Deloitte provides auditing, tax consultancy and cybersecurity advice to banks, multinational companies and government agencies.
One of the world's "big four" accountancy firms has been targeted by a sophisticated hack that compromised the confidential emails and plans of some of its blue-chip clients, the Guardian can reveal.
Deloitte, which is registered in London and has its global headquarters in New York, was the victim of a cybersecurity attack that went unnoticed for months.
One of the largest private firms in the US, which reported a record $37bn (£27.3bn) revenue last year, Deloitte provides auditing, tax consultancy and high-end cybersecurity advice to some of the world's biggest banks, multinational companies, media enterprises, pharmaceutical firms and government agencies.
The Guardian understands Deloitte clients across all of these sectors had material in the company email system that was breached. The companies include household names as well as US government departments.
So far, six of Deloitte's clients have been told their information was "impacted" by the hack. Deloitte's internal review into the incident is ongoing.
The Guardian understands Deloitte discovered the hack in March this year, but it is believed the attackers may have had access to its systems since October or November 2016.
The hacker compromised the firm's global email server through an "administrator's account" that, in theory, gave them privileged, unrestricted "access to all areas".
The account required only a single password and did not have "two-step" verification, sources said.
Emails to and from Deloitte's 244,000 staff were stored in the Azure cloud service, which was provided by Microsoft. This is Microsoft's equivalent to Amazon Web Service and Google's Cloud Platform.
In addition to emails, the Guardian understands the hackers had potential access to usernames, passwords, IP addresses, architectural diagrams for businesses and health information. Some emails had attachments with sensitive security and design details.
The breach is believed to have been US-focused and was regarded as so sensitive that only a handful of Deloitte's most senior partners and lawyers were informed.
The Guardian has been told the internal inquiry into how this happened has been codenamed "Windham". It has involved specialists trying to map out exactly where the hackers went by analysing the electronic trail of the searches that were made.
The team investigating the hack is understood to have been working out of the firm's offices in Rosslyn, Virginia, where analysts have been reviewing potentially compromised documents for six months.
It has yet to establish whether a lone wolf, business rivals or state-sponsored hackers were responsible.
Sources said if the hackers had been unable to cover their tracks, it should be possible to see where they went and what they compromised by regenerating their queries. This kind of reverse-engineering is not foolproof, however.
A measure of Deloitte's concern came on 27 April when it hired the US law firm Hogan Lovells on "special assignment" to review what it called "a possible cybersecurity incident".
The Washington-based firm has been retained to provide "legal advice and assistance to Deloitte LLP, the Deloitte Central Entities and other Deloitte Entities" about the potential fallout from the hack.
Responding to questions from the Guardian, Deloitte confirmed it had been the victim of a hack but insisted only a small number of its clients had been "impacted". It would not be drawn on how many of its clients had data made potentially vulnerable by the breach.
The Guardian was told an estimated 5m emails were in the "cloud" and could have been been accessed by the hackers. Deloitte said the number of emails that were at risk was a fraction of this number but declined to elaborate.
"In response to a cyber incident, Deloitte implemented its comprehensive security protocol and began an intensive and thorough review including mobilising a team of cybersecurity and confidentiality experts inside and outside of Deloitte," a spokesman said.
"As part of the review, Deloitte has been in contact with the very few clients impacted and notified governmental authorities and regulators.
"The review has enabled us to understand what information was at risk and what the hacker actually did, and demonstrated that no disruption has occurred to client businesses, to Deloitte's ability to continue to serve clients, or to consumers.
"We remain deeply committed to ensuring that our cybersecurity defences are best in class, to investing heavily in protecting confidential information and to continually reviewing and enhancing cybersecurity. We will continue to evaluate this matter and take additional steps as required.
Deloitte declined to say which government authorities and regulators it had informed, or when, or whether it had contacted law enforcement agencies.
Though all major companies are targeted by hackers, the breach is a deep embarrassment for Deloitte, which offers potential clients advice on how to manage the risks posed by sophisticated cybersecurity attacks.
"Cyber risk is more than a technology or security issue, it is a business risk," Deloitte tells potential customers on its website.
Deloitte has a "CyberIntelligence Centre" to provide clients with "round-the-clock business focussed operational security".
In 2012, Deloitte, which has offices all over the world, was ranked the best cybersecurity consultant in the world.
Earlier this month, Equifax, the US credit monitoring agency, admitted the personal data of 143 million US customers had been accessed or stolen in a massive hack in May. It has also revealed it was also the victim of an earlier breach in March.
About 400,000 people in the UK may have had their information stolen following the cybersecurity breach. The US company said an investigation had revealed that a file containing UK consumer information "may potentially have been accessed".
The data includes names, dates of birth, email addresses and telephone numbers, but does not contain postal addresses, passwords or financial information. Equifax, which is based in Atlanta, discovered the hack in July but only informed consumers last week.


I bought a Ruckus Wireless R300 from a company who upgraded their wireless infrastructrue.
encyption method WPA2-PSK-AES, even without encryption I'm not able to connect to the SSID.
Ruckus support would/could not help me because this device is not covered under an active support contract (which is normal ... I first would like to learn/experience the Ruckus products before I would like to become a Ruckus Partner).
Does anyone has the same issue in the past? Is this a known bug/problem of is this hardware just faulty?
Maybe a firmware isue? I suggest to get an NFR kid from Ruckus trough a reseller. With the stand allone version you dont get a realistic view of the Ruckus product.
well Basic standalone setup with Packet Forward "Local Subnet NAT and Route to WAN", 1 defined local subnet --- under this option, you shall have a DHCP server running in the network.
do u have that ??
Configuration should be something like this.
thanks for the feedback. The problem was a VLAN id mismatch for the Local Subnet and the LAN interface. I thought that the AP could work in a state where the local subnet vlan ID remained on the AP (afaik like Meraki works).
I switch to bridge mode with all vlan ID on 1 and that worked.
I'm still not able to use the NAT mode (I guess because there's no dhcp running in the network?).


"Pakistani officials say the country is on track to eradicate polio in 2019 despite Taliban attacks and superstition that has spurred many parents in the region bordering Afghanistan to refuse to vaccinate their children against the crippling disease…" (1/9).
"Director General of the World Health Organization (WHO) Tedros Adhanom Ghebreyesus said that polio is likely to be eliminated from Pakistan by the end of 2019, according to an official statement on Tuesday. Ghebreyesus, who led a delegation, met with Pakistani Foreign Minister Shah Mahmood Qureshi here and assured the organization's support to the health care system of the country…" (1/9).


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The best Halloween rock songs pay homage to the fun darkness of the holiday while creating an atmosphere that conjures elements of both traditional and modern interpretations of monsters, slashers, graveyards, and hitting your neighbors up for candy–whatever that may mean to you. What you don't want is Bobby "Boris" Pickett's lame Monster Mash looping in endless auditory torture. Instead, let the rollicking music and lyrics of the following songs provide an otherworldly backdrop for your Halloween festivities.
Pet Sematary : The Ramones
A song written for the movie version of Stephen King's "Pet Sematary." No, you can't live your life again, even if you're just a dead dog or cat. Bad things will happen. You can trust horror master King and the Ramones on that one.
Bela Lugosi's Dead: Bauhaus
This two-chord gem is heavy on atmosphere and plays like the electrified chant of a hopped-up vampire cult. An homage to the silver screen's finest Dracula, it is creepy and fast and rocks with a chorus of: Undead, Undead, Undead.
Goo Goo Muck; Green Fuz; Can Your Pussy Do the Dog?: The Cramps
The Cramps, the unofficial official band of Halloween, rate three tunes. While multiple songs by one artist on a playlist generally indicates a lack of imagination, The Hangover must make an exception for The Cramps and their surf-punk-rockabilly sound. With humor and horror, these tunes would get the zombies of the Walking Dead to do the pogo.
Werewolves Of London: Warren Zevon
A Halloween-perfect romp with werewolves, pina coladas at Trader Vic's, perfect hair, and a little old lady getting mutilated late last night. Gory fun. Ah-wooooo!
Pretend We're Dead : L7
By tying a bit of straight-forward feminist populism to traditional Halloween elements, L7 has fun and makes a statement at the same time. The dose of reality offered by the lyrics is bitter chocolate to the bouncing chorus.
Season Of The Witch: Donovan
A natural choice for the holiday, this early piece of psychedelia is spare and moody with haunting vocals and a chilling guitar that winds its way through the melody. A feeling of unease permeates the song.
Midnight Rambler : The Rolling Stones
The Stones provide a blues backdrop to the traditional dark side of the holiday with a gritty piece that includes allusions to the Boston Strangler and images of Jack the Ripper. (This epic 1969 live version provides maximum effect.)
The Killing Moon: Echo and the Bunnymen
This is a masterpiece of atmosphere with themes of fate and loss. The song is performed with grace and gravity. The lyrics and vocals drip with hurt as the music churns on.
After Dark: Tito & the Tarantulas
From the stylized crime and vampire film "From Dusk Till Dawn," Tito Larriva and his band provide a haunting Latin-influenced backdrop to the dangers of the night. Halloween doesn't get any hotter than the dance that Salma Hayek performs to this song in the film.
Spellbound : Siouxsie and the Banshees
The psychedelic punk rocker is a roller coaster ride in both sound and meaning. The lyrics have laughter cracking through the walls and the singer spinning out of control. Fear abounds as the music swirls. This song's otherworldly credibility was substantiated when the song was chosen to play over the closing credits of HBO's Trueblood (season four, episode four) "Spellbound" episode.
Spirit In The Night: Bruce Springsteen
An early Springsteen classic on letting go of our pedestrian existences, if only for a few hours of the night.. This all happens at Greasy Lake, on the "dark side of Route 88" with Crazy Janie, Hazy Davy, and Killer Joe, not to mention lonely and gypsy angels. Sure sounds like Halloween.
Frankenstein: The Edgar Winter Group
One of rock's most well-known instrumentals, it is big, powerful, and fun–somewhat like the monster itself. But that's not where its title comes from. The song earned its name during production and editing, in which recording tape was pieced together with legendary difficulty in the studio.
Party Time: 45 Grave
This was the featured song on 1985's "Return of the Living Dead" by one the first bands to combine punk rock and horror movie themes. Lead singer Dinah Cancer's screeching vocals and the band's deep-throated guitars get this song up and going.
God Gave Rock 'N' Roll To You II: Kiss
Perhaps no other band has spawned as many Halloween costumes as Kiss. For that reason alone, Kiss deserves a song on the list. From children of the '70's to those walking the streets today, the signature back and white theatrical makeup has shaken down countless households for Milky Ways and Three Musketeers. Bonus factor: This arena rocker is bound to confuse any Christian zealots who have a problem with either Halloween itself or any of the "evil" traditions that it is based on.
Tags: halloween, halloween songs, holiday songs, moody music, Music, punk rock, Rock, songs
Categories Culture, Music, Uncategorized
The Hangover's 2010 Person of the Year is Theo Epstein, General Manager of the Boston Red Sox. It might seem odd for the Hangover to tout the GM of a baseball team when so many are doing so much in the world. But Epstein did something that few others on the national stage have the intestinal fortitude (in the words of Gorilla Monsoon) to do: Form a philosophy based on a set of beliefs and then stick to it, even when it is painful and unpopular to do so.
When Epstein took over as GM of the Red Sox in 2003, he instituted an organizational approach based on player development, which could also be supplemented by key free agent acquisitions. Prospects could be used as trade bait or to strengthen the major league team. This strategy, Epstein maintained, would keep the Sox in contention most years. It worked out okay in 2004, when the Sox won the World Series. It also worked in 2007, when they won it again.
However, in 2006, Epstein briefly left the Red Sox because of interference from certain Sox higher-ups (read: Larry Luchino) who wanted baseball decisions made with marketing and "buzz" impact in mind. Only when owner John Henry worked things out so that Epstein could run the Sox his way, without interference, did Epstein come back to the team. Imagine that, a man with principles and integrity. Many of The Hangover's younger readers might not have heard of such a thing.
Which brings us 2010. On the field, the year was a disaster for the Red Sox. Injuries ravaged the team. Important pitchers had sub-par seasons. Some nights half of the lineup looked like they'd been called up from AA Portland. Many pundits screamed that Epstein was short-changing Sox fans by playing young, unproven players and not going out and finding "major league" replacements. Of course, they failed to realize that trading prospects for what would be overpriced "Band Aids" might hamstring the team for years to come.
By sticking to his philosophy, in the 2010 off-season Epstein was able to retool his team into one that is younger, more powerful, faster, better in the bullpen, and better defensively. Sure, 2010 hurt; however, 2011 should be great (The Hangover is predicting an '84 Tigers-type season). But as we all know, (cliché alert) the games are played on the field, and (cliché alert) the games aren't won on paper. At least these moves should have the Sox challenging well into the future. One can't ask for more than that—unless, of course, you're one of those living-in-Mom's-basement, pre-2004 win-it-all-or-else fanatics. If that's the case, have another PBR and call WEEI.
What sets Theo apart from just about every other public figure this year is that despite hardship, bad publicity, and public outcry, he stayed true to his vision. He was willing to endure the slings and arrows of The Knights of the Keyboard, various talking heads, and countless knuckle-headed zealots. This allowed him to place his organization on a course for long term success. Has anyone in Washington heard of such a thing?
Let's compare Theo to some other public figures in 2010:
President Obama sells out the public option of his health care plan before he even brings it to Congress. His health care makeover creates more business for insurance companies, while claiming health care "should be a right for every American." The Hangover fails to see how that jibes.
Obama then agrees to a tax cut (extending the Bush tax cuts) for the wealthiest 5% of Americans, despite saying, "I'm still opposed to it." The Hangover's glad he's not running the Sox. Admittedly, it's a compromise with Republicans so that unemployment benefits can be extended for two million other Americans. Of course, Obama could have taken the fight to the airwaves and the American people. Perhaps a populist outcry could have broken Republican opposition. Coincidentally, it's the five percent getting the break who contribute the most to presidential and congressional campaigns.
Let's not forget the Republicans and Tea-Partiers, who are intent on doing two things: cutting the deficit and lowering taxes. Enough said.
President Obama recently stated:
"We've got to make some difficult choices ahead when it comes to tackling the deficit. In some ways, this [tax cut deal/"compromise"] was easier than some of the tougher choices we're going to have to make next year."
No kidding, and with the integrity that Washington's show this year, good luck with that.
Perhaps someone could invite The Hangover's 2010 person of the year, Theo Epstein, to our nation's capitol. He might be able tell our leaders that it is important to form a set of values and beliefs based on thoughtful consideration, intellect, and logic. Then he could reiterate the importance of maintaining that philosophy, even if it might not be popular to do so. Perhaps he could introduce them to "long term planning" and "responsibility." If he shows them his shiny World Series rings, they might even listen.
Then again, Theo Epstein's biggest worry isn't about getting re-elected. He's only trying to do what he knows is right. And in 2010, that's a singular quality.
Theo Epstein with the 2007 World Series trophy. Perhaps if our leaders in Washington knew they could get things like trophies as a reward, they might show some interest in long term planning.
Tags: 2010, 2010 person of the year, Barack Obama, man of the year, Red Sox, red sox off season, theo epstein
Categories Barack Obama, Baseball, Democrats, Red Sox, Republicans, Uncategorized
The Hangover's 2009 Person of the Year: Tiger Woods
Tiger Woods had a remarkable 2009. He won 6 of the 17 PGA tournaments he entered, finished 2nd three times, and earned over $10.5 million in prize money. Forbes estimates that he also made $100 million in endorsements. In addition, Tiger managed to bed a host of smoking hot party girls and wanna-be celebrities. If not for the fact that Tiger was married with two small children, his 2009 would have been a year for the ages. Instead, all this remarkable success was overshadowed by his wife taking a golf club to both him and his Cadillac Escalade.
So why does the Hangover name an apparent moral degenerate as its person of the year? For the simple fact that in 2009 Tiger's actions benefitted all married American men. No matter what faults we may have, at least we're (presumably) not Tiger Woods, out banging skanky chicks while our devoted, unsuspecting wives remained home caring for our innocent children. No other action (short of bringing home an STD) could anger the average American woman more than that. Tiger has made the rest of us look good. Really good.
You give your wife a vacuum cleaner for Christmas. Your wife thinks: "He may be an idiot, but at least he's not Tiger Woods."
You lose your job. Your wife thinks: "Well, he may be an unemployed lout, but at least he's not Tiger Woods."
You blow the rent money on an impossible five team parlay that busts on the Colts' loss to the Jets. Your wife thinks: "He may be a degenerate gambler, but at least he's not Tiger Woods."
Your wife catches you checking out her sister. Your wife thinks: "He's on the couch for a week, but at least he's not Tiger Woods."
You get drunk and crash your car into a tree. Your wife thinks: "He's a drunken idiot, but at least I didn't have to go out in this cold and beat him with a golf club. He's no Tiger Woods."
Whatever the rest of us may do this year that our wives may deem ignorant, idiotic, or nearly unforgivable, it won't seem as horrible to them as what Tiger Woods did in 2009. Tiger has made the rest of us appear better than we actually are. Thank you, Tiger Woods–the Hangover's 2009 Person of the Year.
Tiger's 2009 in Pictures:
A win at the Buick.
And porn star Joslyn James.
Led to some pain for the Cadillac.
To the average American wife, even Otis looks good now.
Tags: Elin Woods, Person of the Year 2009, Tiger Woods, Tiger Woods Escalade
Categories Family Life, Lack of Culture, Sports, Uncategorized
A cabal of Goose Rocks Beach homeowners is suing the town of Kennebunkport, claiming that they own the actual beach down to the low water mark. The Hangover's first inclination is to consider this class warfare, a case of the "have's" versus the "have not's." However, this cannot be the case, as the nature of the suit clearly indicates that these homeowners have no class at all. Still, as a public service The Hangover has decided to explore the nature of the impending litigation.
Newspaper reports state that the fat cat homeowners are primarily concerned with overcrowding at Goose Rocks. This is odd. There are a limited number of parking spaces at Goose Rocks, thereby limiting the number of visitors who can actually reach the beach. In middle of the summer, the designated "public beach" is not ever close to being overrun. Areas of the "private beach" are sparsely populated at their most hectic. Even at high tide, there is always room for a family (perhaps the beachfront owners are expecting the Manson's) to spread out and enjoy themselves. Hampton Beach in New Hampshire is a crowded beach. In July and August a gnat cannot find enough room there to lay down a blanket. This is far from the case at Goose Rocks.
If the overcrowding issue is a smoke screen, there must be other reasons for the homeowners' desires to keep people off a beach that has been used by the public for hundreds of years. Here are some possible explanations:
Revenge: As residents of Kennebunkport are well aware, there was a property tax revaluation undertaken this past year. This resulted in property taxes rising substantially for those with beachfront and waterfront homes. Perhaps these privileged landowners are angered by the fact that for the first time in 20 years they now have to pay their fair share of taxes. They are extracting their revenge by taking it out on the town and those residents whose taxes were reduced.
Self-Loathing: Twenty-five years ago, Goose Rocks was a mostly middle class enclave with the majority of its residents coming from the suburbs surrounding Boston and southern New England. The small cottages that marked the beach then have (for the most part) been torn down, rebuilt, and expanded. Many of these "new and improved" homeowners are from–as luck would have it–the suburbs surrounding Boston and southern New England. Coincidentally, many people visiting the beach also come from these regions. Perhaps the beachfront owners just don't want to be reminded of the humble origins from which they slithered.
Health: Everyone knows that tourists emanate from anomie-infested suburbs and angst-ridden cities. They are mentally unclean and tainted. Their presence on the beach could undo the serenity brought about by rolling waves and gliding sea gulls. The horror, the horror. Those soiled must be kept away.
Wanna-be-ness: The lawsuit could be a simple case of celebrity envy. By aping various asinine celebrity behaviors, these homeowners could be hoping to view themselves as important and privileged. In 1999, Jim Belushi sued when a house painter had the audacity to walk across the beach adjoining his property. (Belushi lost in court.) Entertainment industry icon David Geffen fought public access to beaches in Malibu. He also lost. But he did get some headlines. Perhaps this could be a feeble attempt for 15 minutes of fame. Maybe these landowners are hoping to be ridiculed in Doonesbury just like "The Dark Leader" Geffen.
General Snobbery: Could it be that these homeowner's are just your average run-of-the-mill snobs who don't wish to associate with "neighbors" who can't afford beachfront dwellings? This would be an ugly reality. That people so tremendously boring and base could actually exist in Kennebunkport would be embarrassing for the rest of us–and thus, we are doubly injured.
InAction As Action
One response to the suit would be to let the beachfront owners have the beach. We have to consider the future. The town would then have reason to ignore the homeowner's pleas for help as the beach continues to erode–and erode it has over the past ten years. Picture a town manager smirking across his or her desk: "Hey, it's your beach. You do something about it."
Then there's global warming and rising sea levels. As reported by National Geographic and thousands of other reputable scientific authorities, global warming will eventually cause sea levels to rise: "A one-meter sea level rise would wreak particular havoc on the Gulf Coast and eastern Seaboard of the United States." Presumably, this includes King's Highway and Sand Point. These homes could eventually land "below" the low tide mark. The Hangover wonders if that wouldn't place them in the public domain. Certainly, the beachfront homeowners would see the justice in that.
(It's interesting to note that should the beach even slightly flood this winter, these same landowners will likely call the fire department to come pump out their soaked basements. Neighbors in the form of volunteer fire fighters, although not allowed to cross their beach, would be actually allowed in the houses themselves. The fire fighters will surely be grateful.)
On the other hand, if one is inclined to act, The Hangover is all for non-violent, civil disobedient protest. When Tony Soprano needed to extricate himself from the purchase of a waterfront property from a high faultin' neighbor, he didn't call for a hit. He brought in the music. He had associates anchor his yacht just off shore from the would-be seller's house and play a steady stream of Dean Martin: Live at the Sands Hotel. After several hours of Deano, the seller cracked and the deal was off.
This could work here. While many of us can't afford a waterfront manse, we do have boats and boom boxes. Picture a pristine Memorial Day Saturday. The Hangover envisions a fleet of 100 Boston Whalers, dinghies, sunfish, and runabouts anchored just outside the low water mark of Goose Rocks Beach. Only instead of the sultry crooning of Martin, selected beachfront homeowners are bombarded with the non-stop punk-guitar crunch of The Clash. An afternoon and evening of Should I Stay Or Should I Go just might work here:
Tags: Goose Rocks Beach, Goose Rocks law suit. beach use rights, Kennebunkport
Categories Family Life, Maine, society, Uncategorized
Shameless Literary Self Promotion
There's nothing more off-putting than the shameless self-promotion that permeates American society like a besotted rug three days after a keg party. That being said, the Hangover would like to announce that its editor, Albert Waitt, has a short story in the Spring 2009 (current) issue of Third Coast, an award-winning journal published by Western Michigan University.
Mr. Waitt's story, "You Open Your Door," is set in the fictional Laurel, Maine, which does bear some likeness to the town of Kennebunkport. However, any resemblance to actual people, places, or events is purely coincidental.
For $9, less than the cost of a martini at a decent bar, you can enjoy some of today's best literature. Third Coast should be available nationally at your finer book stores (especially those that sell organic coffee and 1000 calorie lattes). It can also be ordered directly from the Third Coast editori al offices:
Third Coast
1903 W Michigan Ave.
Kalamazoo, MI 49008-5331
The Best Rock and Roll Christmas Songs
The best rock and roll Christmas songs can be gifts in themselves. After all, how many times can one listen to a pack of dogs barking Jingle Bells or even the great Burl Ives crooning Rudolph the Red-Nosed Reindeer? And enough with the Fa-La-La-La-La's. Luckily, rock is a genre whose songs encompass all aspects of the holiday. There's the merriment, good cheer, hope, peace, goodwill towards fellow man, heartbreak, spirtiuality, and class warfare. Before this holiday was co-opted by riot-inducing consumerism and Martha Stewart holiday perfection, Christmas was fun. These songs will make it so again.
A Merry Jingle by The Greedies (aka The Greedy Bastards)
A Merry Jingle is a 1978 punked-out mash up of Jingle Bells and We Wish You a Merry Christmas. And it's preformed by a legendary band: Steve Jones and Paul Cook of the Sex Pistols, along with Phil Lynott, Brian Downy, and Scott Gorham of Thin Lizzy. This is the musical equivalent of a snow-cooled six pack delivered by a Victoria Secret model clad in a Santa's Helper mini-dress. (While the Greedies' version is veritably unavailable, the Backstreet Girls worthy cover of the song is available here on Amazon.)
Run Rudolph Run by Chuck Berry
This is likely the first rock 'n roll Christmas song, released by Berry in 1958. It's old school Chuck Berry, a holiday Sweet Little Sixteen that has Rudolph "whizzing like a saber jet" and Chuck "reelin' like a merry-go-round." A fitting tribute to a great reindeer.
The Grinch by Mojo Nixon and the Toadliquors
Mojo Nixon's cover of "You're a Mean One, Mr. Grinch" isn't one for the kids. He lets the low-down, present-swiping creature have it in a Bad Santa, no-holds-barred, swear-filled rampage. What else would one expect from the great Mojo, protector of virtue and wholesome Christian values?
I Saw Mommy Kissing Santa Claus by John Mellancamp
This is straight-ahead holiday roots rocking where a real good time is being had by all. You've got to love the accordion that gives the song a real jump. Mellancamp's cover songs never disappoint and just like Santa, he delivers here.
Christmas Wrapping by the Waitresses
This is no-doubt the greatest of the new wave Christmas songs. The 1981 song tells a story that is relevant today. The over-worked, harried (sound familiar?) singer misses connection with a potential beau all year, only to have that Christmas magic work things out because of forgotten cranberry sauce. A bouncy pace and excellent horns give this suburban rap a sweet bite.
Sleigh Ride by The Ventures
Instrumental greats The Ventures give their surf treatment to Sleigh Ride, and it is a beautiful thing. No sappy lyrics. No over-emoting singer. Just wave after wave of holiday surf.
Happy Christmas (War is Over) by John Lennon
John Lennon doesn't go intellectual here. There is nothing to decipher. Gratitude, hope, and good will are up front and unabashed. All Christmas music should have as much heart and as little pretension.
Little Saint Nick by The Beach Boys
Nothing says Christmas like the sun-drenched harmonies of the Beach Boys. They give Santa's sleigh the Little Duece Coupe/Shut Down car song treatment. Christmas soars with the high notes of the vocals.
2000 Miles by The Pretenders
Chrissie Hynde's voice has been described as snarky, sultry, smoky, and sexy. But on this heartfelt song of longing, it's simply pretty. Heartache and hope never sounded so beautiful.
All I Want For Christmas Is A Rock n Roll Guitar by The Stompers
Boston club-goers will recognize this tilt by The Stompers. Sal Baglio and the band plead for the one present that will make life complete. And they do it in the all-out style that the band was known for. They just don't want the guitar, they need it.
Blue Christmas by Elvis Presley
The King puts his stamp on Christmas with several songs, but none have the depth of this one. In an unplugged segment of his '68 Comeback Special, Elvis lets his voice carry the song. Elvis could do it all–and here he shows how it's done:
Father Christmas by The Kinks
Leave it to Ray Davies to bring a dose of economic reality to Christmas with typical Kinks crunch. Davies points out that not everyone's holiday is egg nog, over-sized Teddy Bears, and carols by the fire. His character, a department store Santa, is accosted by a gang of kids. As usual, Davies' lyrics are humorous and poignant as the kids tell him:
Father Christmas, give us some money
We got no time for your silly toys
Well beat you up if you dont hand it over
Give all the toys to the little rich boys
Have yourself a merry merry christmas
Have yourself a good time
But remember the kids who got nothin
While youre drinkin down your wine
It's a Christmas message for us all.
Tags: christmas music, christmas parties, christmas songs, Elvis Presley, holiday music, holiday songs, holidays, john mellancamp, Music, Rock

redpajama_set_name: RedPajamaCommonCrawl


text:
Quillwork
By Wyoming State Museum
Quillwork, or the use of dyed, flattened porcupine quills as a means of decoration, is unique to the indigenous people of North America. The porcupine's habitat ranges from Maine to Alaska, and quillwork decoration emerged in most places his quills could be found. Dyed with aniline dyes or in "teas" made of natural materials, the quills are softened in the mouth and then wrapped around thread or sinew stitched to tanned leather. Designs can be simple or complex, and there are many ways of wrapping and plaiting the quills to achieve different patterns. Examples of Quillworking have been found that are at least 400 years old, and quillworking toolkits dating to the 6th century AD. The Wyoming State Museum presents examples of quillworking here and in "Unbroken Circle," our permanent exhibit of Native American history at our museum in Cheyenne, Wyoming.
Bag, Pipe Bag, PipeWyoming State Museum
Northern Cheyenne. Sometimes quills are taken from a blanket thrown over a living porcupine, sometimes the porcupine is skinned and the quills are plucked from the hide. Some modern quillworkers use quills from roadkill.
Spoon/LadleWyoming State Museum
Sioux, Brule. Next, the quills are sorted by size and dyed. Here, a zigzag pattern of quills adorns a ladle made from buffalo horn.
Possible Bag (1880/1920)Wyoming State Museum
Sioux. Before synthetic dyes were available in the 1850's, quills were dyed with natural pigments. Blue could be made from earth pigments, purple from chokecherry, yellow from bark and red from marsh bedstraw.
Bandolier BagWyoming State Museum
Arapaho. Spectroscopy, X-ray fluorescence and mass spectrometry reveal methods for creating different colors varied from region to region. Aniline dyes made creating bright colors faster and easier.
MoccasinWyoming State Museum
Sioux. Lines of red quillwork tend to be associated with woman's moccasins and were largely made by the Dakota Sioux tribes in the late 1800's.
Baby's BonnetWyoming State Museum
Sioux. Quillwork is usually done by women, who begin to learn the skill around age 10. Induction into a quillworking society is considered a privilege.
Fully Beaded Man's Moccasins (1880/1920)Wyoming State Museum
Sioux. This moccasin shows a "parallel band" quillwork stitch on the vamp and a "zigzag" stitch on the tongue.
ParflecheWyoming State Museum
Sioux. Parfleches, or rawhide bags, were often painted, but this one is decorated with both quillwork and beadwork. Beadwork has become more common as beads are commercially available, but quillwork is still practiced today.
CupWyoming State Museum
Northern Plains. Quilling was not only used on clothing. Here, quilled bars are attached to a tin cup by leather ties.
QuirtWyoming State Museum
Possible Arapaho or Sioux. Given the time intensive nature of quillwork, decorations could be removed from worn-out articles and attached to new ones.
Bag, From the collection of:
Wyoming State Museum
Bag with quillwork, unknown tribe.
Although quillwork declined in popularity after the introduction of glass beads, it has enjoyed a renaissance in recent decades and is still practiced today. This time and labor intensive art repays the patient artist with a a piece which is "totally and completely ours, the genuine article... found nowhere else in the world." -Norman Moyah, quillwork artist.
Organized by the Wyoming State Museum.
Cole, Christina and Heald, Susan. "The History and Analysis of Pre-Aniline Native American Quillwork Dyes." Textile Society of America Symposium Proceedings. Paper 14 (2010).
Halvorson, Mark J. Sacred Beauty: Quillwork of Plains Women North Dakota: State Historical Society of North Dakota, 1998
Horse Capture, John D. et al. Beauty, Honor, and Tradition: The Legacy of Plains Indian Shirts. Washington DC: National Museum of the American Indian, 2001
Green, Pamela Sexsmith et al. "Quillworking: Traditional Artwork Is Being Resurrected." Saskatchewan Sage volume 2 issue 8 (1998).
Orchard, William C. The Technique of Porcupine-Quill Decoration Among The North American Indians. New York: The Museum of the American Indian Heye Foundation, 1916.
Stories from Wyoming State Museum
This is not a basket
US Flags in Plains Beadwork
A Journey through Yellowstone in 1905
Weaving Survival
Related theme
The stories behind what we wear
Indigenous Americas
Be inspired by a growing collection of Indigenous art and culture from across the Americas


Life can either make you or break you. That much we know. How you end up depends on how much pounding you took and how that pounding affected you. I have seen the strongest of man cower by merely the thoughts of storms and seen the weakest of them come out of the storm bruised, battered but stronger.
How old am I? Not old, but absolutely im not getting any younger. The heydays are several humps behind. I know there will be sporadic parties ahead but you won't see me head banging anytime soon. in truth, Age doesn't really mellow you down, maturity does. I've had my fair share of bruising and battering. Did i come out stronger? The truth is; I don't know. I sure hope I did, or at least I will.
The thing about life is that ; the bruising and battering comes and go. Depending on the circumstances. The choices me make and the life we led creates a potent recipe of pounding and battering if you are not really careful or you really care less. The pounding comes in different strengths, this does not depend solely on how strong the hands that wields the hammer, it also depends on how soft you are when you are pounded. Like storms that comes in different strengths, we come out at the eye of the storm with different lesson learned.
The real journey begins after the storms. when you begin to take the initial steps. when you begin to pick up the pieces. little steps, piece by smaller piece. smirk, just a little smirk each day. strength comes with moving. Keep on moving until the steps becomes a journey, until the pieces becomes whole, until the smirk becomes a smile, until the smile becomes laughter, until laughter becomes life.
But until then…we keep moving.
Live, Love, Cry, Laugh, Rant, Run, Live Free, Life is uncharted.
Unedited ang content nitong blog na ito. di ko na binabasa ulit ang anumang sinusulat ko. So kung may mali ang spelling at may grammatical lapses, normal na yun!


Dr. David J. Heldebrant is currently a Senior Research Scientist in the Materials Chemistry and Surface Research Group in the Energy and Efficiency Division at Pacific Northwest National Laboratory. Dr. Heldebrant joined PNNL as a post-doctoral research scientist in 2005.
Dr. Heldebrant's current research involves the design and development of switchable ionic liquids that chemically capture acid gases such as carbon dioxide and sulfur dioxide from power plant gas emissions. Dr. Heldebrant's CO2-Binding Organic Liquids (CO2BOLs) have shown potential to capture CO2 and SO2 using up to 50% less energy compared to existing gas capture technologies.


text:
\section{Introduction}

The accretion of gas onto binary systems is of widespread astrophysical
importance.  For super massive black-hole binaries in galactic
nuclei, the details of gas accretion is important in setting the observational
signatures of such binaries \citep{BlackHoleSignatures,FlowIntoGap} and in
determining the alignment of black-hole spins \citep{BlackHoleAlign1,BlackHoleAlign2}.

Another important application is to the formation of stellar mass binaries.
This is a central problem for understanding star formation since a large
fraction of stars reside in binary systems
\citep{BfracObs1,BfracObs2,BfracObs3,BfracObs4,BfracObs5,BfracObs6}.
It is well known that the initial mass of a proto-binary forming from a
collapsing cloud is a small fraction of the mass of the parent cloud
(except for the widest binaries).  The initial proto-binary forms from
the first material to collapse, which is located near
the clouds centre and thus has low specific angular momentum.  The
proto-binary then acquires most of its mass from the remaining infalling
material, which has greater specific angular momentum.  Because of its greater
specific angular momentum, this material is expected to first form a
circumbinary disc.  The binary then accretes material through inflowing
streams linked to this circumbinary disc.  The ultimate mass
ratio of the binary ($q=M_2/M_1$ where $M_2$ and $M_1$ are
the masses of the secondary and primary components, respectively) is thus
set by the relative accretion rates from the circumbinary disc onto the
primary and secondary components, not by the mass ratio of the initial
proto-binary fragment.

A number of numerical studies have focused on understanding accretion onto
isolated binaries.  These studies have ranged from ballistic calculations
\citep{ArtyBallistic,BateBallistic} to hydrodynamical calculations using
Smoothed Particle Hydrodynamics (SPH) in 3D \citep{BateSPH,Bate_props} and
grid codes in 2D \citep{Ochi,Hanawa,TTauriGrid,ALMA_binary_obs}.  Simulations
of entire clusters have also been used to predict ensemble properties of
binaries \citep{Bate_ClusterSim,Offner_ClusterSim,Goodwin_ClusterSim1,Goodwin_ClusterSim2,Delgado_ClusterSim}.
The resolution of the simulations of entire clusters is inevitably poorer
than in simulations dedicated to a single isolated binary.

SPH (and also ballistic) simulations of circumbinary accretion
have always found a strong tendency for the majority of the accreted mass to
flow onto the secondary. This is because material inflowing from the
circumbinary disc encounters the secondary first, since it orbits further
from the centre of mass of the binary than the primary. Therefore, SPH studies
of binaries at both the individual binary and cluster scale exhibit a
preference for creating binaries with high $q$ values, since material
falling preferentially on the secondary implies $\dot{q}>0$.
This preference is in mild conflict with the observed statistics
of solar mass binaries, which show a flat $q$ distribution \citep{q_dist_disn}.

A re-examination of the accretion of gas onto binaries using 2D grid
based techniques by \cite{Ochi} made the opposite prediction, finding
more mass accreted by the primary.
Although these simulations also showed that material encounters the secondary first,
they found a significant fraction of it continued to flow past the secondary and
became bound to the primary.  Unless $q << 1$ this results in
a \emph{decreasing} mass ratio (i.e. $\dot{q}<0$).  Higher
resolution grid studies \citep{Hanawa} later confirmed that this effect was not a
result of insufficient resolution. \cite{Ochi} hypothesised that the discrepancy with
SPH simulations was due
to excessive numerical dissipation in the SPH code causing accreting particles
to spiral into the secondary instead of transitioning to the primary.

However, as well as using different numerical techniques, the SPH and grid
based studies of accretion onto isolated binaries also differ in the
temperature used for the accreting gas.
Because the dynamical importance of pressure to the flow
of material onto the binary is a function of temperature, it is possible for
gas temperature to qualitatively alter the accretion dynamics.  It
has been suggested that the discrepancy between SPH and grid based
simulations  is due not to numerical technique but to this difference in
temperature \citep{clarke2008pathways}.

Here we explore the hypothesis that $\dot{q}$ depends on the
temperature of the accreting gas, using 2D SPH simulations at a variety
of resolutions and compare our results with SPH and grid based results
in the literature. We also aim to discover the resolution required
in order to accurately determine the mass flow rates on to the primary and secondary
components of a binary (of value to cluster simulations).  Section \ref{sec:model}
describes the simulations performed,
Section \ref{sec:model} reports on the results and
Section \ref{sec:discussion} discusses the application to
astrophysical systems. Section \ref{sec:conclusion} presents our Conclusions.

\section{Binary model}
\label{sec:model}

We model a binary on an anti-clockwise circular orbit,
with mass ratio $q=M_2/M_1$, total mass $M=M_1+M_2$ and separation $a$.
We use  a modified
version of the SPH code GADGET2 \citep{Gadget2Code} in 2D.  We have chosen 2D
SPH in order to facilitate the comparison with the 2D grid
simulations of \cite{Ochi,Hanawa} and since numerical convergence is faster
in 2D than 3D (for $N$ particles, the SPH smoothing length scales as
$N^{-1/2}$ in 2D and $N^{-1/3}$ in 3D).
 In a real circumbinary disc, accretion is driven by the effective
viscosity in the disc \citep{DiscReview,MRI,GiantPlanetGravInstab,PP6}
which feeds the binary with material that has similar specific angular momentum
to that of the binary itself, even if the
material falling into the disc at large radius has a significantly
higher specific angular momentum. In order to avoid the computational
expense of modeling this situation (with numerical or some prescribed
`physical' viscosity driving the secular evolution of the circumbinary
disc) we instead follow previous authors and inject gas
at large radius $R_{inf} a$ with a ratio ($j_{inf}$) of specific angular momentum
to that of the binary ($\sqrt{GMa}$) of order unity (see Table
\ref{tab:model_params}). We set the initial inward radial velocity of the injected
particles so that these particles are initially marginally gravitationally
bound to the binary.
The stars are treated as sink particles so that particles are
accreted if they stray within the accretion radius of each star ($0.01 a$).
We set the SPH smoothing length $h$ using $h=1.2\sqrt{\frac{m}{\Sigma}}$, where
$m$ is the particle mass and $\Sigma$ is the surface
density \citep{PriceReview}.  This choice gives roughly $18$ neighbours per SPH
particle in 2D.  Details of how to access the exact version of the code used,
along with parameter files and initial conditions can be found in Section
\ref{sec:methods}.

We employ an isothermal equation of state which is parameterised in terms
of $c$:
\begin{equation}
  c = c_s/\sqrt{\frac{GM}{a}}
  \label{eq:norm_cs}
\end{equation}
which is the dimensionless sound speed (normalised to the orbital speed of
the binary).  We explore binaries with $c=.05$ and $c=.25$.
For reference, \cite{BateSPH} used $c\le .05$ while \cite{Ochi,Hanawa} used $c\ge 0.18$.
We neglect both disc self-gravity and the back reaction of the disc on the
binary (i.e. we consider the test particle limit).
The resolution of the simulation is set by parametrising the mass infall rate
in terms of the number of SPH particles
introduced per dynamical timescale of the binary ($\sqrt{{a^3}\over{GM}}$),
so that (at fixed time) the number of particles in the simulation scales
with $\dot{N}$.

\begin{table}
  \centering
  \begin{tabular}{|l|p{6cm}|}
	 Parameter & Explanation \\
    \hline
    $q=M_2/M_1 = 0.2$ & Mass ratio of the binary. \\
    $j_{\inf} = 1.2$  & Specific angular momentum of injected material
    divided by the specific angular momentum of the binary.\\
    $R_{\inf} = 20 $ & Distance from centre of mass of the binary at which
    material is injected, divided by the binary separation.\\
    $\dot{M}/m = \dot{N}$ & The number of particles injected per
    dynamical time.\\
    $c=\frac{c_s}{\sqrt{\frac{GM}{a}}}$ & Ratio of the isothermal
    sound speed to the orbital speed at one binary separation from the binary
    centre of mass.  Determines the dynamical importance of the pressure
    forces.
  \end{tabular}
  \caption{All the dimensionless parameters which must be specified to
  describe our model.}
  \label{tab:model_params}
\end{table}

Note that the number of injected particles is higher for the `hot' simulations
($c=0.25$: 5-8 in Table \ref{tab:model_params}),
since a significant  fraction of the marginally bound injected
particles are pushed out by pressure gradients. These particles are deleted
from the simulation soon thereafter.
The `cold'   simulations  (with $c=0.05$: 1-4 in Table \ref{tab:model_params})
are each matched with a corresponding hot simulation (5-8)
so that they have roughly the same number of particles actively contributing
to the simulation at any time (see Table \ref{tab:model_params} for the
corresponding values of $\dot N$).

\begin{table}
  \centering
  \begin{tabular}{|l|l|l|l|l|}
    ID & $c$ & $\dot{N}$ & $N_{end}$ & $(h/H)_{sec}$ \\
    \hline
    1 & .05 & 100 & 4e4 & .25\\
    2 & .05 & 200 & 8e4 & .1\\
    3 & .05 & 500 & 2e5 & .06\\
    4 & .05 & 1000 & 5e5 & .04\\
    5 & .25 & 200 & 4e4 & .75\\
    6 & .25 & 500 & 1e5 & .45\\
    7 & .25 & 1000 & 2e5 & .3\\
    8 & .25 & 2000 & 5e5 & .2\\
  \end{tabular}
  \caption{Parameters used for simulations in this paper.  $\dot{N}$ is the
  number of particles injected per dynamical time ($\sqrt{a^3/GM}$),
  $N_{end}$ is the number of particles at the end of the simulation and
  $(h/H)_{sec}$ is the resolution at the edge of the disc around the
  secondary.
  All simulations were run with $a=1.0$, $q=0.2$, $j_{\inf}=1.2$,
  $R_{\inf}=20$ and were run for 500 dynamical times.}
  \label{tab:simulations}
\end{table}

For each simulation, we also measure $h/H$ (SPH smoothing length over disc
scale height) at the outer edge of the circumsecondary disc.  This quantity
measures how well resolved the secondary's disc is at the point where it
interacts with infalling material.  As expected, $h/H$ scales as $N^{-1/2}$,
except for the lowest resolution simulations where it increase more
rapidly with declining particle number.  This rapid increase occurs when the
role of numerical viscosity is enhanced to the point that the accretion time
scale of the circumsecondary disc becomes comparable with the infall time scale.

We analyse all our simulations in the frame co-rotating with the binary,
translated so the secondary is at $(x,y) = (-1,0)$ and the primary is at the origin.
In this non-inertial frame it is possible to modify the gravitational potential to
include the effect of the centrifugal force due to the rotating reference
frame.  This modified potential,  the Roche potential, is given by
\begin{equation}
  \Phi =
  -\frac{GM_1}{|{\bf{r}-\bf{r_1}}|}-\frac{GM_2}{|{\bf{r}-\bf{r_2}}|}-\frac{1}{2}(\bf{\Omega}
  \times\bf{r})^2
  \label{eq:mod_pot}
\end{equation}
where $\bf{r}$ is the position vector, $\bf{r_1}$ and $\bf{r_2}$ are the
positions of the primary and secondary respectively and $\bf{\Omega}$ is the
angular momentum vector of the binary.  Equipotential surfaces of $\Phi$, as
well as points of zero gradient (the Lagrange points) are shown in
figure \ref{fig:Roche_lobes}.

\begin{figure}
  \begin{center}
	 \includegraphics[width=0.5\textwidth]{Figures/Roche_overview.png}
  \end{center}
  \caption{Equipotential surfaces of $\Phi$, the modified potential
  (gravitational potential plus term to include centrifugal force
  of non-inertial frame) for the values of $\Phi$ obtained at the three
  Lagrange points L1,L2 and L3.  The colour map shows $\Phi$ elsewhere.  The
  stars are marked in red (secondary) and green (primary) and the centre of
  mass of the system is marked in blue.  The green and blue lines are the
  locations where the x and y components of the force resulting from this
  potential (i.e., $-\nabla{\Phi}$) are zero.}
  \label{fig:Roche_lobes}
\end{figure}

\section{Results}
\label{sec:res}
\subsection{Dependence of mass ratio evolution on temperature}

The most important quantity in setting the final, post-accretion, value of $q$
 attained by the binary is the fractional change in $q$ normalised to the
fractional change in mass of the binary.   In our
simulations, this value is given by the dimensionless number:
\begin{equation}
  \Gamma  = \frac{(1+q)}{q(\dot{N_1}+\dot{N_2})}\left( \dot{N_2} - q\dot{N_1} \right)
  \label{eq:qdot}
\end{equation}
where $\dot{N_1}$ and $\dot{N_2}$ are the particle accretion rates of the primary and
secondary (obtained by counting the number of particles accreted by each star).
To reduce noise, accretion rates were smoothed by taking a rolling average across one
orbital period of the binary. Figure \ref{fig:conv_accretion_hard}
shows the accretion rates per unit accreted mass, as well as the resulting
values of $q\Gamma$, for the cold (left panel) and hot (right panel)
simulations.  For both the cold \& hot simulations, simulations are shown at
three resolutions, chosen so they are separated by roughly a factor of $2$
in $h/H$ at the edge of the secondary's disc.

\begin{figure*}
  \begin{subfigure}[b]{.49\textwidth}
    \includegraphics[width=\textwidth]{Figures/Accretion_cold.pdf}
  \end{subfigure}
  \begin{subfigure}[b]{.49\textwidth}
    \includegraphics[width=\textwidth]{Figures/Accretion_hot.pdf}
  \end{subfigure}
  \caption{Accretion rates and corresponding $q\Gamma $ (equation
  \ref{eq:qdot}) for cold (left)
  and hot (right) simulations.  Red lines represent
  $q\Gamma$, blue is accretion onto the primary and green is accretion
  onto the secondary (both per unit accreted mass).  The solid, dashed and
  dot-dashed lines represent $h/H = .04$, $.1$ \& $.25$ ($\dot{N} = 1000,200$ \&
  $100$), respectively, for the
  cold simulation and $h/H = .2$, $.45$ \& .$75$ ($\dot{N}=2000,500$ \& $200$),
  respectively, for the hot simulation. The first $\sim 30$ orbits are
  not shown as the simulation has
  yet to settle into a quasi steady-state.}
  \label{fig:conv_accretion_hard}
\end{figure*}

It is clear that significantly more material is accreted by the
primary in the hot simulation than in the cold.  Averaging across the steady
state, this translates into a higher value of $\Gamma$ for the cold
simulation (where $\Gamma \approx 5$) compared with the hot simulation
($\Gamma  \approx 3.5$). We note that for the cold simulation, this
value is
very similar to that found
in the previous 3D SPH simulation of \cite{BateSPH} for the
same parameters, implying that the dimensionality of the problem is
not critical here.

Our result for the hot simulation is close to, but
somewhat larger than, the value ($\Gamma \sim 2.5$) obtained by \cite{Ochi}
for their corresponding model (2-12).  However, the value reported by Ochi
et al is obtained by averaging over a short time period ($t \sim 30$ in the
units of Figure \ref{fig:conv_accretion_hard}) compared to the period of the
variability ($t \sim 90$).  If we average our results on a similarly short
time period, $\Gamma$ can take values between $2.5$ and $4$ depending on when
the average is taken.  Furthermore, the total duration of the Ochi et al simulations
is shorter than the period we have excluded from our analysis on account of it
not being in a steady state.  As such, the value of $\Gamma$ reported by Ochi
et al may still
be partially measuring transient accretion driven by their initial conditions.
Finally, Ochi et al use a different definition of accretion (counting mass
within the entire disc) which we found to produce greater variability.
Given these differences, our results do not suggest a large discrepancy
between grid based and SPH results.

Although we have limited our analysis to
simulations that have already settled to a quasi steady-state, there is still
some time variability in the accretion rates (particularly in the hot simulations)
as has been identified by previous authors \citep{FlowIntoGap,Ochi,Hanawa}.
We find very little change in the accretion rates or average $\Gamma$ with
resolution for the models detailed in Table \ref{tab:simulations},
indicating that our results are numerically converged (see Section
\ref{sec:numerics} for an exploration of lower resolution models).  Note also that the
discs become better resolved as a function of time (as more particles
accumulate in our simulation domain) and so the lack of any secular changes
also indicates that numerical convergence has been reached.

\subsection{Dependence of flow morphology on temperature}

To better understand the flow morphology, we averaged the flow velocity on a
grid over the final 60 binary orbits (the first 30 orbits were ignored as they
represent a transient settling phase).  Figures \ref{fig:streamlines} and
\ref{fig:streamlines2}
shows streamlines constructed from this averaged flow for the highest
resolution cold and hot simulations respectively.  The colour scheme indicates the average
density of the flow, normalised to the average surface density of the
circumbinary disc.

\begin{figure*}
  \begin{subfigure}[b]{.99\textwidth}
    \includegraphics[width=\textwidth]{Figures/Streamlines_cold.png}
  \end{subfigure}
  \caption{Average density and streamlines of the velocity field for the
  highest resolution cold simulation (simulation 4).  The density and velocity
  field were obtained by averaging the velocity and density on a
  grid across roughly 60 orbits.  The colour scheme shows the average
  surface density, normalised to the surface density in the circumbinary
  disc.  Contours of the Roche potential and the Lagrange points are shown as
  in Figure \ref{fig:Roche_lobes}.}
  \label{fig:streamlines}
\end{figure*}

\begin{figure*}
  \begin{subfigure}[b]{.99\textwidth}
    \includegraphics[width=\textwidth]{Figures/Streamlines_hot.png}
  \end{subfigure}
  \caption{The same as Figure \ref{fig:streamlines} but for the hot
  simulation (simulation 8).}
  \label{fig:streamlines2}
\end{figure*}

In both hot and cold simulations, there are two
spiral arms which join the circumbinary disc to the circumstellar discs
via the L3/L2 Lagrange points. In both cases the spiral arm via L2
is much more pronounced than that through L3. This is consistent with
the lower value of the Roche potential at L2 \citep{Ochi} which
provides an energetically favourable route for material inflowing from
the circumbinary disc. The morphology of the flow in the vicinity of L2
is however quite different in the two cases: in the cold simulation
the flow is narrow and the trajectory of its peak surface density is
offset from L2 by around $60$ degrees (measured with respect to
the secondary). The flow traverses the Roche lobe (solid line in
Figure \ref{fig:streamlines}) more or less radially and impacts the disc edge well inside
the Roche lobe. At this point the material becomes entrained in the disc
flow.

In the hot simulation, we find that material of similar
normalised surface density (coded orange) occupies a broad swathe of space between the
secondary and the circumbinary disc and covers nearly half the surface of the
secondary's Roche lobe.
This much broader structure is simply a result of the much larger pressure scale
length in the hot simulations.
Moreover, in contrast to the nearly radial flow seen in the cold simulations,
material entering the secondary's Roche Lobe
describes  more or less tangential trajectories, skirting  the boundary of the Roche lobe
`below' the secondary (at negative y).\footnote{This ``skirting'' behaviour is
aided by outwardly directed pressure gradients which produce a force with a
magnitude of $\sim 20\%$ of the inwards pull of gravity.}
At the lower right
of the secondary (at small negative x), the flow divides into a portion
that is retained within the secondary's Roche lobe and one which flows
out through the saddle region in the vicinity of L1. The latter flow of
material then enters the primary's Roche lobe to the lower left of the
 primary. The pronounced orange figure of eight structure which wraps
around the Roche lobes represents weakly bound material which in some
cases orbits the binary several times before eventually being accreted
into the disc of one of the stars. As noted above, the main feeding sources
for this flow are the two spiral arms from the circumbinary disc, especially
that in the region of L2.

To further explore the modes of binary accretion demonstrated in
Figures \ref{fig:streamlines} and \ref{fig:streamlines2} we computed the
mass flux across the boundary of the Roche lobe in our simulations.  In 2D the
 flux is  $F= \Sigma \bf{v} \bullet d\bf{S}$, which we compute using  SPH
interpolation to estimate $\bf{v}$ \citep{PriceReview,splash} and calculating
 the  surface normal for the critical Roche equipotential.  This flux was then
 averaged over the final 60
orbits at each point on the boundary of the Roche lobe and plotted in figure
\ref{fig:flux} for the highest resolution hot and cold simulations.

\begin{figure*}
  \begin{subfigure}[b]{.49\textwidth}
    \includegraphics[width=\textwidth]{Figures/Boundary_flux_cold.png}
  \end{subfigure}
  \begin{subfigure}[b]{.49\textwidth}
    \includegraphics[width=\textwidth]{Figures/Boundary_flux_hot.png}
  \end{subfigure}
  \caption{Flux across Roche lobe boundary for the highest resolution cold
  (left) and hot (right) simulations.  Negative flux implies an inflow.  The
  flux is normalised by the particle injection rate, $\dot{N}$.  See
  text for the details of how the flux is calculated.}
  \label{fig:flux}
\end{figure*}

Figure \ref{fig:flux} (left) shows that in the
cold simulation the net flux of particles is into the secondary at all points
but is strongly concentrated in the region of the high density feeding
stream (Figure \ref{fig:streamlines}) near L2.
For the primary, a significant fraction of the inflow
occurs in the vicinity of (0., 0.5), which can be seen in Figure
\ref{fig:streamlines} to connect
to L3 via a spiral arm.
The remainder of the primary's Roche lobe is divided into alternating regions of mild
inflow and mild outflow, of which the most significant is the outflow in the region
of L1.  The outflow near L1 is partly re-accreted by the primary and partly
forms a minor input to the adjacent secondary lobe.
Over all, the transfer of material between the Roche lobes
is small in the cold simulation, with only $6(18))\%$ of the material
finally accreted by the primary(secondary) having spent some time in
the Roche lobe of the other star.

The picture is quite different in the hot simulations.
As noted above, the flow into the secondary's Roche lobe in the vicinity
of L2 is much broader and the flow of material once it has entered the Roche
lobe is nearly parallel to the Roche lobe boundary. Although much of this
material is retained
by the secondary, a significant minority exits the secondary's
Roche lobe on the approach to the L1 point and transitions to the
primary's Roche lobe. In the hot simulation this provides the major accretion
stream
into the primary's Roche lobe (i.e. at around (-0.6,-0.1)).
Since this flow is nearly parallel to the critical equipotential,
the remainder of the primary's Roche lobe is  again crossed by alternating
bands of mild inflow and outflow; the outflow at small positive
$y$ in the vicinity of L1 is linked to a corresponding mild inflow
to the adjacent portion of the secondary's lobe.

This circulation of material between the lobes does not greatly
affect the dominant accretion mode of the secondary.
The fraction of material accreting on to the secondary that has ever been in
the primary's Roche lobe is only $21 \%$ in the hot simulation,
a figure scarcely different from that in the cold simulation. However,
 $65 \%$ of the material accreted by
the primary in the hot simulation has spent
time in the secondary's Roche lobe (compared to only $6\%$ in the cold
simulations).

We thus find that the hotter conditions previously modeled by
\cite{Ochi,Hanawa} indeed favour an increased net flow from
secondary to primary.\footnote{We also concur with previous simulations
in finding that the flow morphology and resulting accretion pattern fluctuates
over timescales longer than the orbital timescale due to the shifting location of the
stagnation point near L1.}
This dominant flow
boosts the ratio of accretion  onto the primary to that onto the
secondary when compared with the cold simulation (see Figure
\ref{fig:conv_accretion_hard}).

As noted above, our hot simulation is broadly consistent with
model 2-12 of \cite{Ochi}, a finding which undermines the argument
that previous `cold' results reported in the literature were
corrupted by numerical issues associated with SPH. Nevertheless we next discuss
whether our results are likely to be corrupted by excessive numerical
dissipation.

\subsection{Numerical effects}
\label{sec:numerics}

The models presented here represent some of the highest resolution
simulations of this problem conducted to date. This statement
may seem surprising given the relatively modest numbers of particles
involved (see Table \ref{tab:simulations}) but is based on an evaluation of the
ratio of a resolution element to the local pressure scale
height \emph{in the vicinity of the Roche lobes} ($h/H$). For our highest
resolution cold simulation the ratio of SPH smoothing
length to pressure scale height in this region is $0.2-0.5$  while
the corresponding value for the previous (3D) cold
SPH simulations of \cite{BateSPH} is of order unity. For our
highest resolution hot simulation this ratio is
$0.04-0.1$, somewhat less than in the grid based simulations
of \cite{Hanawa} and comparable with the simulation of
\cite{Ochi}.\footnote{For grid simulations, we consider the ratio of grid
cell size to pressure scale height.}
We note that grid based codes have not previously been used to
model `cold' conditions, because of the difficulty of resolving the
inner regions of the circumstellar discs in this case.

Given our agreement with lower resolution results in the literature
it is unsurprising that we have demonstrated that our results are
numerically converged.  The SPH smoothing length varies
by around a factor $5$ between models $1/4$ and $5/8$, yet the difference in
fraction accretion rates (shown in Figure \ref{eq:qdot}) is at the $10\%$
level.
This suggests that resolution is \emph{not} a key factor in determining which
component of the binary accretes material. This is difficult to reconcile with
the conjecture of \cite{Ochi} (which ascribed the results from SPH
simulations to excessive numerical dissipation in SPH) since such
dissipation is a function of resolution.

As a more direct  test of the effect of numerical dissipation, we follow
\cite{Ochi} and calculate the Jacobi constant $J$ along representative
particle trajectories in our simulations.  For an isothermal equation of
state in 2D, $J$ is given by
\begin{equation}
  J = \frac{1}{2}v^2 + \Phi + c_s^2\ln{\Sigma}
  \label{eq:jacobi}
\end{equation}
where $v$ is the particle speed and $\Phi$ is Roche potential defined in
equation \ref{eq:mod_pot}.  This quantity is just the Bernoulli constant in a
rotating reference frame and so, for an inviscid flow in a steady state, is conserved
on a per-particle basis.

We find that for all particles, $J$ only undergoes significant changes on
timescales shorter than the dynamical time at shock-fronts.  An example is
shown in Figure \ref{fig:jac_examp}, where a particle in the near radial
accretion stream in the cold simulation impacts the secondary's circumstellar
disc.
Away from obvious shock-fronts (such as where the particle in
Figure \ref{fig:jac_examp} strikes the disc), we find $J$ to be conserved
to within a few percent on a dynamical
time scale. This means that the material that is skirting the lower edge
of the secondary's Roche lobe in Figure \ref{fig:streamlines2} should change its
orbital radius due to numerical viscosity by no more than a few per cent in its
first half-revolution around the secondary. Evidently, such a tiny change would have
very little effect on which streamlines should remain confined within the
secondary's Roche lobe and thus on the resulting flow from secondary to
primary.

\begin{figure}
  \begin{center}
	 \includegraphics[width=0.5\textwidth]{Figures/Jacobi_trajectory.png}
  \end{center}
  \caption{The Jacobi constant for a single particle at different points along its trajectory (cold simulation).}
  \label{fig:jac_examp}
\end{figure}

We therefore find no evidence that our results are driven by unphysically large
numerical viscosity effects. In order to compare grid based
and SPH results in more detail it will be necessary to compare
numerically converged results for the same parameters and for
simulations that have been run to a quasi-steady state. Such a comparison
is currently not possible since the higher resolution simulations
reported by \cite{Hanawa} are subject to large secular variations
in accretion rates throughout the duration of the experiment.

Finally, we explore the effects of degrading the resolution further, motivated
by a desire to understand the potential systematic effects of under-resolving
binary gas flow in large scale cluster simulations.  In Figure
\ref{fig:lowres} we plot the relative accretion rates onto the primary and
secondary for hot and cold simulations, where we have parameterised the
resolution in terms of the ratio of the SPH smoothing length to pressure scale
length at the edge of the circumsecondary disc.  The lowest resolution
simulations contain only a few hundred particles in the circumsecondary disc.
We include error bars on each simulation to show the range of variation in
$\Gamma$ in the steady-state.

\begin{figure}
  \begin{center}
	 \includegraphics[width=0.5\textwidth]{Figures/Gamma_resolution.pdf}
  \end{center}
  \caption{Average $\Gamma$ for hot (green triangles) and cold (blue circles) simulations,
  averaged over the final 20 binary orbits, for a range of resolutions.  The
  error bars show the variation in $\Gamma$ (1 standard deviation) over the
  same period.
  Resolution is reported as $h/H$ (SPH smoothing length to disc scale height)
  at the edge of the circumsecondary disc.  The dashed line shows the
  $\Gamma$ for purely ballistic particles \citep{BateBallistic}.}
  \label{fig:lowres}
\end{figure}

We find that provided $h/H<1$ at the edge of the secondary's disc, the
differential accretion pattern is only modestly affected.  For the cold
simulations, the effect of under-resolving the accretion flow is to
over-estimate accretion onto the primary.  The magnitude of this
over-estimation remains less than $5\%$ so long as $h/H<1$, but once $h/H > 1$
$\Gamma$ rapidly transitions to the value found for the
accretion of purely ballistic particles \citep{BateBallistic}.
The hot simulations are subject to larger temporal variability in $\Gamma$
(see Figure \ref{fig:conv_accretion_hard} and error bars in Figure
\ref{fig:lowres}), but the average $\Gamma$ still only changes by roughly $10\%$
when $h/H<1$.  There is also some evidence for a step change in
$\Gamma$ similar to the cold simulations when $h/H$ exceeds $1$.
We caution that the fact that the well
resolved hot simulation have $\Gamma$ similar to that of ballistic simulations
makes detecting changes in $\Gamma$ at low resolution potentially difficult
to detect.

We thus conclude that poor resolution in cluster scale simulations (where the
normalised sound speeds tend to be close to our cold case) is unlikely
to severely compromise the mass ratio of binaries formed in such simulations.

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

Our isothermal simulations  have demonstrated the critical role played by
the normalised sound speed in determining the relative accretion rates
on to the primary and secondary. In real (non-isothermal) discs we would
expect that it is the gas temperature in the vicinity of the Roche lobes that
most critically affects the accretion pattern (since it is here that we have seen
the decisive role of pressure gradients in affecting the
flow morophology).
This allows us to make some crude estimates of the values of normalised
sound speed to be expected in astrophysical systems.

In the case of proto-binaries, a 1 A.U. binary with primary mass in the regime
typical for T Tauri stars will have orbital velocity $\sim 30$ km s$^{-1}$.
For a typical disc, heated mainly by irradiation from the central star
\citep{TTTemp1,TTTemp2},
we expect $T \sim 100$K for gas on an A.U. scale.  These typical numbers yield
$c \sim 0.02$.  Since the
temperature of a disc heated by irradiation scales as $R^{-1/2}$, the sound
speed at the relevant distance ($a$) scales as $a^{-1/4}$.  By contrast, the
orbital velocity of the binary scales as $a^{-1/2}$.  Thus the normalised
sound speed scales as $a^{1/4}$.  Eventually (at $\approx 100$ A.U.), the
temperature attains a `floor' value of order $10$K and the normalised sound
speed rises more steeply with binary separation ($\propto a^{0.5}$).
\footnote{For example, modeling
of the Class I  binary L1551 NE, imaged by ALMA, suggests $c \sim 0.1$
for this wide ($\sim 300$ A.U.) binary.\citep{ALMA_binary_obs}}

Taken together this suggests
that $c$ lies in the range of $\sim 0.01-0.1$ for proto-binaries
of roughly solar mass. These values would be a factor of a few larger
or smaller for earlier or later type pre-main sequence stars.
We thus conclude that $c$ values similar to our cold simulation
are characteristic of young binaries although higher values are possible
in higher mass, wide systems and/or where heating by accretion significantly
boosts the gas temperature.

 In the case of supermassive black hole binaries, the aspect ratio of
the disc (which is similar to the normalised sound speed in the vicinity
of the binary) is a very weak function of system parameters
and is of order $0.01$ \citep{BHTemp}. Thus the cold regime is the relevant
one in this case also.

\section{Conclusion}
\label{sec:conclusion}

 We have investigated the quantitative and qualitative discrepancies
previously reported in the literature between SPH and grid based
studies of accretion onto proto-binaries. Our results are broadly
in line with results in the literature obtained by both methods and
demonstrate that the differences reported are in fact due to the different
gas temperatures previously used in SPH and grid based calculations.
The fact that (for a given temperature) our (2D SPH) calculations agree with
previous 3D SPH calculations and 2D grid based calculations
implies that neither the dimensionality of the simulation nor
the numerical technique are critical in determining the modes of accretion
onto binaries.

 We find that as the ratio of the sound speed in the accreting gas
to the orbital speed of the binary is increased (i.e., the temperature is
increased), there is an increasingly
dominant flow between the secondary and primary Roche lobes. In our
cold and hot simulations (where this ratio is respectively $0.05$ and
$0.25$ ) the fraction of particles ultimately
accreted by the primary that have previously spent time in the
secondary's Roche lobe changes from $6 \%$ to $65 \%$.  The existence
of this cross Roche lobe flow accounts
for the slower increase of $q$ in the hotter simulations.

 It would be premature to lay out the implications for protobinary
evolution from this pilot study at a single value of $q$. We have
however demonstrated that it is possible to obtain numerically converged
quasi-steady flow solutions where the role of numerical dissipation
in the critical region around the binary Roche lobes is
demonstrably small away from shocks. We emphasise that
that
 quantitative statements should not be based on the initial transient
stage of the simulation. We have found that a quasi-steady state
is only attained after $\sim 30$ binary orbits and we base our
accretion rates on long timescale averaging once this initial
phase is concluded.

Finally, we have explored the effect of very poor resolution.  We find that
provided the ratio of the resolution length to the pressure scale height at
the edge of the secondary's disc ($h/H$) remains below 1, the relative accretion
rates are only mildly compromised.  Our results suggest that even in the poorly
resolved regime expected in cluster scale simulations, the evolution of binary
mass ratios should be captured correctly.

\section{Materials \& Methods}
\label{sec:methods}

In the interests of reproducibility and transparency, all the code needed to
reproduce this work has been made freely available online at
\url{https://bitbucket.org/constantAmateur/binaryaccretion}.  See the readme
file in this repository for further details.

All figures in this paper were generated using the python package
{\sc matplotilb} \citep{MPL}.

\section{Acknowledgements}
\label{sec:ack}

Matthew Young gratefully acknowledges the support of a
Poynton Cambridge Australia Scholarship.  This work has been
supported by the DISCSIM project, grant agreement 341137 funded by
the European Research Council under ERC-2013-ADG.

We are indebted to Eduardo Delgado-Donate who was working on this problem
at the time of his untimely death in 2007.

We thank the referee for comments that improved the clarity of the paper.

\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


text:
Archibracon is een geslacht van insecten uit de orde vliesvleugeligen (Hymenoptera) en de familie schildwespen (Braconidae).

Soorten
A. aterrimus (Enderlein, 1920)
A. atricauda (Enderlein, 1920)
A. capensis (Cameron, 1905)
A. curticornis Quicke, 1989
A. deliberator (Szepligeti, 1905)
A. dimaensis (Cameron, 1912)
A. dubius (Bingham, 1902)
A. elizabethae (Cameron, 1906)
A. fasciatus (Szepligeti, 1914)
A. fenestralis (Szepligeti, 1911)
A. flaviceps (Brulle, 1846)
A. flavimanus (Szepligeti, 1913)
A. flavofasciatus (Cameron, 1906)
A. fulvipes (Szepligeti, 1913)
A. grangeri Quicke, 1989
A. gutta (Enderlein, 1920)
A. luteoflagellaris Quicke, 1989
A. nigricephalus Quicke, 1989
A. pulchricornis (Szepligeti, 1914)
A. ruficeps (Szepligeti, 1914)
A. servillei (Brulle, 1846)
A. sigwalti Quicke, 1989
A. silvestrii (Szepligeti, 1913)
A. spilopterus (Cameron, 1905)
A. szepligetii Brues, 1926
A. voeltzkowi (Szepligeti, 1913)
A. xanthocephalus (Szepligeti, 1914)
A. zonatipennis Fahringer, 1931

redpajama_set_name: RedPajamaWikipedia


text:
Worldwide car sales 2010-2021
Number of cars sold in the U.S. 1951-2019
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Electric vehicles in use worldwide
Gas prices in the United States 1990-2019
Automotive industry worldwide - statistics & facts
Motorcycle Industry in the United States - statistics & facts
Transportation & Logistics›
River cruise calls of Port of Amsterdam in the Netherlands 2009-2019
Published by I. Wagner, Oct 28, 2020
Between the period of 2009 to 2018, the number of river cruise arrivals increased steadily. In 2009, 999 rive cruises were counted arriving in the Port of Amsterdam, whereas by 2018 this increased to just over 2,000 calls. However, in 2019 the number of arrivals decreased slightly and approximately 1,900 river cruises were registered at the passenger terminal in the capital city of the Netherlands.
Number of river cruise calls of Port of Amsterdam in the Netherlands from 2009 to 2019
Number of river cruise calls
The figures have been taken from several publications.
Cruise industry Netherlands
Number of global ocean cruise passengers 2009-2019
European cruise passenger volume 2018, by source country
Top 20 travel agencies in the Netherlands 2018, by revenue
Leading cruise destinations from the Netherlands 2016-2018, by passenger number
I. Wagner
Research Lead covering road traffic and motor vehicle manufacturing
Statistics on "Cruise industry in the Netherlands"
GDP contribution of tourism industry in the Netherlands 2016-2018
Distribution of added value in the tourism industry in the Netherlands, by sector
Number of cruise passengers from the Netherlands 2012-2018
Volume of cruise passengers from the Netherlands 2018, by age group
Number of cruise passengers from the Netherlands 2018, by length of cruise
Average length of cruise taken by passengers from the Netherlands 2016-2018
Cruise calls of Port of Amsterdam in the Netherlands 2016-2019
Sea cruise calls of Port of Amsterdam in the Netherlands 2009-2019
Number of sea cruise passengers in Amsterdam (Netherlands) 2009-2019
Number of river cruise passengers in Amsterdam (Netherlands) 2009-2018
Number of river cruise calls at ports Amsterdam region (Netherlands) 2018
Sea cruise calls of Port of IJmuiden in the Netherlands 2015-2019
Number of sea cruise passengers in IJmuiden (Netherlands) 2014-2018
River cruise calls of Zaanstad in the Netherlands 2015-2019
Number of cruise visitors to Aruba 2008-2019
Volume cruise ship arrivals in Curaçao 2009-2019
Number of cruise arrivals in Curaçao 2009-2019
Number of cruise passengers arriving to Bonaire 2012-2019
Revenues from sea and river cruises in Germany 2000-2016
Number of river cruise ships worldwide 2014, by region
Annual growth in inbound visitor arrivals in Hong Kong 2008-2019
Inbound tourists from Africa Philippines 2010-2019
Cruise passenger arrivals Chile 2003-2019
Number of visitors to Byron, Australia 2013-2014
Cruise passenger arrivals in Canada, by purpose 2003-2016
Value added by the cruise industry in New Zealand 2014-2018
Direct expenditure of cruise industry in New Zealand 2014-2018
Value added by the cruise industry New Zealand 2015/2016 by region
Number of unique cruise passengers in New Zealand 2014-2018
Number of cruise passenger arrivals New Zealand in 2015/16 by country of origin
Number of voyages during the cruise season in New Zealand 2014-2018
Expenditures shopping services in inbound tourism Philippines 2012-2018
Number of immigrants arrived by sea in Europe 2020, by country of first arrival
Hotel guests from America in the Netherlands Q2 2020, by region
Impact of tourism on jobs in Poland 2018
Average flight delay time at selected airports in the United Kingdom (UK) 2014-2019
Cruise industry Netherlands Cruise industry Cruise industry in Europe
Port of Amsterdam. (April 24, 2020). Number of river cruise calls of Port of Amsterdam in the Netherlands from 2009 to 2019 [Graph]. In Statista. Retrieved January 20, 2021, from https://www.statista.com/statistics/1117055/river-cruise-calls-of-port-of-amsterdam-in-the-netherlands/
Port of Amsterdam. "Number of river cruise calls of Port of Amsterdam in the Netherlands from 2009 to 2019." Chart. April 24, 2020. Statista. Accessed January 20, 2021. https://www.statista.com/statistics/1117055/river-cruise-calls-of-port-of-amsterdam-in-the-netherlands/
Port of Amsterdam. (2020). Number of river cruise calls of Port of Amsterdam in the Netherlands from 2009 to 2019. Statista. Statista Inc.. Accessed: January 20, 2021. https://www.statista.com/statistics/1117055/river-cruise-calls-of-port-of-amsterdam-in-the-netherlands/
Port of Amsterdam. "Number of River Cruise Calls of Port of Amsterdam in The Netherlands from 2009 to 2019." Statista, Statista Inc., 24 Apr 2020, https://www.statista.com/statistics/1117055/river-cruise-calls-of-port-of-amsterdam-in-the-netherlands/
Port of Amsterdam, Number of river cruise calls of Port of Amsterdam in the Netherlands from 2009 to 2019 Statista, https://www.statista.com/statistics/1117055/river-cruise-calls-of-port-of-amsterdam-in-the-netherlands/ (last visited January 20, 2021)


Cast your vote for the top play of week 8 of the football season here.
Week 8 featured great plays from all around the county.
Voting closes Wednesday evening, with the winner announced Thursday. In the future: Please send us any and all video highlights we may not have captured or received to sports@columbian.com.
Union's Daron Ulrich 56-yard interception return for touchdown in rout of Battle Ground.
Luc Sturbelle, a Camas receiver, gets crucial first down on 3rd and 5 with 2:37 left in the fourth quarter. The Papermakers would score on the next play and hold on to beat Skyview.
Union's Alishawuan Taylor, a receiver, lines up as QB and rushes for a 31-yard touchdown.
Columbia River's Dawson Lieurance hurdles Woodland defender on a scramble. The play — an illegal move — was called back, which is lame in our book. Don't try this at home, kids.
Washougal's Brevan Bea takes screen pass 70 yards for a touchdown against Hockinson.


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On 6 June 1944 Britain woke up to a profound silence. Overnight, 160,000 Allied troops had vanished and an eerie emptiness settled over the country. The majority of those men would never return. This is the story of that extraordinary 24 hours.Using a wealth of first person testimonies, renowned historian Max Arthur recounts a remarkable new oral history of D-Day, beginning with the two years leading up to the silent day which saw the UK transformed by the arrival of thousands of American and Canadian troops. We also hear the views of the American troops, who quickly formed strong views of both the British military and civilian populations. Then, on that June morning, many Britain people woke up to discover that vast areas of the country, which had throbbed with life only the day before, were now empty and silent. Civilian workers found coffee pots still warm on the stove but not a soul to greet them. Many women - and children - felt bewildered and betrayed.Then, throughout that day and the days that followed, the whole population gathered around wireless sets, waiting for news. There are powerful testimonies from families of who lost loved ones on the beaches of Normandy, and dramatic personal accounts from young widows who had never had the chance to say goodbye.THE SILENT DAY is an original and evocative portrait of a key event in world history, and a poignant reminder of the human cost of D-Day.
Most of us know a bit about what passes for good manners - holding doors open, sending thank-you notes, no elbows on the table. We certainly know bad manners when we see them. But where has this patchwork of beliefs and behaviours come from? How did manners develop? How do they change? And why do they matter so much to us? In examining our manners, Henry Hitchings delves into the English character and investigates our notions of Englishness.Sorry! presents an amusing, illuminating and quirky audit of English manners. From basic table manners to appropriate sexual conduct, via hospitality, chivalry, faux pas and online etiquette, Hitchings traces the history of our country's customs and courtesies. Putting under the microscope some of our most astute observers of humanity, including Jane Austen and Samuel Pepys, he uses their lives and writings to pry open the often downright peculiar secrets of the English character. Hitchings' blend of history, anthropology and personal journey helps us understand our bizarre and contested cultural baggage - and ourselves.
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text:
import java.util.HashSet;
import java.util.LinkedList;
import java.util.Queue;
import java.util.Set;

public class branching extends graphPlacement{
	double shouldBeAwayDistance;

	public branching(){
		super();
		shouldBeAwayDistance = Double.valueOf(cfg.get("shouldBeAwayDistance"));
	}

	public void graphCreate() {
		Queue<visualNode> openQueue = new LinkedList<visualNode>();
		Set<visualNode> closedList = new HashSet<visualNode>();
		visualNode currentNode = null;
		// HardCoded stuff here
		double maxX=0, maxY=0, minX=heightAndWidth/2, minY=heightAndWidth/2;

		visualNodes.clear();
		visualEdges.clear();

		heightAndWidth = 800;

		for (String name: graph.graph.keySet()){
			currentNode = new visualNode();
			currentNode.actualNode = graph.graph.get(name);
			visualNodes.put(graph.graph.get(name), currentNode);

	        if (currentNode.actualNode.h == 0.0) {
	        	currentNode.x = heightAndWidth/2;
	        	currentNode.y = heightAndWidth/2;
	        	openQueue.add(currentNode);
	        	minX = currentNode.x; // This is wrong.
	        	minY = currentNode.y;
	        //} else if (rand.nextInt(100) + 1 <= 35){
	        //	currentNode.nodeNumberId = rand.nextInt(currentNode.nodeCount) + 1;
	        //	closedList.add(currentNode);
	        }
	        for (Node neighbor: graph.graph.get(name).costs.keySet()){

	        	visualEdge edge = new visualEdge();
	        	edge.node1 = graph.graph.get(name);
	        	edge.node2 = neighbor;

	        	visualEdge edgeAlt = new visualEdge();
	        	edgeAlt.node1 = neighbor;
	        	edgeAlt.node2 = graph.graph.get(name);

	        	if (!visualEdges.contains(edge) && !visualEdges.contains(edgeAlt) ) {
	        		visualEdges.add(edge);
	        	}
	        }
		}

		while (!openQueue.isEmpty()) {
			currentNode = openQueue.poll();
			closedList.add(currentNode);
			if (currentNode.x > maxX){
				maxX = currentNode.x;
			}
			if (currentNode.y > maxY){
				maxY = currentNode.y;
			}
			if (currentNode.x < minX){
				minX = currentNode.x;
			}
			if (currentNode.y < minY){
				minY = currentNode.y;
			}
			double firstDeg = 0;
			double divisions = currentNode.actualNode.costs.size()+1;
			for (Node neighbor: currentNode.actualNode.costs.keySet()){
				double wideX=Double.valueOf(cfg.get("branchingWideX"));
				double wideY=Double.valueOf(cfg.get("branchingWideY"));
				firstDeg +=1;
			    visualNode currentNeighbor = visualNodes.get(neighbor);

			    if (closedList.contains(currentNeighbor)) continue;
			    //if (firstDeg/divisions == startDeg) continue;
			    boolean positionedProperly = false;

			    while (!positionedProperly){
			    	positionedProperly = true;
				    currentNeighbor.calcX(wideX, currentNode.x, firstDeg/divisions);
				    currentNeighbor.calcY(wideY, currentNode.y, firstDeg/divisions);
				    for (visualNode otherNode: closedList){

				    	double d = Math.sqrt(Math.pow(otherNode.x - currentNeighbor.x, 2)+Math.pow(otherNode.y - currentNeighbor.y, 2));
				    	//System.out.println(currentNeighbor.actualNode.label + ":"+ otherNode.actualNode.label);
				    	//System.out.println("X"+currentNeighbor.x + ":"+ otherNode.x);
				    	//System.out.println("Y"+currentNeighbor.y + ":"+ otherNode.y);
				    	//System.out.println(d);
				    	if (d < shouldBeAwayDistance){
				    		positionedProperly = false;
				    		break;
				    	}

				    }
				    wideX += 50;
				    wideY += 50;

				}

			    if (!closedList.contains(currentNeighbor)) {
				    openQueue.add(currentNeighbor);
			    }

			}
		}

		double polX = (minX >= 0 ? 0 : -minX);
		double polY = (minY >= 0 ? 0 : -minY);;
		// I think i might have this two confused
		imageHeight = 2 * (int)(maxX);
		imageWidth = 2 * (int)(maxY);
		//System.out.println("H"+imageHeight+"W"+imageWidth);
		polX = Math.abs((minX+(maxX-minX)/2)-(heightAndWidth/2));
		polY = Math.abs((minY+(maxY-minY)/2)-(heightAndWidth/2));

		//System.out.println("IX:"+imageHeight+"IY:"+imageWidth);
		//System.out.println("PX:"+polX+"PY:"+polY);

		for (Node n : visualNodes.keySet()) {
			visualNode s = visualNodes.get(n);
			//System.out.println("BPX:"+s.x+"BPY:"+s.y);
			if (s.x > heightAndWidth/2){
				s.x -= polX;
			} else {
				s.x += polX;
			}
			if (s.y > heightAndWidth/2){
				s.y -= polY;
			} else {
				s.y += polY;
			}

			//System.out.println("APX:"+s.x+"APY:"+s.y);
	    }

	}

}

redpajama_set_name: RedPajamaGithub


The frame of the goggle is equipped with a ventilation system, increasing air circulation and comfort, high quality, Firm and Durable. Freely adjust the length of elastic strap to fit your head size and suitable for different people. What's more, it can be used with helmet. With Super Toughness. It will not be cracked and broken during the intense movement. Good protection for your eyes.
High Material- Goggle Frame: ABS Plastic; Lens: UV400 Protection CE. The goggle has excellent anti-corrosion, scratch-resistant, shockproof and resist dust and liquid splash.
Unique Design- High density sponge in goggle frame has great exhaust ventilation for comfortably wearing. Streamline Design Can Reduce Wind Resistance to achieve a Good Windproof Effect.
Great Value- UV Protection that filters out 100% UVA/UVB/UVC & harmful blue light, The lens coating reduce dazzle light and tuned light transmission to protect your eyes.
Easy To Fit- Easy to put on and take off by adjusting the non-slip and high elastic strap to fit most person's head.
Variety Usages- Can be used as Motorcycle Goggles, Skiing Goggles, Sport Glasses, Sunglasses etc. You can also wear it to protect your eyes during the playing games.


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AARON MERREIGHN of Riverton, who ran for lieutenant governor last year under the Conservative Party banner, says he'll run as a Republican next year for state representative in the 87th House District, now represented by Rep. TIM BUTLER, R-Springfield.
Merreighn said he "left the Republican Party last year" when he became running mate to then-state Sen. SAM McCANN. Their ticket got 4.2 percent of the statewide vote in November.
Merreighn ran as a Democrat for precinct committeeman in 2014 and was listed on a Libertarian Party of Illinois news release when he ran for Riverton village trustee in 2015. He was not elected in either race.
If he loses maybe he'll run on the Green Party's ticket.
And, yes, it's a thing.
Cut him some slack. He's tryin every way he knows how.
If he even gets on the ballot, Butler will destroy him. Tim works his district very hard and is an experienced campaigner.
What's next? Is he going to ruin someone's Black Panther Party?
The party switching concerns me. On the other hand- I'm in this district and I've never met Mr. Butler. He's never responded to any concerns I've sent to him. I'm pretty sure he could care less about those concerns since I'm a state employee. So I'll at least check this guy out. I think every race should be contested in order to elect the best person possible.
If he keeps it up, he might accidently run against himself.
He could simply create his own party and call it the Sybil Party. It suits him.
Thumbs up on this comment!
He's running out of political parties. Crash will be crashing quinceaneras and bar mitzvahs pretty soon.
This has to be in the running for best comment of the year.
I can't get upset on his bailing on the IL GOP last year; it was actually the Raunerite party. If he were to not stay around now and help rebuild the IL GOP … then I could get upset.
In a world without Rauner, will Butler get a run for his money (Doesn't have much) since the cash is gonna dry up?
Never heard of the Veterans Party. He is all over the political map, pick a party already.
He'll be the best fundraiser Tim Butler can find.
He'll have the last laugh when he gets that full set of steak knives.