text:
Extinction Rebellion mob cause traffic NIGHTMARE in London
MailOnline
Earlier today the eco fanatics climbed onto a Shell oil tanker at a petrol station in Bayswater, London
Along with eco-mob Just Stop Oil, XR have brought 16 days of disruption to traffic, oil depots and commuters
Comes after activists blocked four of London's busiest bridges on Good Friday – causing traffic chaos
Several oil firms secured injunctions to stop environmental protesters from targeting fuel processing sites
By WILLIAM COLE FOR MAILONLINE
PUBLISHED: 10:51, 16 April 2022 | UPDATED: 20:17, 16 April 2022
A mob of Extinction Rebellion protesters have swamped London's Marble Arch, glueing themselves to a limousine and bringing traffic to a standstill.
The eco-fanatic rabble have once again brought chaos to the streets of the capital as they launched a series of 'disruptions' on a sixteenth days of protests alongside Just Stop Oil activists.
XR members convened in Hyde Park earlier today before one group – which included two former Olympians – climbed onto a Shell oil tanker at nearby Bayswater, leading to six arrests.
But in their 'mass action' event of the day, they targeted the landmark near Speaker's Corner, lighting flares and playing bongos in the middle of the road as infamous activist Swampy was seen climbing the 45-foot-tall monument.
The group had prepared the disruption ahead of time, getting hold of a black limousine and parking it in the road of the road for activists to lock or glue their hands to.
Holly-Anna Petersen, a Christians of Extinction Rebellion activist, revealed: 'Blocking the road at Marble Arch, by people locking onto a limo. Massive well done to all those who made this possible.
It's ridiculous that we're still having to do this. Arrests happening now. By the way – the people in the car are @XRebellionUK people too!'
It came after six people were arrested for interfering with an oil tanker outside of a petrol station a short distance down the road.
Gold medal-winning slalom canoeist Etienne Stott and sailor Laura Baldwin glued themselves to the top of the tanker at a petrol station in Bayswater, near Paddington this morning.
The eco-mob group, who have pledged to bring chaos and huge disruption to London's street, unfurled banners reading 'End fossil fuels now'.
The Met said six arrests for vehicle interference had been made. It is not known if the two Olympians were among those arrested.
Met Police officers were earlier photographed at the scene, but appeared to only be standing by to prevent a traffic build up and to guard the tanker rather than pull down the protestors.
Etienne Stott, a former British Olympian who took home gold at London 2012, was seen atop the tanker being given a hard hat as police looked to remove him and another activist.
In a tweet about the protest, XR said: 'Rebels including Olympians Etienne Stott & Laura Baldwin are occupying an oil tanker in central London. We call on the govt to end all new #FossilFuels investment NOW.'
In a statement, Met Police said: 'We attended Bayswater Road at approx. 0850 BST to deal with a number of protestors who had climbed on an oil tanker. We have made six arrests for vehicle interference. The road is now open.'
It comes after members of the eco-mob blocked four of London's busiest bridges on the first day of the Easter bank holiday.
Hundreds of Extinction Rebellion activists were on Waterloo, Blackfriars, Lambeth and Westminster bridges, calling for an end to new fossil fuel investments.
Demonstrators played bongos and waved banners reading 'end fossil fuels now' and 'love in action' in front of queues of traffic.
Some of their actions have proved questionable, after the bridge stunts affected several routes for London buses, which are either eco-friendly or emit zero exhaust emissions.
It a video clip seen on Sky News on Thursday, a interviewee claimed the group had mistakenly stopped a tanker that was carrying cooking oil, rather than fossil fuels.
Earlier, activists who have infiltrated an oil plant near Birmingham vowed 'we'll be here as long as we can' after climbing on top of the facility as part of a series of dawn protests.
Eco-zealots from Just Stop Oil have managed to climb on top of a loading bay at Kingsbury Terminal in Warwickshire after gaining access to the facility in the early hours of this morning.
Members of the group – who aim to put pressure on the Government to block new oil and gas projects in the UK – have also climbed on top of an oil tanker at Gray's Terminal in Essex and have targeted the nearby Navigator Terminal in Thurrock.
Warwickshire Police say they have already arrested 12 activists from the group, while Essex Police say they have charged 12 people following protests in Thurrock. Despite the police crackdown, today one member of the group said they and six others are still inside the Kingsbury Terminal.
In a video, posted on the Just Stop Oil Twitter account, one activist said: 'In the early hours of this morning seven of us climbed up in amongst the pipes of the loading bay, blocking the terminal.
'We intend to stay here as long as we can, or until the Government decides to stop all new oil and gas projects.'
It comes as tempers today flared between lorry drivers and activists at one protest, with one haulier seen appearing to yank an activist off a tanker.
Several oil firms have now secured civil injunctions aimed at the stopping environmental protesters from targeting their fuel processing sites.
A number of key operators including Navigator Thames, ExxonMobil and Valero gained their injunctions in the last few days, the Department for Business, Energy and Industrial Strategy (BEIS) said yesterday.
It comes as dozens of climate activists were charged after arrests were made at protests at oil depots.
The Just Stop Oil activists say they arrived in the early hours of Friday at the Kingsbury terminal near Tamworth, Staffordshire, as well as the Navigator Oil terminal in Thurrock and Grays oil terminal, both in Essex.
The recently imposed injunctions aim to prevent protest activity at oil sites across the UK.
Energy Minister Greg Hands said: 'While we value the right to peaceful protest, it is crucial that these do not cause disruption to people's everyday lives.
'That's why I'm pleased to see oil companies taking action to secure injunctions at their sites, working with local police forces to arrest those who break the law and ensure deliveries of fuel can continue as normal.'
Valero Energy had obtained a High Court injunction against a number of environmental groups and 'persons unknown' earlier this week following recent protests at the Kingsbury terminal.
It bans anyone from damaging any part of the land at each of the firm's sites, from 'affixing themselves to any other person or object' on the land or parts of access roads, and from building any structure.
Valero also owns and operates sites in Manchester, Cardiff, Plymouth and Avonmouth.
On Friday morning, pictures of climate activists, affiliated with Extinction Rebellion, showed people in orange hi-vis jackets on top of oil tankers and blockading roads, while holding signs.
Essex Police says a further 12 people aged 19 to 64 have been charged following the protests, bringing the total to 23.
They are charged with either interfering with a motor vehicle and wilful obstruction of a highway or aggravated trespass.
The force said 28 people were arrested on Friday, bringing the total number of arrests made since April 1 to 454.
Warwickshire Police said 12 arrests had been made.
Activists from Just Stop Oil and Extinction Rebellion have been blocking access to oil terminals, demanding that the Government stops new oil and gas projects.
A dozen activists are said to be at the scene in Tamworth and have locked themselves on to pipes, while roadblocks and 'tanker-surfing' has taken place at the sites in Essex.
Officers remain in Thurrock where a small number of people continue to protest.
Essex Police Assistant Chief Constable Glen Pavelin said: 'It is anticipated the road network will be busy today and in the coming days, as people travel and spend time with family and friends during the Bank Holiday weekend.
'Our dedicated officers will continue to work across the weekend to keep Essex moving, keep people safe and minimise disruption to the public.
'We also continue to work closely with our colleagues at the Crown Prosecution Service to secure charges where possible.
'As demonstrated this week, if you come to Essex and engage in disruptive and dangerous protest, we will arrest you.'
Warwickshire Police said: 'Officers remain at Kingsbury Oil Terminal today and are currently dealing with protest activity after a number of protesters arrived overnight.
'There is minimal impact to the wider community at this time.'
Dozens of climate activists have been charged after arrests were made at protests at oil depots.
The activists say they arrived in the early hours of Friday at the Kingsbury terminal near Tamworth, Staffordshire, as well as the Navigator Oil terminal in Thurrock and Grays oil terminal, both in Essex.
Pictures from Just Stop Oil, a group of climate activists affiliated with Extinction Rebellion, show people in orange hi-vis jackets on top of oil tankers and blockading roads, while holding signs.
Posted in: Alternative Energy, Alternative Fuels, Big Oil, Business Ethics, Business Principles, Climate Change, Environment, Extinction Rebellion, Fossil Fuels, Gas, Greenwash, Human Rights, Oil, Royal Dutch Shell Plc, Shell, Shell Employee Safety, Shell Energy, Shell PLC, Sin Stocks, Toxic contamination.
Tagged: Alternative Energy · Environment · Gas · Oil · Royal Dutch Shell Plc · Shell
← Shell to develop blue hydrogen plant
Strong progress towards net zero for Shell →


Excerpt from J.K. Chambers, "The Canada-U.S. border as a vanishing isogloss: the evidence of chesterfield." Journal of English Linguistics 23 (1995): 156-66.
The most comprehensive evidence of the decline [of the Canadianism chesterfield] comes from the survey called Dialect Topography of the Golden Horseshoe (Chambers 1992). This postal survey, undertaken in the winter of 1991-92, elicited linguistic responses from a large representative sample in Canada's most populous region, the so-called Golden Horseshoe around the western tip of Lake Ontario. The region takes in the conurbations of Oshawa, Scarborough, Toronto, Mississauga, Oakville, Burlington, Hamilton, St. Catharines, Welland and Niagara Falls. Over five million people, more than one-sixth of Canada's population, live in this 250km strip.
The 80 American respondents on the U.S. side of Niagara answered the question about the name they used for the long upholstered seat that holds three or four people in a straightforward way: 81.2% said couch, another 12.5% said sofa, 2.5% said davenport (two people) and coach (two others), and one said love seat. The Canadians, by contrast, provided eleven terms. Moreover, whereas none of the Americans responded with more than one term, 70 of the 935 Canadians did.
Table 1: Lexical choices of Canadian respondents by age groups, with each item shown as a percentage (with the total in parentheses). The columns are labeled with the following abbreviations: O 'couch', X 'chesterfield', S 'sofa', D 'davenport', E 'settee', L 'love seat', l 'love couch', J 'lounge', V 'divan', B "bank', and 'chair'.
Table 1 divides the Canadian respondents into age groups and lists the percentage of each group (with the raw score in parentheses) for each term. Only three of the terms,couch, chesterfield, and sofa,occur in all age groups. The other terms,davenport, settee, love seat, love couch, lounge, divan, bank and chair have very little currency.
An obvious observation about Table 1 is that the percentages decline steadily as you scan the first column, couch, from top to bottom, that is, from the youngest to the oldest, and conversely the percentages increase as you scan the second column, chesterfield, from top to bottom. Sofa, in the third column, shows a slight and inexplicable currency among the middle groups, from ages 30 to 59, suggesting that it briefly, but unsuccessfully, competed with couch when chesterfield was losing ground. Among the other terms, settee occurs widely enough to give it status as a variant in the Golden Horseshoe. The others may well be family terms (bank from an 80-year-old woman whose parents were Dutch), or nonce terms (love couch, lounge), or mistakes (chair from a 20-year-old university student from St. Catharines).
The rapid replacement of the indigenous chesterfield by the American standard term couch is graphically evident in Figure 1, which plots the use of these two terms by the age groups, from the oldest to the youngest. Fig. 1: Use of couch and chesterfield by different age groups, with the oldest on the left and the youngest on the right.
The chronology of the decline of chesterfield and the rise of couch can be inferred from the apparent-time display in Figure 1. Chesterfield remains the most frequent term for people 50 and over. In the 1930s, when the 50-59 year- olds were born, it was presumably nearly unanimous. In the 1950s, when the 30-39-year-olds were born, it was being supplanted, and in the 1970s, when the youngest group represented here was born, it was coming to be associated with the speech of older people. They consider it to be 'quaint', and it is sometimes unknown by younger people.


Well this might seem kind of stupid for a few. But I know that some users (not to mention anyone's name) hate the dub in some anime and liked it better subbed. But for some other users, they like all the anime dubbed. So I was thinking that maybe AC should have subbed and dubbed episodes, movies, ovas. It doesn't have to be for all of the animes though. Just a thought.
It is a good thought, but it wont happen any time soon... "of a few nameless reasons". It would be nice though, atleast then I would actually watch somthing on AC, rather then just moderating it.
when ive watched animes that are dubbed..
actually.. can someone tell me which epi it is after when.. inuyasha gets the.. adament birrage or something? when sesshomaru and naraku were fighting in his fathers grave.. inuyasha was there also. then inuyasha attacked naraku with the adament birrage that he got from the adamentite demon.. which epi is this?
when ive watched an anime being english dubbed..
"While Sesshomaru does battle with Naraku, Hosenki challenges Inuyasha to slay him in order for the Tetsusaiga to absorb his demonic power. However when Naraku's miasma threatens Inuyasha's friends, he abandons his fight with Hosenki to protect them."
I dont really care on whether AC will adventually have subbs or not, but what should be done is; all anime that have not yet finished releasing "Dubbed", should be added "Subbed" until the dubb is fully released.. Its pretty understandable, and reasonable, though last time we had this discussion, a few nameless people objected to it.. I've got no idea why, its pretty shameful really.
I think Curt has a point, if it's not out dubbed yet and lots of people really want it on the site then it should just be added subbed, then there's less of a wait and it's actually better.
Again, I don't really mind either subs or dubs, but it makes sense to add the subs which are in high demand if the dubs aren't out yet.
yah thats the one.. and..
so its almost the end? i look at the list right now and it says 137 out of 167..
They could do that, add subbed and dubbed, and don't they buy the DVD and on the DVD u have both subbed and dubbed, so wont be hard getting the subbed version.


The Really Old Website Resurrector: faced with defunct copies of departmental websites stored on CDs and DVDs, the University of North Carolina at Chapel Hill University Archives tested their ability to temporarily host the websites again using Archive-It and what's now called the Really Old Website Resurrector. Code for the Resurrector is up on GitHub.
You still have time to submit proposals to Web Archiving Histories and Futures, to be held November 13-15 in Wellington, New Zealand. Proposals are due February 28, and may cover: building web archives, maintaining web archive content and operations, using and researching web archives, and / or web archive histories and futures.


text:
In Sudan, senior citizens successfully stage a military coup, the prime minister is detained
inNews
NFL nice Tom Brady retires 'for good' - February 1, 2023
Ufuomaee to drop one other chart-buster, 29th e book - February 1, 2023
McDonald's Australia faces huge disadvantage - February 1, 2023
Soldiers successfully carried out an offensive against members of the country's interim government on Monday morning.
According to reports, Sudanese Prime Minister Abdalla Hamdok was apprehended by soldiers when an unknown group of soldiers invaded his home.
Abdalla Hamdok, Sudan's Prime Minister
This latest development has sparked fears of yet another military coup in a country already riven by political unrest.
Armed soldiers have detained five ministers of the Transitional Sovereignty Council, including four military officials and one civilian, according to local media sources.
This armed offensive is the latest in a series of attempts to depose Hamdok, who took power in 2019.
Citizens should come to the streets to oppose any military coup, according to the Sudanese Professionals Association.
On Monday, there were additional reports of internet failures in Khartoum's capital, which were confirmed by online infrastructure watchdog Netblocks.
"Internet disrupted in #Sudan amid claims of a military coup and the incarceration of the Prime Minister; real-time network data reveal countrywide connection at 34% of normal levels; incident ongoing," the group tweeted.
Recall that on Sunday, pro-military protestors shut off all access to the capital.
Since Omar al-ouster Bashir's in 2019, the military and civilians have shared authority, and last month's attempted coup was mostly blamed on soldiers loyal to Bashir, who has been charged with war crimes.
Tags:Sudan news

redpajama_set_name: RedPajamaCommonCrawl


text:
StreetDance 2 est un film de danse germano-britannique de Max Giwa et Dania Pasquini sorti en 2012. C'est la suite de StreetDance 3D sorti en 2010.

Synopsis
Pour battre la meilleure équipe de Break dance du monde, Ash, un « street dancer » exceptionnel, et Eddie partent à la recherche des meilleurs danseurs dans toute l'Europe. Ils découvrent des personnalités et des styles tous plus surprenants et variés les uns que les autres. À Paris, Ash rencontre la sublime danseuse de salsa, Eva. Ash va alors découvrir la puissance d'une danse en duo…

Fiche technique
 Réalisation : Max Giwa et Dania Pasquini
 Scénario : Jane English
 Musique :
 Photographie : Sam McCurdy
 Montage : Tim Murrell
 Décors : Richard Bullock
 Costumes : Andrew Cox
 Direction artistique : Alex Marden
 Production : Allan Niblo et James Richardson
Producteur délégué : Charles Salmon
Coproducteurs : Henning Ferber, Maria Grazia Vairo et Marcus Welke
 Sociétés de production : Vertigo Films, BBC Films, BFI, Square One Entertainment, Deutsche Filmförderfonds, Film1 et Eagle Pictures
 Distribution :
 : Eagle Pictures
 : Metropolitan Filmexport
 : E1 Films
 Pays d'origine : Allemagne et Royaume-Uni
 Genre : Film de danse
 Durée : 85 minutes
 Format : Couleur - 1.85:1- 3D
 Dates de sortie :
 :
 :

Distribution
Falk Hentschel (VF : Emmanuel Garijo et VQ : Guillaume Champoux) : Ash
George Sampson (VF : Alexis Tomassian et VQ  : Nicolas Bacon) : Eddie
Sofia Boutella (VF : Angèle Humeau et VQ : Annie Girard) : Eva
Tom Conti (VF : Patrick Raynal et VQ : Denis Gravereaux) : Manu
Brice Larrieu "Skorpion" (VF : Lui-même) : Skorpion
Samuel Revell (VF : Gilles Toutirais et VQ : Gabriel Lessard) : Tino
Elisabetta di Carlo (VF : Alisa Alessandro et VQ : Pascale Montreuil) : Bam-Bam
Delphine Nguyen (VF : Elle-même et VQ : Catherine Hamann) : Yoyo
Stephanie Nguyen "Lil Steph" (VF : Marie Facundo et VQ : Ariane-Li Simard-Côté) : Steph
Niek Traa (VF : Donald Reignoux) : Legend
Terabyte Kaito : Masai
Akai Osei-Mansfield (VQ : Nicolas DePasillé-Scott) : Junior
Lilou (VF : Christophe Peyroux et VQ : Kevin Houle) : Ali
Ndedi Ma-Sellu (VF : Lui-même) : Killa
Maykel Fonts (VF : Gunther Germain) : Lucien
Anwar Burton (VF : Namakan Koné) : Vince
Source et Légende doublage : VF = Version Française

Bande originale
 Go In Go Hard Ft Wretch 32 - Angel
 Domino - Jessie J
 High & Low - Sunday Girl
 Rockstar - Dappy
 Who Says You Can't Have It All - Dionne Bromfield
 Invincible - Anwar 'Fliistylz' Burton
 Rack City - Tyga
 Bow Wow Wow Ft Chipmunk - Bodyrox
 Superbass - Nicki Minaj
 Mama Do The Hump - Rizzle Kicks
 The Motto Ft Lil Wayne - Drake
 Troublemaker - Taio Cruz
 Bright Lights Ft Pixie Lott - Tinchy Stryder
 Burning Benches - Morning Runner
 Unorthodox Ft Example - Wretch 32
 Apache - Incredible Bongo Band
 Midnight Caller - Chase & Status
 Bass Down Low Static Avenger Remix - Dev
 Together - Herve
 Hold On - Skepta
 Baudelaires Tango - Lloyd Perrin & Jordan Crisp
 Catacombs Remix - Lloyd Perrin & Jordan Crisp
 Cuba 2012 Dj Rebel Streetdance 2 Remix - Latin Formation
 Agua Remix - Los Van Van
 Ride My Beat - Polluted Mindz

Notes et références

Liens externes

Film britannique sorti en 2012
Film allemand sorti en 2012
Film musical dramatique britannique
Film dramatique allemand
Film musical allemand
Film de danse
Film en relief
Film IMAX
Suite de film britannique
Suite de film allemand
Film de la BBC

redpajama_set_name: RedPajamaWikipedia


text:
\section{Introduction}

The existence of close-in giant planets whose orbits lie in close
proximity to their host stars is now well established
\citep[e.g.,][]{Cumming-2011}. Although these objects constitute the
best observationally characterised sample of exoplanets, their origins
remain puzzling from a theoretical point of view. As in-situ formation
of hot Jupiters is problematic \citep{Chiang-Laughlin-2013}, it is
likely that these objects have formed beyond the ice-line in the
proto-planetary disk (i.e, at an orbital separation of a few AU) and
have since been transported inwards
\citep{Lin-etal-1996}. Traditionally, smooth migration forced by
interaction with the proto-planetary disc in which planets form, has
been invoked to facilitate transport
\citep{LinPapaloizou1986b,Lin-etal-1996,Wu-Murray-2003,Crida-Morby-2007,Papaloizou-etal-2007}. Recently,
substantially more violent processes have been proposed to account for
the generation of hot Jupiters
\citep{Fabrycky-Tremaine-2007,Nagasawa-etal-2008,Beauge-Nesvorny-2012}.
However, the dominance of the roles played by each mechanism remains
controversial \citep{Dawson-etal-2012arXiv}. Accordingly, observations
of the stellar spin-planetary orbit misalignment has been invoked as a
means of differentiating among the proposed models.

Among the $\sim 1000$ exoplanets detected to date, $\sim 60$ have an
observed measure of the angle between their orbital plane and the
equatorial plane of their host star
\citep[e.g.,][]{Winn-etal-2007,Triaud-etal-2010}. Traditionally, this
has been achieved through the Rossiter-McLaughlin effect
\citep{McLaughlin-1924}\,; however, recently novel techniques involving
asteroseismology \citep{Huber-etal-2013} and star-spot measurements
\citep{Hirano-etal-2012} have also been utilised to this end. A wide
variety of measured angles have been reported to date, and many
exo-planets are apparently characterised by \emph{spin-orbit
  misalignment}\,: the orbital obliquity differs significantly from
$0$. Instinctively, this is surprising as planets are supposed to form
within a proto-planetary disk whose angular momentum direction is the
same as that of the star. Therefore, the origin of the spin-orbit
misalignment has received considerable attention over the past few
years.

A promising way to disentangle the roles of the various transport
mechanisms, is to analyse the observed distribution of the spin-orbit
angles, and to compare it to the expected distribution from a given
model. However, observations only provide the \emph{projected}
spin-orbit angle, not the real one. Accordingly, in
section~\ref{sec:proj}, we describe the 3D geometry of the problem,
and we infer the distribution of the projected spin-orbit angles from the
real ones (and vice-versa).

In section~\ref{sec:PDFs}, we compute the distributions of the
projected spin-orbit angles expected from various mechanisms, devoting
special attention to the disk-torquing model
\citep{Batygin-2012}. Within the framework of the disk-torquing
mechanism, a (possibly transient) companion to a young star makes the
proto-planetary disk precess around the binary's axis, so that the
plane in which planets eventually form and the equatorial plane of the
central star can differ. Contrary to the violent category of migration
mechanisms --\,e.g., planet-planet scattering
\citep{Rasio-Ford-1996,Ford-Rasio-2008} and Kozai resonance
\citep{Wu-Murray-2003,Fabrycky-Tremaine-2007,Naoz-etal-2011}\,-- this
process predicts that all the planets of the system can share the same
misalignment. The recent discovery of significant misalignment among a
multi-transiting system \citep{Huber-etal-2013} therefore puts
emphasis on this model.

Using analytical arguments and Monte-Carlo simulations, we find that
the current observational aggregate can be well explained by the
disk-torquing effect, implying that disk-driven planet migration in
(torqued) disks could be the dominant source of (mis)aligned hot
Jupiters.

\section{The 3D geometry of the spin-orbit angle}
\label{sec:proj}

There is considerable confusion in the literature about the spin-orbit
angle. Let us define precisely what we are interested in here. The
true misalignment angle is actually the angle between two vectors in
3D space\,: $\vec{L}_p$, the orbital angular momentum of the planet,
and $\vec{L}_s$, the angular momentum of the spin of the star. As
such, it can only lie between $0$ and $180$ degrees (there are no
negative angles in 3D). This real, 3D angle is denoted below as
$\Psi$.

The projections of these two vectors onto the plane of the sky (noted
$\vec{L}_p'$ and $\vec{L}_s'$) form an oriented angle, which in
principle could range between $-180^\circ$ and $+180^\circ$. However,
whether the angle ($\vec{L}_p',\vec{L}_s'$) is positive or negative
when measured clockwise, corresponds to the same 3D configuration,
observed from either side of the star, from the ascending or
descending node. In any case, the two cases are indistinguishable
observationally (Triaud, personal communication). Thus, it does not
make sense to report negative angles. The projected spin-orbit angle
should also be expressed as between $0^\circ$ and $180^\circ$. Still,
on \texttt{exoplanets.org}, one finds many negative projected
spin-orbit angles, taken from published articles. This angle is
sometimes noted $\lambda$
\citep[e.g.,][\texttt{exoplanets.org}]{Fabrycky-Winn-2009}, and
sometimes it is noted as $\beta$ \citep[e.g.,][]{Triaud-etal-2010}. The
projected angle is denoted below as $\beta$, and will be taken as the
absolute value of the misalignment angle $\beta$ or $\lambda$ reported
in the literature.

\subsection{Relation between the real and projected spin-orbit angle}

Assume that $\Psi$ is fixed. Which $\beta$ will be observed~? What is
the probability density function (PDF) of $\beta$~?

This question has already been addressed in general by
\citet{Fabrycky-Winn-2009}. They provide $\beta$ (that they note
$\lambda$) as a function of $\Psi$ and $i_o$, the inclination of the
orbital angular momentum with respect to the line of sight. Here, we
propose a simpler, one column derivation, making the assumption that
the observer is exactly in the orbital plane ($i_o=\pi/2$)\,; this is
appropriate because all the planets with known spin-orbit angle
transit their host star, so $|\pi/2-i_o|$ is very small. In this case,
$\vec{L}_p=\vec{L}_p'$ is perpendicular to the line of sight, and is
in the plane of the sky. Let us consider spherical coordinates
($r,\phi,\theta$) centred on the star, such that colatitude $\theta=
0$ corresponds to the north pole of the orbit, the direction of
$\vec{L}_p$\,; the origin of the longitude ($\theta=90^\circ$,
$\phi=0$) corresponds to the direction of the observer. In these
coordinates, $\vec{L}_s$ has a colatitude $\theta_s=\Psi$. Its azimuth
$\phi_s$ \footnote{This angle $\phi_s$ was noted $\Omega$ by
  \citet{Fabrycky-Winn-2009}} can be anything between $0$ and $2\pi$,
with a uniform distribution. Clearly, if $\phi_s\equiv 0 [\pi]$, the
observer sees $\beta=0$ if $\Psi<\pi/2$, and $\beta=\pi$ if
$\Psi>\pi/2$\,; conversely, if and only if $\phi_s=\pm\pi/2$ the
observer sees $\beta=\Psi$ exactly.

This configuration is shown in the right panel of
Figure~\ref{fig:proj}. The point $O$ is the centre of the unit sphere, and $P$ and $S$
are the intersection of the sphere with the vectors $\vec{L}_p$ and
$\vec{L}_s$ respectively. The point $A$ has colatitude $\theta=\Psi$
and azimuth $\phi=0$, facing the observer, while $R$ has colatitude
$\theta=\Psi$ and azimuth $\phi=\pi/2$, appearing on the limb of the
star for the observer. Accordingly, $OA=OS=OP=OR=1$\,.

The plane $(OPR)$ is the plane perpendicular to the line of sight
passing through $O$\,: it is the plane of the sky as seen by the
observer, onto which everything is orthogonally projected, along the
direction of the line of sight.

The circle gathering all the points with colatitude $\Psi$ is the
dashed circle passing through $A$, $S$, and $R$. This circle is represented
in the top left of Figure~\ref{fig:proj}. The orthogonal projections
of $A$ and $S$ onto the plane $(OPR)$, are $A'$ and $S'$ respectively. The
centre of this dashed circle is $A'$, and its radius is obviously
$A'A=A'S=A'R=\sin\Psi$. Thus, $A'S'=\sin\Psi\,|\sin\phi_s|$.

In the projected plane (shown in bottom left of Fig.~\ref{fig:proj}),
the angle between the north pole of the orbit and the spin of the star
appears to be $\beta=\widehat{POS'}$. As $A'$ is the orthogonal
projection of $S'$ on the $(OP)$ line, we have $\tan\beta=A'S'/OA'$, where
$OA'=\cos\Psi$ is negative when $\Psi>\pi/2$. Finally,
\begin{eqnarray}
\label{eq:beta1}
\beta & = & \arctan\left(|\sin\phi_s|\,\tan\Psi\right) \equiv G(\phi_s)\\
|\phi_s| & = & \arcsin\left(\frac{\tan\beta}{\tan\Psi}\right)\ .
\end{eqnarray}
This is equivalent to Eq.~(11) of \citet{Fabrycky-Winn-2009}, with $i_o=\pi/2$, $\Omega=\phi_s$ and $\lambda=\beta$.

\begin{figure}
\includegraphics[width=\linewidth]{./Projection_all.eps}
\caption{\textbf{Right\,:} 3D representation of the problem. The yellow sphere is the unit sphere centred on the star. P marks the direction of the orbital angular momentum vector $\vec{L}_p$ and S that of the stellar spin $\vec{L}_s$. The dashed circle passing through points A and S gathers all the points making an angle $\Psi$ with P. It is represented in the top left.\newline
\textbf{Top left\,:} The circle of the unit sphere gathering all the points at colatitude $\Psi$ with respect to the orbital angular momentum vector of the planet. A is the point facing the observer\,; S is the point corresponding to the direction of the stellar spin. A and S are projected on the diameter of this circle perpendicular to the line of sight onto A' and S'\,; $\phi_s$ is then $\widehat{AA'S}$.\newline
\textbf{Bottom left\,:} The projected plane, as seen by the observer. The previous dashed circle is now a dashed horizontal line, on which A' and S' are the projections of A and S along the direction of the line of sight. The arc PR defines an angle $\Psi$, while the projected spin orbit angle $\beta$ is $\widehat{A'OS'}$, marked in red.
}
\label{fig:proj}
\end{figure}

\subsection{Probability density function of $\beta$, for fixed $\Psi$}

Now, as the distribution of $\phi_s$ is uniform in the interval $[0;2\pi[$,
and $|\sin(x)|=|\sin(\pi-x)|=|\sin(\pi+x)|=|\sin(2\pi-x)|$, it is
sufficient to consider a uniform distribution for $0\leqslant\phi_s<\pi/2$, with
probability density $2/\pi$. In this case, $\beta$ is a monotonic
function of $\phi_s$. It is well known that if $X$ is a random variable
of probability density function $f_X$, and $Y=G(X)$ with G a monotonic
function, then the PDF of $Y$ is
\begin{equation}
f_Y(y) = f_X\left(G^{-1}(y)\right)\times \left|\left(G^{-1}\right)'(y)\right|\ .
\label{eq:compoVA}
\end{equation}

Thus, using Eq.~(\ref{eq:beta1}) for fixed $\Psi$, the PDF of $\beta$ is\,:
\begin{equation}
f(\beta|\Psi)=\left\{\begin{array}{ll}
\displaystyle\frac{2}{\pi}\frac{1+\tan^2\beta}{(\tan^2\Psi-\tan^2\beta)^{1/2}}& {\rm if\ }\beta\in\mathcal{T}\ ,\vspace{3pt}\\
0 & {\rm otherwise}
\end{array}\right.
\label{eq:project1}
\end{equation}
where $\mathcal{T}=\{ 0\leqslant\beta<\Psi<\frac{\pi}{2}\}
\cup \{\frac{\pi}{2}<\Psi<\beta\leqslant\pi\}$.

This equation is identical to Eq.~(19) of \citet{Fabrycky-Winn-2009}\footnote{Using $1+\tan^2(u)=1/\cos^2(u)$ leads to their expression easily.}.

Figure~\ref{fig:f_Psi_beta} shows the decimal logarithm of
$f(\beta|\Psi)$ in the $\beta-\Psi$ plane. For a given real spin-orbit
angle $\Psi_0$, the PDF of the observed projected angle $\beta$ can be
found by going along a $\Psi=\Psi_0$ line in the figure. One can check
analytically that for all $\Psi$,
$\displaystyle\int_{\beta=0}^{\beta=\pi}f(\beta|\Psi)\,{\rm
  d}\beta=1$~, as it should.

\begin{figure}
\includegraphics[width=\linewidth]{./f_Psi_beta_contourf_leg.eps}
\caption{Contour map of $f(\beta|\Psi)$ as defined by
  Eq.~(\ref{eq:project1}). The contours correspond to values $10^k$,
  with $k=-1.5,\,-1\ldots 1,\,1.5$\,; the curves corresponding to
  $f=1$ and $f=0.1$ are marked. Note that $f$ actually diverges
  towards $+\infty$ approaching the $\Psi=\beta$ line.  }
\label{fig:f_Psi_beta}
\end{figure}

\subsection{Conversion of the PDF of $\Psi$ into the PDF of $\beta$}

If now $\Psi$ has its own PDF $w(\Psi)$, the corresponding PDF of
$\beta$ will be\,:
\begin{equation}
f(\beta)=\int_{\Psi=0}^{\Psi=\pi}f(\beta|\Psi)w(\Psi)\ {\rm d}\Psi\ .
\label{eq:f_b}
\end{equation}
Computing this integration corresponds to summing vertically in
Figure~\ref{fig:f_Psi_beta}, after having given to every horizontal
line a weight $w(\Psi)$.

For example, assuming a uniform $w(\Psi)=1/\pi$, one gets the
double-peaked distribution shown in Fig.~\ref{fig:horny}. On the other
hand, assuming that $\Psi$ is isotropically distributed,
$w(\Psi)=(\sin{\Psi})/2$, one can solve Eq.~(\ref{eq:f_b}) and find
$f(\beta)=1/\pi$, uniform, as expected. The observed distribution of
$\beta$ (see histogram in Fig.~\ref{fig:Bat-anal}) is neither flat nor
reminiscent of the distribution shown in Fig.~\ref{fig:horny},
implying that the real distribution of $\Psi$ is neither uniform, nor
isotropic.

\begin{figure}
\includegraphics[width=\linewidth]{./horny.eps}
\caption{Representation $f(\beta)$ when $w(\Psi)=1/\pi$ (uniform
  distribution of $\Psi$).}
\label{fig:horny}
\end{figure}

\subsection{Deprojection}

Let $i_s$ be the angle between the stellar angular momentum $\vec{L_s}$
and the line of sight\,; an isotropic distribution of $\vec{L_s}$ on
the unit sphere gives to $i_s$ a PDF $f(i_s)=\frac12\sin(i_s)$ between
$0$ and $\pi$. On the projected plane (bottom left of figure~1), we
now have $OS'=\sin i_s$, and
$OA'=OS'\times\cos\beta=OR\times\cos\Psi=\cos\Psi$. Thus,
\begin{equation}
\Psi=\arccos(\cos\beta\times\sin i_s) = G_2(i_s)\ .
\label{eq:Psi}
\end{equation}
Note that $i_s$ or $\pi-i_s$ give exactly the same projection. One can
therefore assume that $i_s$ is distributed between $0$ and $\pi/2$
with PDF $f(i_s)=\sin(i_s)$. Then, using Eqs.~(3) and
(\ref{eq:Psi}), one gets\,:
\begin{equation}
f(\Psi|\beta) = \left\{\begin{array}{ll}
\vspace{6pt}\frac{\cos\Psi}{\cos\beta}\frac{\sin\Psi}{\sqrt{\cos^2\beta-\cos^2\Psi}}
& \begin{array}{l}{\rm if\ }\ 0<\beta<\Psi<\pi/2\\{\rm or\ }\pi/2<\Psi<\beta<\pi\ ,\end{array}\\
0 & \begin{array}{l}{\rm otherwise\ ,}\end{array}
\end{array}\right.
\label{eq:DPF_Psi}
\end{equation}
in agreement with Eq.~(21) of \citet{Fabrycky-Winn-2009}.

Then, the PDF of $\Psi$ can be deduced from the observations of $\beta$\,:
\begin{equation}
f(\Psi)=\sum_{i} f(\Psi|\beta_i)
\label{eq:deproj}
\end{equation}
where the index $i$ spans the whole sample.

Applying this to the data found on \texttt{exoplanets.org} at the end of 2013,
we get an irregular curve peaked at each of the $\beta_i$, as $f(\Psi|\beta_i)$ diverges towards $+\infty$ as $\Psi\to\beta_i$. This curve is displayed as a thin blue line in Figure~\ref{fig:deproj}. To avoid this, one could smooth the data using the error-bars $\sigma_i$ and compute\,:
$$f(\Psi)=\sum_{i} \int \frac{1}{\sqrt{2\pi}\sigma_i}\exp\left(-\frac{(\beta-\beta_i)^2}{2\,{\sigma_i}^2}\right)\ f(\Psi|\beta)\ {\rm d}\beta\ .$$
However, the $\sigma_i$ are so diverse (from $0.3$ to $60^\circ$) that this operation would only degrade the information, without completely smoothing the curve. Therefore, we prefer to operate similar to the observations of $\beta$ and build a histogram\,: we average $f(\Psi)$ on successive intervals of $20^\circ$ width. This is represented in Figure~\ref{fig:deproj} as the red stairs, while the histogram of the observations of $\beta$ is shaded grey.
It seems here that aligned hot Jupiters are a minority. However, one should realize that if all hot Jupiters were actually aligned, $\Psi=\beta=0$, but Eq~(\ref{eq:DPF_Psi}) gives $f(\Psi|\beta=0)=\textrm{max}\{\cos\Psi\,,\,0\}$\,; it is therefore almost impossible that the first step of the red stairs is the highest step, even if there is a large majority of aligned hot Jupiters.

In any case, with only $18$ cases with $\beta>40^\circ$ in the data, and
large error bars, the statistics is rather poor to infer the PDF of
$\Psi$ accurately. Therefore, in what follows, we prefer to infer the
PDF of $\beta$ from various mechanisms, and compare it directly with
the observed distribution of $\beta$.

\begin{figure}
\includegraphics[width=\linewidth]{./Deproj_v2.eps}
\caption{Grey shaded histogram\,: distribution of the observed projected spin-orbit angle $\beta$ (taken as $|\beta|$ or $|\lambda|$ in the data from \texttt{exoplanets.org}). Blue thin curve\,: $f(\Psi)$, as given by Eq.~(\ref{eq:deproj}). Red stairs\,: Histogram of the PDF of $\Psi$ with bins of $20^\circ$.}
\label{fig:deproj}
\end{figure}

\section{Application to proposed mechanisms}
\label{sec:PDFs}

In this section, we compute/take the PDF of $\Psi$ that is expected
from several mechanisms of formation of hot Jupiters. Then, we compute
the corresponding PDF of $\beta$ using Eq.~(\ref{eq:f_b}), and
compare it with the distribution of the observations.
The distribution of the observations is shown as a grey shaded histogram in Figures~\ref{fig:Bat-anal}, \ref{fig:Bat-MCall}, and \ref{fig:All}. The bins have a width of $20^\circ$, and many of them contain only two cases. This small number statistics is prone to significant variations with new observations, or change of the bins\,: one object more or less in a bin represents a $50\%$ variation. Nonetheless, it appears robust that the distribution of the projected spin-orbit angle beyond $60^\circ$ is almost uniform. Models should account for this.

To be more precise, assuming the small number of planets in our bins follows a Poisson process of parameter $\lambda$, when $N$ are found in a bin, the likelihood of $\lambda$ is given by $\lambda^N\exp(-\lambda)/N!$~. Thus, in the bins where two are found, one can say with $50\%$ confidence that $1.17<\lambda<3.16$ and with $95\%$ confidence that $0.31<\lambda<6.34$.

\subsection{Disk torquing}

Contemporary observational surveys suggest that a considerable
fraction of solar-type stars are born as binary or multiple systems
\citep{Ghez-etal-1993,Kraus-etal-2011}. Moreover, most stars form in
embedded cluster environments \citep{Lada-Lada-2003} where dynamical
evolution can lead to the acquisition of transient companions
\citep{Malmberg-etal-2007}. Recently, \citet{Batygin-2012} showed that
the presence of a companion to a young star can force the
proto-planetary disk to precess around the binary's axis, so that the
plane in which planets eventually form and the equatorial plane of the
central star can differ.

\subsubsection{Analytic simple model}

Denoting the angle between the orbital plane of the companion and
the stellar equator as $i\,'$ (therefore, $0\leqslant i\,' \leqslant \pi/2$),
$\Psi$ evolves between $0$ and $2i\,'$ in this mechanism. At first sight
of Fig.~2 of \citet{Batygin-2012}, it seems reasonable to consider
this evolution as linear with time, back and forth. In the end, the
PDF of $\Psi$ is a uniform distribution between $0$ and $2i\,'$\,:
\begin{equation}
f(\Psi\,|\,i\,')=\frac{1}{2i\,'}\ \textrm{\ if\ }0\leqslant\Psi\leqslant2i\,'\ ;\ \ 0 \textrm{\ otherwise.}
\label{eq:fPi'}
\end{equation}
The PDF of $i\,'$ should correspond to an isotropic distribution of the
orbital angular momentum vector of the companion with respect to the
stellar spin, thus it reads\,:
\begin{equation}
g(i\,') =  \sin(i\,')\ .
\label{eq:g}
\end{equation}

Now, the PDF of $\Psi$ is given by\,:
\begin{eqnarray}
f_{B12}(\Psi) & = & \int_0^{\pi/2}f(\Psi\,|\,i\,')g(i\,')\ {\rm d}i\,'\nonumber\\
 & = & \int_{\Psi/2}^{\pi/2} \frac{\sin(i\,')}{2i\,'}\,{\rm d}i\,'\nonumber\\
f_{B12}(\Psi)  & = & \frac{1}{2}\left[\textrm{Si}(\pi/2)-\textrm{Si}(\Psi/2)\right]
\label{eq:f-de-Psi}
\end{eqnarray}
where $\mathrm{Si}(x)=\int_0^x\frac{\sin(t)}{t}\,{\rm d}t$, which has
unfortunately no easy analytical expression. Nonetheless, this
expression can be computed numerically. On Figure~\ref{fig:Bat-anal},
$f_{B12}$ is displayed as the red thin curve\,; it looks linear, but
it's actually not a straight line. The corresponding PDF of $\beta$
(using Eq.~(\ref{eq:f_b})\,) is shown as the blue thick curve. The
major difference between the two curves enlights the necessity of
taking the projection into account. In the background, the histogram
of the observations shows a good agreement with the predicted
distribution of the projected angles. The PDF of $\beta$ is normalised
to have $18$ planets with $\beta>40^\circ$, like the data.

\begin{figure}
\includegraphics[width=\linewidth]{./Bat-vs-Obs_anal.eps}
\caption{Distribution of the spin - orbit angle expected in the
  disk-torquing mechanism. Red thin line\,: distribution of $\Psi$,
  given by Eq.~(\ref{eq:f-de-Psi}). Blue thick line\,: corresponding
  PDF of $\beta$. Background histogram\,: observations.}
\label{fig:Bat-anal}
\end{figure}

With this normalisation, the number of planets with $\beta<20^\circ$
(resp. $20^\circ<\beta<40^\circ$) is only $14.2$ (resp. $6.8$), while
$34$ (resp. $9$) are observed. This excess of aligned planets in the
observations should not bother us. Indeed, hot Jupiters form in the
proto-planetary disk, and migrate inwards irrespective of the
multiplicity of the stellar system. Thus, if the proto-planetary disk
is not torqued (e.g., the star is always single), the hot Jupiters are
expected to be aligned. If the proto-planetary disk is torqued by a
companion, then the planets will be misaligned, with the distribution
given above. The apparent excess of aligned hot Jupiter can therefore
be interpreted as the fraction of disks that were never significantly
torqued. We come back on this issue in the next sub-section.

\subsubsection{Monte Carlo simulations}

Within the framework of the model proposed by \citet{Batygin-2012}, the stellar spin axis is taken to remain in the primordial plane of the disk for all time. Physically, this simplifying assumption corresponds to a non-accreting, unmagnetised young stellar object that rotates at a negligibly slow rate. This picture is somewhat contrary to real pre-main-sequence stars, which typically accrete $\sim 10^{-8} M_{\odot}$/year from the disk \citep{Hartmann-2008,Hillenbrand-2008}, have $\sim 1$ kGauss magnetic fields at the stellar surface \citep{Shu-etal-1994a,Gregory-2010}, and rotate with characteristic periods in the range $P_{\rm{rot}}\simeq 1-10$~days \citep{Herbst-etal-2007}. Accordingly, \citet{Batygin-Adams-2013arXiv} examined magnetically and gravitationally facilitated disk-star angular momentum transfer with an eye towards constraining the conditions needed for the acquisition of spin-orbit misalignment. They showed that the excitation of spin-orbit misalignment is only quenched when the host star continuously spins up because of gravitational contraction \citep[i.e., the stellar field is too weak for magnetic breaking to occur\,; see][]{Shu-etal-1994a,Matt-Pudritz-2005ApJ,Matt-Pudritz-2005MNRAS}. However, they also found that the process by which spin-orbit misalignment is attained is somewhat more complicated than that described in \citet{Batygin-2012}. Specifically, as the disk mass decreases throughout its lifetime, the gravitational coupling between the star's quadrupole moment (that arises from rotational deformation) and the torqued disk gives rise to orbital obliquity via a secular resonance encounter between the stellar spin-axis precession frequency and the disk-torquing frequency \citep[see][for details]{Batygin-Adams-2013arXiv}.

Cumulatively, the more complete model of \citet{Batygin-Adams-2013arXiv} does not easily lend itself to analytic manipulation. As a result, to derive the associated distribution of projected misalignment angles, we perform a Monte Carlo simulation, utilising their perturbative model (for brevity, we shall not rehash their formalism here, but instead refer the reader to their description). As above, the inclinations of the binary companion stars are taken to be isotropic, the binary semi-major axis is drawn from a log-flat distribution spanning $10^{2.5}-a_{\rm max}$~AU \citep[where $a_{\rm max}$ can vary, see caption of Figure~\ref{fig:Bat-MC}\,;][]{Kraus-etal-2011}, while the eccentricity and the primary-to-perturber mass ratio are taken to be uniform in the intervals [0,1] and [0.1,10], respectively \citep[see][]{Kraus-etal-2008}. The primary star's mass and the disk's  initial mass are also drawn from uniform distribution spanning [0.5,1.5] $M_{\odot}$ and [0.01,0.05] $M_{\odot}$, respectively \citep{Herczeg-Hillenbrand-2008}. For all simulations, a surface density profile of the form $\Sigma \propto r^{-1}$ is assumed. The disk's outer edge is taken to lie between $10^{1.5}$ and $10^{2}$ AU \citep{Levison-etal-2008,Anderson-etal-2013}, while the inner edge corresponds to the stellar corotation radius \citep{Koenigl-1991,Shu-etal-1994a}. In turn, the stellar rotation periods are randomly chosen to lie between 1 and 10 days in rough agreement with the observational samples of \citet{Littlefair-etal-2010,Affer-etal-2013}. Following \citet{Gallet-Bouvier-2013}, pre-main sequence rotational evolution is ignored because of the inherent complexities. Finally, the disk mass loss, stellar structure, and stellar gravitational contraction are modelled as described in \citet{Batygin-Adams-2013arXiv}.

With the aforementioned ingredients in place, we compute the
disk-torquing frequency as described in \citet[][see equations 6 \& 7
  in the SI]{Batygin-2012}, while the rest of the calculation follows
directly from section 4 of \citet{Batygin-Adams-2013arXiv}. The
results are shown in Figure~\ref{fig:Bat-MC}. One thousand random sets
of parameters have been chosen with the distributions described above,
and the resulting $1000$ final spin - orbit angles have been binned in
bins of $20^\circ$ width to produce a histogram, to be compared to the
observations (Figure~\ref{fig:Bat-anal}). Three cases are presented,
where the only difference is the assumed value of $a_{\rm max}$, the
maximum possible value of the semi-major axis of the binary\,; from
left to right, $a_{\rm max}=10^3$, $10^{3.75}$, and $10^{4.5}$~AU. The
fraction of disks that will experience a negligible torquing appears
to be very sensitive to $a_{\rm max}$. However, the distribution of
the angles in the torqued cases remains unchanged, and close to the
observations, as can be seen in Figure~\ref{fig:Bat-MCall}. In this
figure, the three distributions obtained by the three sets of Monte Carlo
simulations have been normalised to have $18$ planets with
$\beta>40^\circ$, like in the data. They are represented in blue,
green, and red stairs, and are very similar beyond $40^\circ$. In the
background, the histogram of the data is shown in grey bars. All the
three stairs are within 1 count of the histogram, signaling excellent
agreement.

\begin{figure}
\begin{center}
\includegraphics[width=\linewidth]{./Bat-vs-Obs_MC_hists.eps}
\end{center}
\caption{Distributions of the projected spin - orbit angle found in Monte Carlo simulations as described in the text, for three values of the maximum of the log-flat distribution of the semi-major axis of the binary. Top right\,: $a_{\rm max}=10^3$~AU. Middle\,: $a_{\rm max}=10^{3.75}$~AU. Bottom left\,: $a_{\rm max}=10^{4.5}$~AU.}
\label{fig:Bat-MC}
\end{figure}

\begin{figure}
\includegraphics[width=\linewidth]{./Bat-vs-Obs_MCalld.eps}
\caption{Distributions produced by the Monte Carlo simulations, normalised to $18$ cases with $\beta>40^\circ$. Thin blue\,: $a_{\rm max}=10^3$~AU. Thick green\,: $a_{\rm max}=10^{3.75}$~AU. Red\,: $a_{\rm max}=10^{4.5}$~AU. Background histogram\,: observations.}
\label{fig:Bat-MCall}
\end{figure}

The choices of input parameters employed in the simulations are essentially naive estimates, predominantly guided by observational surveys. The observed agreement between the data and the model is thus compelling. However, with a considerable number of marginally constrained (and in some cases poorly understood) values at hand, it would not come as a surprise if the utilised model admitted significant variability in the distributions it could produce. Although a complete search of the parameter space is well beyond the scope of this study, it is noteworthy (as already alluded to above) that the model appears to be most sensitive to the orbital distribution of binary companions. While the median widest allowed binary orbit ($10^{3.75} \simeq 5\,600$~AU) in the simulation was motivated by the observational study of \citet{Kraus-etal-2011}, if we reduce this range to $10^{3\,}$AU, the enhancement near $\beta = 0$ in Figure~\ref{fig:Bat-MC} disappears entirely. On the contrary, if the range is extended to $10^{4.5\,}$AU, the enhancement near aligned orbits grows by almost a factor of $\sim 2$, although in both cases the shape of the PDF in the significantly misaligned region remains unchanged. The physical reason behind this is not exceedingly difficult to understand. As binary orbits get wider, the free precession (i.e., torquing) frequency of the disk decreases. This allows stars to adiabatically trail their disks for extended periods of time \citep{Batygin-2012}. In turn, this means that by the time the secular resonance encounter between the stellar spin-axis precession rate and the disk precession rate happens, the disk mass is systematically lower, leading to smaller excitation of misalignment.

Ideally, one would like to examine the sensitivity of the model to the assumed parameters in greater detail, although for such an activity to be meaningful, the underlying physics (particularly in the case of pre-main-sequence rotational evolution) must await some clarification. Therefore, we leave this exercise for a later study.

\subsection{Other mechanisms}

\subsubsection{Perturbations to the planetary orbit}

A few processes of formation of hot Jupiters have been proposed by several authors, who provide the expected distribution of the final inclination of the hot Jupiter with respect to its initial orbital plane. As already argued in Section~\ref{sec:proj}, this angle should be $\Psi$ in the end. We have collected these data from the papers, and derived the expected distribution of the projected spin-orbit angle $\beta$. We refer the reader to the original papers for a detailed explanation of how the distributions of $\Psi$ were derived by the authors. The data is originally in the form of a histogram $(\alpha_i,N_i)$, where $\alpha_i$ is the angle at the centre of the bin, and $N_i$ the number of planets with $\Psi$ in this bin. From this, we constructed $f=\sum_i f(\beta|\Psi=\alpha_i)N_i$, the distribution of $\beta$. We then bin $f$ using the same bins as in the original histogram. We checked that spreading the $N_i$ planets among angles different from $\alpha_i$ in the bin does not change the final histogram of $\beta$ significantly.

The results are shown in Figure~\ref{fig:All}. The red line with \texttt{+} symbols labelled \texttt{F.T. 2007} represents the distribution of $\beta$ expected in the \citet{Fabrycky-Tremaine-2007} mechanism of Kozai cycles with tidal friction (their Fig.~10b providing $\Psi$ in bins of $10^\circ$). The blue line with stars labelled \texttt{N.I.B.2008} corresponds to the distribution found by \citet{Nagasawa-etal-2008} in their model of planet-planet scattering, tidal circularisation, and Kozai mechanism\,; the data is taken from their Figure~11c, which shows the histogram of $\Psi$ of formed close-in planets in all simulations, with bins of $0.1$~rad. The green line with circles labelled \texttt{B.N.2012} corresponds to the distribution found by \citet{Beauge-Nesvorny-2012} in their model of multi-planet scattering, in the case of three planets after 1 Gyrs of evolution (their fig.~16). All the distributions of $\beta$ have been normalised to have $18$ cases with $\beta>40^\circ$, for an easier comparison.

\begin{figure}
\includegraphics[width=\linewidth]{./All-vs-Obs_.eps}
\caption{Distribution of $\beta$ expected from several mechanisms of forming hot Jupiters. Background histogram\,: observations.}
\label{fig:All}
\end{figure}

The agreement between the curves and the histogram beyond $40^\circ$
is in general satisfactory. Based on the small number of planets
observed in each bin, it seems impossible to exclude one or the other
mechanism at present. However, none of these processes can
individually account for the sharp peak at $\beta<20^\circ$. To this
end, \citeauthor{Beauge-Nesvorny-2012} point out that ``\emph{it is
  possible that the population of hot Jupiters with $\beta<20^\circ$
  have a different origin}''.

It should be noted, however, that \citet{Beauge-Nesvorny-2012} had
studied other scenarios, varying the inital number of planets, and the
final age of the systems. Four different cases are shown in their
paper, giving four different distributions. In particular, we have
checked that the case with four planets, after 3~Gyr of evolution,
once normalised to the $\beta>40^\circ$ cases, would give an excess of
aligned hot Jupiters compared to the observations. Thus, one can not
exclude that a combination of all the distributions matches the
observations. We found that their four published distributions give an
excess of planets in the $20^\circ<\beta<60^\circ$ range, but this
concerns only four cases. Actually, the observations do sample the
parameter space (in age and unknown initial conditions), so making a
combination would be appropriate.

\subsubsection{Perturbations to the stellar apparent spin}

Along a completely different line of thought, \citet{Rogers-etal-2012,Rogers-etal-2013} have proposed the misalignments to arise from the modulation of the outer layers of the host stars by interior gravity waves, rather than relics left behind by the dominant transport mechanism.

\citet{Cebron-etal-2011,Cebron-etal-2013} also suggest that the excitation of the elliptical instability in the star by the tides raised by the planet could give an apparent tilted rotation axis. Even the total spin of the star could change direction, if the coupling with the planet is efficient. This will also lead to misalignment between a star and its hot Jupiter.

In order to assess the viability of these intriguing ideas, an expected distribution of spin-orbit angles should be generated within the framework of these models, and compared against the observed distribution via a treatment such as that presented in this work.

\section{Discussion and conclusion}

In this paper, we provide a simple derivation of the probability
density function of the projected spin - orbit angle $\beta$, for
fixed real spin - orbit angle $\Psi$. This allows us to link models
(that produce distributions of $\Psi$) to observations (that measure
$\beta$).

Firstly, our geometric description shows that only positive values for
$\beta$ and $\Psi$ are sensible. These angles are between $0$ and
$180^\circ$, where $\Psi=0$ corresponds to prograde aligned orbits,
and $\Psi=180^\circ$ to retrograde aligned orbits. In particular, the
notation $\lambda=-\beta$ often found in the litterature is
irrelevant.

Second, we find that the observed distribution of $\beta$ presents a significant excess of quasi-aligned hot Jupiters ($\beta<20^\circ$) compared to the one expected from most models. This suggests that the scattering models and the Kozai cycle tidal friction models can not be solely responsible for the production of hot Jupiters. In previous studies \citep[see][]{Winn-etal-2010,Albrecht-etal-2012}, the excess of nearly-aligned hot Jupiters has been attributed to tidal re-alignment of the star. However, \citet{Rogers-Lin-2013} recently pointed out that tidal re-alignment preferentially leads to prograde aligned, retrograde aligned, or orthogonal spin-orbit angles, in some contradiction with the observed distribution \citep{Lai-2012}.

Third, in the simplest variant of the disk-torquing model, the over-representation of quasi-aligned planets is also not reproduced if the binaries responsible for the excitation of orbital obliquity have orbital semi-major axes smaller than $\sim 10^3$\,AU. However, within the framework of the picture envisioned by \citet{Batygin-Adams-2013arXiv}, alternative explanations are possible. These include adiabatic trailing of the host star, and early stripping or non-existance of the binary companion. In fact, the fraction of aligned disks increases dramatically with the maximum semi-major axes of the exciting binaries, $a_{\rm max}$. To this end, it is also worth noting that the wide binary fraction in star formation environments is a strong, growing function of primary stellar mass \citet{Kraus-etal-2011}. Thus, a thorough investigation of the mass-dependence of the disk-torquing mechanism appears worthwhile.

On the other hand, the expected distribution of $\beta$ for $\beta>40^\circ$ in the disk-torquing model hardly depends on $a_{\rm max}$, and is in very good agreement with the observations. Although other parameters, poorly constrained, can have an influence on the distribution of $\Psi$ and $\beta$ in the disk-torquing mechanism, we can conclude that the presently observed distribution of the spin - orbit angles is compatible with most hot Jupiters having been transported by smooth migration inside a proto-planetary disk, possibly torqued by a companion.

\subsection*{Acknowledgments}
K.B. acknowledges the generous support from the ITC Prize Postdoctoral
Fellowship at the Institute for Theory and Computation,
Harvard-Smithsonian Center for Astrophysics.  This research has made
use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at
\texttt{exoplanets.org} \citep{exoplanets.org}. We thank the referee
C. Beaug\'e, as well as D. Nesvorny, for comments and suggestions that
led to improvement of this article. We further thank S. Tremaine for
having pointed out a mistake (now corrected) in our section 2.4.

\small

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


text:
Footie Central | Football Blog Blogging the football world
– EFL Championship
Home » Famous Quotes » - Players » Eden Hazard Quotes: Best Eden Hazard quotes
Eden Hazard Quotes: Best Eden Hazard quotes
Posted by: Kieran Keogh June 19, 2020
Eden Hazard has gone on from strength to strength in his career especially at Chelsea as the quick and skillful Belgian has made a good impression on the football world.
With his career currently at a turbulent stage at Real Madrid it's important to look at what he can do when he is the main man in the team and he can be an extremely important player.
During his career Eden has won two Premier Leagues, one FA Cup and two Europa Leagues first one coming with French side Lille and the second one with Chelsea.
Hazard is currently the captain of the Belgian National team and has won 106 caps whilst scoring 32 goals for his home country.
The position he is in now with Real Madrid is not ideal for the 29-year old, however, we know he has the quality to dust himself off and become even better because let's forget, he has done that before at Chelsea.
He had nine months without a goal which scuppered his confidence dreadfully, but it was the moment he scored his first goal since his last tat he changed back into the player Chelsea fans knew and loved.
We will now take a look at what the football world has to say about Eden Hazard.
"Does he have the capacity to reach the level of a Messi or Cristiano? Now I say yes, because his evolution is great,"
"He's faster than Zidane, more technique than Thierry Henry."
—Christophe Dugarry
"He can play in any top team in the world, today or tomorrow."
"After Messi and Ronaldo, Hazard is my favourite player. "I love watching him because he is a player who creates things, and it is often spectacular to see him play.I love the player and that's all."
"He is a legend, look at what he achieved in six years at the club. He won the league twice, won the FA Cup, won Player of the Year. We are talking about Eden Hazard. Please! "He brought something that we hadn't seen for such a long time".
—Dider Drogba
"Hazard is one of those very talented players that the public loves to see. One of those players who fill the stadiums,"
"Eden Hazard's definitely at the very top, He's such an unbelievable player. The more I've spent time with him the more I appreciate him as a player, but also as a boy."
"He's been great. I would love to have him for longer."
"I said on commentary that he is the best player in the Premier League. It's not because he scored that goal, I believe it. I think he should have been named the best player of the World Cup also. He is an absolute superstar".
"Eden Hazard is a special player" "You need at least at 6 players to handle Eden Hazard he's a fantastic player"
"He is the type of high-level player like Lionel Messi and Cristiano Ronaldo, this type of player is difficult to stop. These type of players need special attention"
"This is a player, you don't worry about tactics you just tell him to go out there and play anywhere out on that pitch, he's got so much ability".
"Switch on the TV, look at him, immediately you realise his qualities. You know his qualities better than me. He's an exceptional player. One, by far, one of the best players in the world."
"He has been the Premier League's outstanding player over the whole campaign, and he deserves the individual recognition. That is how I felt in 1995 when I won the title with Blackburn Rovers and was also Player of the Year for the first time."
"The bad news for Chelsea's rivals is that at 24, Hazard is only going to get better. In three or four years, I think we could be talking about the Belgian being the best player in the world – he has the potential to be that good."
"I consider Eden Hazard to be a really, really top player"
"One character you cannot miss is Eden Hazard. He's on fire. He's probably the best player in the Premier League".
"A player like him (Hazard) can make a difference"
"It is a privilege for a striker to have a player like him or Juan, Oscar or Lamps behind you.
"We have seen only 70%, 75%, 80% of his potential," "If he is able to improve, he will be the best player in the world without a doubt."
"It depends on the players you have. If I had (Eden) Hazard, I would give it to him and he would make the difference,"
"I think he'll be seen as being one of the best players in the world. His skill on the ball, how he does it at speed, he's just a world-class player" "He's at the top of the tree in terms of ability on the ball, awareness and skill"
"But believe me he really is and he's up there with Messi and Ronaldo without a shadow of a doubt. I've seen him day in, day out for the last five/six years and he's a top, top player and he will only get better as well."
"He's been the spark with the players and the fans, he's brought something different and he's got much more to give. He needs to get a run of games and continue playing because he could be at the top."
"If you take Ronaldo and Messi away, I don't think you can find another player as decisive as Eden Hazard". "Eden has won the league at Lille, a team that didn't have the right to win it. And he has won the league at Chelsea in two different projects.
"I think Hazard is the best player in the Premier League I've seen talk about maybe Van Dijk winning Premier League POTY, but there should only be one winner and his name is Eden Hazard. I watch Chelsea matches just because I want to watch Hazard play.
"Eden Hazard is a Chelsea legend no matter what"
"Hazard is a player of the highest level who comes to win everything: the Champions League, La Liga and the Cup."
Kieran Keogh
Editor of Vital Charlton and a passionate Charlton fan. Kieran has been involved in the Charlton press conferences and local newspaper News Shopper and has met with the Charlton manager Lee Bowyer on numerous occasions. He is a regular in the press box on matchdays and also reports on U-23 games.
Hazard set to become the highest paid Premier League player
The Sun reports that Eden Hazard is set to become the top earner in the…
Real cool interest in Eden Hazard
According to The Evening Standard, Real Madrid's interest in Chelsea star Eden Hazard has cooled.…
Real Madrid board block move for Eden Hazard
According to the Metro, reports in Spain suggest that the Real Madrid board have told…
Eden Hazard has another French club as preference over PSG
Chelsea star Eden Hazard has downplayed the rumors linking him to the French side PSG…
CFC Chelsea eden hazard Real Madrid RMA 2020-06-19
Follow Us: @_Footiecentral
RT @kristianreed: 15 years ago today since tiki-taka football was invented between Scunthorpe and Brentford Never forget https://t.co/exV… 2020/11/26
Spurs striker hunt continues https://t.co/t2qmf4FV58 2020/09/30
PSG want to sign Jorginho https://t.co/1RvOFgldTQ 2020/09/30
United midfielder linked with Lazio https://t.co/W2zWXcXwmv 2020/09/30
Chelsea to bid for Rice https://t.co/UcB0Up5n4f 2020/09/30
Biggest Football Controversies
– Managers
FIFA Ballon d'Or
Football Comparisons
Football Records
Greatest Underdog Stories
Managerial Legends
The Best FIFA Football awards
Tournament in Focus
– AFCON
– Bundesliga
– Club World Cup
– English Premier League
– FIFA World Cup
– Indian Super League
– La Liga
– Ligue 1
– Primeira Liga
– Scottish Premiership
– Serie A
– Super Lig
– UEFA Euro
Unpopular Opinions
Ighalo hopes for MLS move
Spurs and Chelsea eyeing South Korean centre-half
Forgotten man departs Chelsea
Arteta given limited transfer budget
Lingard eyeing Nice move
AC Milan AFC Arsenal Aston Villa AVFC Barcelona Bayern Munich Borussia Dortmund Bundesliga CFC Championship Chelsea CPFC Crystal Palace EFC Euro 2016 Everton Fulham inter milan Juventus La Liga LCFC Leicester City LFC Ligue 1 Liverpool manchester city Manchester United MCFC MUFC napoli newcastle united NUFC Premier League PSG Real Madrid Roma Scottish Premiership Serie A THFC tottenham hotspur west ham united WHUFC Wolverhampton Wanderers WWFC
Copyright © 2020 Footiecentral.com All rights reserved. Information on Footiecentral.com may not be published, broadcast, rewritten, or redistributed without prior written authority of Footiecentral.com


Actors Tiger Shroff and Shraddha Kapoor will be seen promoting their forthcoming film "Baaghi" on ace comedian Kapil Sharma's show "The Kapil Sharma Show".Shraddha took to Twitter to share a photograph of her dress that she is going to be seen wearing on the show."On 'The Kapil Sharma Show'! Stylist Tanya Ghavri and make-up/hair Shraddha Naik and Amit Thakur," Shraddha wrote alongside the image.The duo shot for the episode on Monday. Comedian Sunil Grover, who is part of the show, also took to the micro-blogging site to thank the "Baaghi" stars for appearing on "The Kapil Sharma Show"."Thanks 'Baaghi' family. Such happy and positive energy. Had lots of fun," Sunil tweeted."The Kapil Sharma Show" will start on April 23 on Sony Entertainment Television.The first episode will feature Bollywood superstar Shah Rukh Khan.Shraddha and Tiger will appear on the second episode of the show which will be aired on April 24.


My first memory of Václav Havel is of watching the news as a kid, after the Hanna-Barbera cartoons, and seeing pictures of Havel in his living room: a prison of stuffed bookshelves. For me, Havel was the image of a literary hero, an ideal of literature as integrity.
This was why, in the summer of 2010, I found myself proposing a Paris Review interview to Havel. I wanted to ask him my own series of Prague questions, about his love of Bohumil Hrabal's stories, the cinema of the Czech New Wave, his intuition of farce … These questions, basically, were one big question: What was it like for a writer, as he did, to end up in the Presidential Palace?
The Interview, however, turned into a melancholy comedy of its own.
When we met, in November 2010, Havel was seventy-four, and in the middle of postproduction on his first movie: an adaptation of his last play, Leaving, which was first put on in Prague in 2008, five years after he'd left the presidency of the Czech Republic. The play tells the story of Vilem Rieger, a former chancellor of an unnamed country, who must either support the new regime of his previous deputy or be forced from his state-owned villa.
Havel was neatly dressed in a black turtleneck and a black corduroy jacket. He looked, I thought, sometimes like William H. Macy and sometimes like Asterix. He was magnificently small. His offices were around the corner from the Café Slavia and the National Theater. They were kept tropically warm: for Havel, who had already had one lung removed, lived in constant danger of respiratory problems. On the walls, there were photos of Havel with Obama, with the Prince and Princess of Wales, with the former Pope. There was a kind of rich, jazzy, sixties style to the furniture: angles and leather, black and red.
But as the conversation proceeded it became clear that my ideal dialogue would have to wait. Havel's exhausting work on his film meant that, for the moment, he could only offer me forty minutes. Time, therefore, was the first problem. The second was language. I asked my questions in English, then Havel replied in Czech—very quickly, and very softly—and then his translator translated. Which is another way that language connives in unreality.
The film of Leaving premiered around four months later, in March of this year. Earlier that month, Havel had been hospitalized following an inflammation of the lungs. After the premiere, his personal assistant politely wrote saying that they had indefinitely cleared Havel's schedule.
When I heard with sadness this weekend that Havel had died, I considered our transcript. It was so sketchy that it felt more like a bootleg tape. But, then again, maybe that was right. Because, famously, Havel's Prague Revolution was also American, a revolution in love with the New York counterculture. And after all, the last thing that I'd talked about with this hero of the Velvet Revolution was his love of the Velvet Underground.
You began your most recent play, Leaving, before the Revolution of 1989. Could you describe the process of this play's composition?
Before the 1989 Revolution, I had an idea for a character like King Lear, who loses power, and then the world starts to disintegrate. It might have been the influence of the generation of 1968—the people who had been party members, who had professional careers. And then all of a sudden after '68 they were thrown out and started to live ordinary lives, and they pretended that they didn't mind, but in fact they did. I was also trying to make certain references to other works. There's a certain hint of King Lear, a certain hint of Chekhov's The Cherry Orchard, a certain hint of Samuel Beckett. Mostly they were just references for myself.
There are also many moments when you quote from your own essays. In one essay you say that man should be at the center of politics. This phrase gets repeated, sarcastically, in your play. It's almost as if you're writing the play against yourself.
I think it's important for one to take a certain distance from oneself. I've always tried to see the absurdity of my own dealings, my own acts—and I think that this is reflected not just in the plays but in my civic life as well. I always noticed, even in my dissident life, the comical moments.
In your work there's a very porous boundary between the absurd and the political. In your 2007 memoir To The Castle and Back, you suddenly use the term "Ptydepe," the nonsense language you invented in your 1965 play The Memorandum, to describe the language of European Union communiqués. And I wonder if there's something specifically Prague about this—in showing the gap between a word and its meaning. Are there other Central European writers who influenced you?
I like Hašek, with his very original and very specific sense of humor. And Ionesco really influenced me in my youth in the late fifties, together with Beckett and Genet. But if I were to say who influenced me most, then I'd say Franz Kafka. And his works were always anchored in the Central European region. About twenty years ago, I was awarded an honorary degree at the University of Jerusalem where I gave a speech called "Franz Kafka and my Presidency." I basically said that if Franz Kafka hadn't written his works, then I would have had to do it for him. Which sounds a bit vain, but I think people understood what I meant.
I remember that in the fifties you also wrote one of the earliest essays on Bohumil Hrabal.
I was one of the first people, maybe the first person, to write about his work. It was published in one of those samizdat pamphlets. I was very young then, about twenty, and people noticed this particular piece. He wasn't published then. He was working in some waste-collection point, where he was sorting rubbish. The first texts by Hrabal were absolutely breathtaking, like Jarmilka. It was a very short novel—it was rough, it was almost surreal, it was mysterious, it had a very tense note to it. Later, in the sixties, Hrabal started to be published—and his texts were smoother, more polished, cleaner, which resulted from the fact that, unfortunately, he listened to his editors.
Why did you decide to make Leaving into a film?
Originally, it wasn't my idea to make a film. A Czech director thought of it. But then I decided I could do it myself. I'd always had so many other people interpreting my texts and putting them in movies.
Did Jan Němec and his generation of filmmakers—like Jiří Menzel, and Miloš Forman—influence you?
We were the first generation unstained by the conflict of Communism or anti-Communism: we were still young in the postwar years, in February 1948. We were friends, and even though we were all studying something different, we were close. We shared the same experience: a non-ideological experience. We were a non-ideological generation.
But how far do you think a style can be non-ideological? There's a famous anecdote of Forman in Cannes in May 1968. He was there to show his movie The Fireman's Ball, which had only just gotten past the Communist censors. But Godard and Truffaut, in support of the students in Paris, had stopped the whole festival. They were shouting Communist slogans, in favor of the workers. And Forman, in the end, because he loved their films so much, allowed his film to be withdrawn in solidarity. It's such a strange illustration of the way ideology was fluid, how the experiences of Paris and Prague in 1968 were fundamentally misaligned.
I think it depends on how we define ideological. If we see it as a set of opinions that are fixed, stationary, closed, that have no room for curiosity, that are omnipresent and omniscient—in this sense, we were a non-ideological generation. As opposed to some older friends who could be called left wing, or could be called former Communists, we didn't start with a dogmatic ideology. That's the difference between the two generations.
There's a moment in Disturbing the Peace where you say that every member of the audience must find a play out for themselves. You've always separated this writing from your political essays—but is there a way in which your theory of the audience is also a theory of a citizen in a democracy, of someone who interprets and takes part in a dialogue?
In my opinion, theater shouldn't give advice to citizens. Theater is there to search for questions. It doesn't give you instructions. I always fought for a more humble position in life. For the small, the mysterious: something that can't be summed up in four words. How each citizen takes on his citizenship is very individual. And I think that theater is there to create a certain atmosphere of togetherness. I think people are there to ask themselves questions, as a community.


text:
SNL Fires Shane Gillis After Racist, Homophobic Comments Resurface
By Andy Swift / September 16 2019, 1:04 PM PDT
Courtesy of Comedy Central
Ratings: Perfect Harmony Eyes Lows, Evil Rises, Deputy Dips Again
Good Place Recap: Change Can Be Hell
Live from New York, it… won't be Shane Gillis. The comedian, one of three new cast members recently announced for Saturday Night Live's upcoming 45th season, has been fired over a series of racist and homophobic comments that resurfaced online.
"After talking with Shane Gillis, we have decided that he will not be joining SNL," says a show spokesperson on behalf of SNL boss Lorne Michaels. "We want SNL to have a variety of voices and points of view within the show, and we hired Shane on the strength of his talent as comedian and his impressive audition for SNL. We were not aware of his prior remarks that have surfaced over the past few days. The language he used is offensive, hurtful and unacceptable. We are sorry that we did not see these clips earlier, and that our vetting process was not up to our standard."
(UPDATE: Gillis has responds to his firing by taking a swing at SNL — read his statement.)
Just a few hours after Gillis' casting was announced on Sept. 12, tweets began to circulate with clips from a particularly offensive episode of Matt and Shane's Secret Podcast, which Gillis co-hosted with fellow comic Matt McCusker in 2018. During a conversation about New York City's Chinatown neighborhood, Gillis used a racist slur, asking, "Why do the f–ing ch–ks live there?"
today SNL announced the hiring of its first cast member of East Asian descent, and also this guy pic.twitter.com/0FAGJZJUkK
— Seth Simons (@sasimons) September 12, 2019
Another episode found Gillis referring to Judd Apatow and Chris Gethard as "white f—got comics," calling them "f—ing gayer than ISIS." As if it wasn't bad enough that Gillis made these racist and homophobic comments, one of SNL's other new hires for Season 45 is Bowen Yang, an openly gay Asian-American. The other addition is Groundlings performer Chloe Fineman.
In response to the backlash, Gillis released a statement on Thursday that, frankly, did him no favors. "I'm a comedian who pushes boundaries," he tweeted. "I sometimes miss. If you go through my 10 years of comedy, most of it bad, you're going to find a lot of bad misses. I'm happy to apologize to anyone who's actually offended by anything I've said. My intention is never to hurt anyone but I am trying to be the best comedian I can be and sometimes that requires risks."
Your thoughts on NBC's response to Gillis' comments and non-apology? Drop 'em in a comment below.
If you like TVLine, you'll LOVE our weekly newsletter. Click here to subscribe.
TAGS: NBC, Saturday Night Live, Shane Gillis
GET MORE: Casting News, Controversy, Fall TV Preview


text:
Dokpesi loses APDA battle
written by Taiwo Adediran September 15, 2017
Raymond Dokpesi loses APDA battle
An Abuja High Court in Jabi on Thursday, affirmed Mallam Mohammed Kabiru and Mr Emeka Okegwu as interim National Chairman and interim Secretary of newly-registered All Progressive Democratic Alliance (APDA).
Kabiru and Okegwu were joined by APDA as defendants in a suit by a member of the party, Chief Raymond Dokpesi, who claimed to be the Chairman of the party's Board of Trustees (BoT).
Dokpesi had prayed the court to stop Kabiru and Okegwu from parading themselves as members of the National Executive Committee of the party.
He alleged that the defendants' tenure as members of the NEC of the party expired on March 14, 2017, based on the letter of appointment allegedly issued to them.
The judge, Justice Yusuf Halilu, while delivering judgment on the matter stated that based on facts before the court, the defendants had assumed office as interim officers of APDA before the purported appointment letter.
"Going by exhibits C and D before the court, the Independent National Electoral Commission (INEC) had been relating with the defendants before March 14,'' he said.
Halilu noted that exhibit C, which was the party's letter of application for registration as a political party dated March 2, 2017 was signed by the interim chairman and secretary.
He added that exhibit D was an INEC reply to the application, saying that as a result of this, the defendants could not have been appointed by Dokpesi.
The judge further held that two contradictory letters written by the party to INEC, informing it of its interim National Working Committee meeting were replied by INEC to the defendants.
He stated that going by Section 7 (1) of APDA Constitution, the meeting of the party's interim National Working Committee summoned by the interim BoT chairman should not have held.
He said that this was especially so since the section of the constitution stated that two-third of members of the executive committee should notify the chairman to summon such meeting, which did not happen.
According to the judge, whatever decision taken at the said meeting after INEC's reply to the two contradictory letters could not stand in the eye of the law.
He, therefore, set aside the decision taken at the meeting summoned by Dokpesi, which resulted in the election of Mainasara Ilo as the party's acting national chairman.
Halilu further held that by the provision of the party's Constitution, Dokpesi could not have been its interim BoT chairman since he had not spent up to five years as it stipulated.
According to him, since the party was newly registered, Dokpesi could not have spent five years to qualify as a BoT member.
The judge stated that while filing INEC's form PA1 for registration, the column for BoT was left blank and pointed out that if Dokpesi had been the party's BoT chairman the column would not have been left blank.
"It is clear that High Chief Dokpesi has acted in violation of the party's Constitution, all such acts carried out are hereby set aside," Halilu stated.
"The first and second defendants remain the only national officers and those elected under their supervision," he added.
BBOG to begin street matches in October
Secretary to Bayelsa state govt resigns
Wike Lifts Curfew in Some Local Govt Areas
Olumide Akpata emerges NBA President
D'Tigers begin title defence against I'Coast
Community Policing: Gov. Yahaya Inaugurates Advisory Committee, pledges...
President Buhari summons Oyo-Ita, Kyari over heated argument...
G20: Pope makes case for the poor, marginalised
Nigerians react hours after Wike bans #EndSARS protests...
States get another Paris Club refund
Police to deploy 28,000 personnel for Anambra elections
Switzerland sues Nigeria over vessel detained by navy...


Kimberlin Construction is an owner-operated remodeling company that was established in 1996. We have built many room additions in St.Louis as well as countless other construction projects. We have a crew of qualified men that can handle all your construction needs from a simple plumbing job to a complete renovation of a kitchen.
Our service area is approximately 70 miles around the St. Louis Metro area. We offer a full range of construction services from foundation repairs to fixing leaking roofs and everything in between. No job is too large or too small for Kimberlin Construction.
Have you been dreaming of the new room addition? Kimberlin Construction can also design and build a custom room addition to fit your family's needs. We are a company committed to providing quality craftsmanship and excellent customer service to each and every client, no matter how small or large the project.
We are fully insured and would be glad to provide a list of referrals from satisfied customers. We accept Mastercard and VISA, also we can provide referrals to local lending institutions to help finance your project.
If you have any questions about our company and the services we provide, please take a moment to fill out our contact us form. We look forward to hearing from you.


text:
Home Actors/Actresss Bella Thorne Height, Weight, Measurements, Net Worth, Boyfriend
Bella Thorne Height, Weight, Measurements, Net Worth, Boyfriend
Annabella Avery Thorne shortly known as Bella Thorne is an American actress and singer. She is best known for appearing as Ruthy Spivey in TV series "My Own Worst Enemy". Bella was born in Florida to Tamara and Delancey Reinaldo Thorne. She started her acting career appearing as MC Sideline in short movie "Stuck on You". Since then she has appeared in several movies like Blind Ambition, The Seer, Raspberry Magic, Blended, Big Sky, Blended and many others. However, she rose to fame after appearing as Celia in Alexander and the Terrible. She has also appeared in several TV shows including Dirty Sexy Money, Little Monk, Shake It Up and Frenemies.
Bella Thorne is widely popular for dating superstars. She has been in relationship with actors/singers like Charlie Puth, Tyler Posey and recently, she has highlighted the news by dating reality TV star Scott Disick.
Full Name: Annabella Avery Thorne
Nick Name: Bella
Born Place: Pembroke Pines, Florida, USA
Date of Birth: October 08, 1997
Sun Sign: Libra
Race/ Ethnicity: White/ She has Cuban ancestry on her father's side, while she is of Italian and Irish descent on her mother's side.
Occupation: Actress, Singer, model and dancer
Education: She attended Sylvan Learning Center
Father: Delancey Reinaldo "Rey" Thorne
Mother: Tamara Thorne
Siblings: Dani Thorne (Older Sister), Kaili Thorne (Older Sister), Remy Thorne (Older Brother)
Bella Thorne Height Weight and Body Details
Bella Thorne height weight
Bella Thorne Height: 5 ft 8 in or 173 cm
Bra Size: 32B
Shoe Size: 7 (US)
Bella Thorne Net Worth: Bella Thorne net worth is estimated to be $10 million as per reported by Celebrity net worth.
Bella Thorne Husband/Boyfriend: Currently, she is single after breaking up with Scott Disick recently.
Her previous relationships: Jake T. Austin, Garrett Backstrom, Cody Simpson, Tristan Klier, Tyler Posey, Gregg Sulkin, Charlie Puth, Sam Pepper, Chandler Parsons, Scott Disick.
Her first language is Spanish. She is also fluent at it.
She is Cuban American. Her father had Cuban ancestry and she also has Italian and Irish ancestry.
Bella released single "Watch Me" with Zendaya in 2011.
Her father died due to car accident when she was 9 years old.
Bella has 2 pet dogs – Cocker Spaniel and a wolf hybrid. Apart from dogs, she has six cats and a turtle.
She is good friend with Peyton List.
Gregg Sulkin
Previous articleCameron Boyce Height, Weight, Age, Family, Net Worth, Girlfriend
Next articleCardi B Height, Weight, Measurements, Family, Net Worth, Boyfriend
Jennifer Aniston Height, Weight, Age, Bio, Body Measurements and Features
Milo Manheim Height, Weight, Age, Bio, Body measurement, Net Worth, Family and Facts
Jay Critch Height, Weight, Age, Bio, Net Worth and Facts
Misha - December 25, 2017
Personal Details What is his real name and stage? His real name and stage name is Jay Critch. Occupation and Job He is a rapper. Birthday/Date of Birth He was...
Presley Gerber Height, Weight, Age, Family, Net Worth, Girlfriend
Pia Mia Height, Weight, Age, Family, Measurements, Net Worth, Boyfriend