digital age. Panelists are Rosalind Murphy (moderator), John Kiehl, Jose Martinez, Paris Cheffer, Peter Lurie and Davie R. Iannone Jr.
The Composers Now Festival celebrates living composers, the diversity of their voices and the significance of their musical contributions to our society. Composers Now is a project partner of The Fund for the City of New York. Composers Now gratefully acknowledges the support of the ASCAP Foundation, the BMI Foundation, the Cheswatyr Foundation, the Ann and Gordon Getty Foundation and the Rockefeller Brothers Fund.
Things to do in New York, NY
New York Performances
New York Film & Media Performances
Organizer Mardi-Ellen Hill
Organizer of Stop. Watch. Listen. Transform.
Mardi-Ellen Hill is a groundbreaker in the world of business synergy and integration. She has won international acclaim in multiple fields.
In 2002, she was the recipient of an award from the American Society of Composers and Publishers (ASCAP) for her work as a pioneer in the world of music invention and application in multiple markets.
In 2000, as a professor at LIU, Ms. Hill was selected to represent the University in Washington D.C., at the definitive educational/literacy conference on "Intellectual Property and Distance Learning", sponsored by the PEW Charitable Trust. She also developed/executive produced a Leadership Symposium where she introduced Kenneth K. Fisher, Brooklyn Representative to the New York City Council, as the keynote speaker.
In 1995, Banque Nationale de Paris tapped her technical talents as business analyst by sending her to review and oversee their systems dissemination at the International Monetary Fund Conference in Washington, D.C.
During the 90's Ms. Hill received numerous other grants and awards as composer/writer, including two awards from the National Endowment for the Arts, the Annette Kade Fulbright Grant, Works in Process at the Guggenheim Series, She received several international commissions, including being the first woman commissioned by the Group Musiques de Vivantes in Lyon France, the French Consulate, the Canadian Consulate General and the Royal Bank of Canada. She has served as judge and panelist of several international competitions, and state and federal arts programs, including the Brooklyn Arts Council.
Ms. Hill has had front page stories and other articles written about her in The Brooklyn Heights Press, The Music Connoisseur, Newsday, Artspeak, and The Boston Herald, and she has been interviewed on National Television and is a WSJ Woman of Note.
A graduate of Bard College, Ms. Hill's graduate work was completed at Longy School of Music. She taught at New York University, LIU, Marymount Manhattan College, and she has lectured at Bard College, Mount Holyoke College, State University at Stoneybrook and other universities.
Currently, she is completing a book/game series as a business vehicle; and a legal thriller, "Star Child", about a child's DNA code musically encrypted in a city plan, as a new entertainment franchise model that presents an innovative platform for copyright in a wireless world.
Stop. Watch. Listen. Transform. at The General Society Library
Mardi-Ellen Hill
Fri, Apr 1 10:00 PM
BICEP LIVE
Knockdown Center, Queens
Fri, May 13 3:00 PM
Desertfest New York
Sun, Jan 23 7:45 PM
Sunday Sqool Comedy
Sour Mouse, New York
Lantern Comedy Presents: The Comedy Shop
The Comedy Shop (formerly Lantern Comedy), New York
SESH Comedy - LES BYOB Comedy Club!
Sesh Comedy, New York
Sun, Apr 17 7:00 PM
Kaiju Big Battel
The Bell House, Brooklyn
Mary Beth & Friends
Sat, Feb 5 10:00 PM
Akumandra - Brooklyn: Sainte Vie (Vortex Live A/V Show), SOEL, Mateo, Eli
Tue, Jan 25 7:30 PM
Freestyle Comedy (w/ FREE PIZZA!) - Tuesday 1/25 (Doors @ 7:00PM)
The Bowery Electric, New York
FREE Comedy Show Tix! Top Comics!
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