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Home Knicks Beat Up On Lakers Early, Withstand Late Lakers Run in MSG
Knicks Beat Up On Lakers Early, Withstand Late Lakers Run in MSG
Lakers Rumors & News Recap: All Stars? The Lakers Got 'Em
Daniel Buerge
The Lakers visited New York for the first time of the season on Thursday night, and it would be their only visit to Madison Square Garden during the regular season. They found themselves up against the surprisingly upstart New York Knicks, who were 16-5 entering the game. L.A., on the other hand, has been in a season-long slump and were looking to end a three-game losing streak.
After the team fell to the lowly Cleveland Cavaliers on Tuesday night, they had their hands full on Thursday. It was also Mike D'Antoni's first game against the team he coached a season ago. New Knicks coach Mike Woodson, who took over for D'Antoni upon his resignation, has the Knicks playing exceptional basketball, and they're sitting near the top of the Eastern Conference. In order for the Lakers to get the win and end the losing streak, they would have to do it without Steve Nash or Pau Gasol, both of whom were still out with injuries. Oh, and the Knicks were undefeated at home (8-0) headed into the game.
The game started with a bang as both teams were red hot from the field. New York struck first with a Carmelo Anthony three-pointer, and it didn't stop the rest of the quarter. Anthony was unconscious early, making his first five field goal attempts, including three from three-point range. But, always a fan of the big stage, Kobe Bryant wasn't about to let Melo steal the spotlight. Bryant also got things going early on the offensive end, scoring eight early points in the first five minutes of the quarter.
First to 200 points wins tonight
— Mark Medina (@MedinaLakersNBA) December 14, 2012
Both teams were shooting well early, and it had the Madison Square Garden crowd abuzz. New York, who has been one of the best shooting teams so far this season, lived up to their reputation in the first period.
In news that will surprise … nobody, the Knicks are shooting 66.7 percent. BK
— Kamenetzky Brothers (@KamBrothers) December 14, 2012
From there things got ugly for the Lakers. Their defense was all sorts of dreadful, and the Knicks ran them out of the building in the second half of the quarter. Open jumpers and uncontested layups allowed New York to put up their highest scoring quarter of the season, and head into the second period with a 41-27 lead.
Things didn't get much better for the Lakers in the second quarter. A lack of offensive rotation led to poor defense on the other end and things simply looked pitiful for Los Angeles. Many of the problems we've seen so far this season that have plagued the Lakers (turnovers, fastbreak points, etc.) once again allowed the Knicks to get ahead of the Lakers early, and essentially never look back.
Nash is able to stand atill and shoot the ball. I don't understand how that makes him less able to play than any other Laker
— J. Doug Hatings (@basquiatball) December 14, 2012
The first half there were not many bright spots for the Lakers, especially on the offensive end. Other than 16 points from Howard and 13 from Bryant, no other Laker made much of an impact on that end. And even Bryant's 13 points came on 4-11 shooting. But the bigger problem was defense, as the Lakers gave up nearly 70 points in the first half. At the break the Knicks were blowing out Los Angeles 68-49.
Remember when we all thought that the Lakers would be good?
— Alex Kennedy (@AlexKennedyNBA) December 14, 2012
The Lakers never made things close in the third quarter, and other than a hard fall by Carmelo Anthony there wasn't much of anything that can be considered noteworthy. Instead of writing two hundred more words on how depressing it is to watch the Lakers, I'll just fill in some tweets and hope I don't ruin my computer with my tears.
Showtime 2.0… The worst sequel ever!
— Craig Kwasniewski (@CTKwasniewski) December 14, 2012
I bet Mike D'Antoni is wishing he were still coaching the Knicks.
— Suki (@TheRealSuki) December 14, 2012
Why is Kobe still in this game? He looks really banged up and it's all but over.
— Noam Schiller (@noamschiller) December 14, 2012
Anyways, at the end of the third quarter the game was still a blowout, with the Knicks leading the Lakers 93-80.
Even though the Lakers never made a run in the third quarter, they did finally show some life in the fourth. About midway through the period they were able to get the game within a manageable distance, mainly due to the play of Howard and Kobe. Those two players were the backbones for the team offensively, and allowed Los Angeles to pull within 10 points with just over six minutes left in the fourth.
They also got some help from Metta World Peace, who was their third highest scorer on the night.
3 Lakers with 20 or more points. Kobe (26 along with 9 reb 5 ast 4 threes). Metta (20 along with 3 threes and 5 boards). Dwight (20 w/6 reb)
— NBA Fantasy (@NBAFantasy) December 14, 2012
One of the reasons L.A. was able to get back into the game was the absence of Carmelo Anthony, who sat out the final quarter after injuring his ankle in the third quarter. It was evident that the Knicks missed him on the offensive end, which was one of the reasons the Lakers were able to crawl back into the game.
Kobe hit a fadeaway three-pointer from the corner to bring Los Angeles within seven, but that's as close as it was going to get. The next two times down the floor New York got a dunk from Tyson Chandler and a three-pointer from JR Smith to seal the deal. L.A. was able to make it somewhat interesting at the end, but ultimately they fell short once again.
The theme to this Lakers season seems to be – fall behind big early, climb back late, lose in the end. It was a trend they followed again on Thursday night, and resulted in a 116-107 loss.
March Madness: Luke Walton Believes 'East Coast Bias' Limited Pac-12 To 3 Teams In NCAA Tournament
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Monday Moaning – Put a shovel in it!
Use a mini watermelon for these festive trees. Cut crosswise into rounds. Slice each round into 8 wedges. Trim rind off bottom, leaving a 1/2 inch piece in the middle for the tree trunk. Score branches on wedges.
Oh what fun for the little grade ones! Just pipe blended whipped cream, icing sugar and cream cheese around the edges of a vanilla wafer. Pop a strawberry in the middle and pipe a pompom on top.
Now where did I put that BBQ cover?
The good news is, it's only -10C.
You know you've delivery-dialed Domino's Pizza one too many times when they send you a Christmas card! With coupons inside!
I finally found some Thrills. Got them cheap at the dollar store. The package says "It Still Tastes Like Soap." Good marketing! And soap never tasted so good!
and winter came with a vengeance!


Architecture, photography, design festivals, mappings, places and special spaces.
Fashion, graphic and interior design you can enjoy and shop in Barcelona.
Take this tour if you want to see architecture and sample Catalan taste at the same time.


In late January, I took a trip to Banff with Eden to get away from the city for a night. We spent a wonderful night and day away. During our timeout, I took the opportunity to test out my Sigma Art 35 1.4. Here are some of the shots from the trip.
Dessert in a cloud of dry ice.
Shot together on the trip back. Had an Amazing time with this lady.


sounds amazingly like the stranglers 'always the sun' for the first 30 seconds or so, and then stops...another mid-tempo track with some nice muted trumpet playing throughout. another one to miss if you're unhappy, 'cos it's about a weekend-only relationship. example lyrics: "Caroline whispers, every monday morning I wish that you'd come home"


Every Wednesday night a volunteer group called "The Movement Family" serves a family style meal for the homeless at the Buckley Garage on Common Street in Lawrence. In the last five weeks The Valley Patriot has put out a call on Facebook looking for local business in the community to help with food donations resulting in several businesses and individuals stepping forward. We want to thank Rick Comeau owner of 5 Dragons Martial Arts Academy in Salisbury and Haverhill, for donating a full dinner to the 20+ homeless people at the bus stop. Rich paid out of pocket for dinner from Pizza Factory in North Andover who threw in some free meals to help out themselves. We also want to thank Bob St Louis for donating dinner from Jocelyn's Mediterranean Restaurant & Lounge (who gave Bob a discount for his generosity) to feed 20+ people, Stachey's Pizza in North Andover, as well as Shannon Marie who pitched in and cooked food to help feed the homeless on another night. We are ALWAYS looking for restaurants and eateries to donate dinner for the homeless for Wednesday night's family dinner. Please email me if you know anyone interested and I will even come pick up the food and deliver it myself.
THERE'S AN ELECTION GOING ON SEPTEMBER 4th SO WAKE UP!
This year's state primaries will be held on September 4th, the day after Labor Day and some say that Secretary of State Bill Galvin scheduled it that way to keep voter turnout low. Low voter turnouts traditionally favor incumbents getting reelected and Galvin faces a real primary challenge this year from a left-wing radical who believes in open borders and allowing illegal aliens to vote. The Secretary of State is in charge of state elections, so no matter how much you may not like Galvin, here's hoping that he can get past Josh Zakim or we are in really big trouble.
With ten candidates running for the Democratic Party's nomination for congress, the winner of this primary on September 4th will most likely be elected in the November final election as the 3rd congressional district is very liberal and includes Lowell, Haverhill, and Lawrence.
Here are your candidates: Jeff Ballinger, Alexandra Chandler, Abhijit Das, Rufus Gifford, Leonard Golder, Dan Koh, Barbara L'Italien, Juana Matias, Bopha Malone, and Lori Trahan. Quite frankly there's not much difference between any of these candidates. They are all for abortion on demand up till birth, open borders, giving amnesty to illegal aliens, allowing illegals to vote, support higher taxes, more government spending, and are obsessed with race and gender division.
Of course, anyone who has been paying attention to the Democratic Party at the national level knows that most of the dems in power in Washington D.C. believe the exact same thing. But, just try asking them about it directly and you will hear a lot of distractions and poll tested political phrases that don't actually mean anything.
At least Juana Matias isn't lying to the voters about her ultimate political goals. So, if anyone from this crowd is going to end up the congressman from the 3rd district I'd prefer someone who is going to be honest about selling out Americans citizens and the American taxpayers rather than a phony who smiles and pretends they care about American citizens or are really fighting for "rights".
In Methuen and North Andover there's an open state rep. seat because incumbent Diana DiZoglio is running for state senate. Since this is a district dominated by Democrats, whoever wins the primary is surely to be the winner in November. Former Methuen City Councilor Lisa Ferry is facing off against first time candidate Christine Minicucci from North Andover. In a normal election cycle with a low turnout, this race should be Lisa Ferry's to lose. After all, the district was purposely carved up to give Methuen candidates a lock on this seat. Plus, State Rep. Diana DiZoglio is endorsing Ferry and working hard to help her get elected. But Minicucci has a lot of money and with the controversy surrounding the Methuen City Council Ferry is going to have to work harder to win this race than she normally would. Had she called for a full investigation of the police salaries (which she voted for) to show the public she had nothing to do with it, she would be back in the driver's seat. But, since she balked at doing that and with others now calling for an investigation this is anybody's race. In fact, as of right now I'm calling Minicucci the front runner.
REGISTRY OF DEEDS – The current Register of Deeds is former Lawrence State Rep. M. Paul Iannuccillo and he has a tough fight on primary day. The Register of Deeds is in charge of all property deeds in this part of Essex County. It's a six-year term and it's an important government position because the person who holds that job can affect the purchase or sale of real property. This year, Iannccillo faces two challengers in the primary; Alexcy Vega the City of Lawrence's current City Assessor and former Lawrence City Councilor Michael Fielding, who has the support of former Lawrence Mayor Willie Lantigua. With Iannuccillo having two opponents dividing up the votes of people planning on voting against him it puts him in the front-runner's seat… for now. The daily newspaper, however, seems to hate him and will be actively campaigning against him as they have published several negative "gotcha" stories, so there is a legitimate chance he could be unseated. This race will be largely ignored. Don't ignore it. Go on line and research all three candidates and make up your own mind when you vote in this race. But, whatever you do, make sure you vote in this race.
STATE SENATE BARRY FINEGOLD IS BAAAAACK (yawn).
Since State Senator Barbara L'Italien is leaving the senate to run for congress, that leaves her seat open. Enter the guy who used to have that seat; Barry Finegold. Come on, you guys remember Barry. I know it's hard to remember him sometimes because he's very low key and doesn't really do anything, but surely you remember he was Willie Lantigua's biggest champion at the state house. You also might remember the only thing he actually did accomplish as a legislator was "baby drop-off" whereby mothers who no longer want the responsibility for their children can just abandon the kid(s) at any fire station and just walk away with immunity, no questions asked. Challenging Barry in the September 4th primary is Lawrence Firefighter Mike Armano. Armano is a young and energetic candidate who is working hard and will take a lot of votes away from Finegold in Lawrence, especially among union voters. Joe Espinola is running as a Republican and is working the district hard and will be able to take votes away from Finegold in Dracut and among the blue-collar voters. He may even surprise some people in Lawrence. Finegold is the front runner here but with a low turnout anything can happen.
While many people are blaming the Methuen police for the budget mess, Methuen City Councilor Steve Saba said on "Looped in Live" with Tim Wood that the budget mess was caused by the prior city council and the current school committee. During his appearance, he said the prior council was "asleep" adding that they were just a "rubber stamp" and called for an investigation into their previous actions.
"The previous council and previous mayor… just watch the meetings. Everything was just being rubber stamped. They bragged about the fact that they had such short meetings," he said. Saba added that the school department budget shortfall was not the fault of the police, but the school committee.
It seems someone is whispering in Joyce's ear, using her to attack Jessica for political reasons and Joyce is simply falling for it. For the record, what Finocchiaro posted on Facebook was NOT inaccurate and did NOT misinform the voters. If Joyce had bothered to actually read the Facebook post she was publicly complaining about she would not have made a fool of herself and the city council that night.
For his part Steve Saba also took a cheap shot at Jessica, not only at the meeting but on Looped in Live with Tim Wood where he said social media was not helping and that "certain" posts on social media were causing problems. So much for transparency. Saba is wrong on this. The fact is, most voters are now getting their information on local politics from Facebook and other social media sites. If more elected officials utilized social media to INFORM the public about what's going on, Methuen voters might be more educated and might not be in this mess to begin with. I'm just hoping all these childish cheap shots at Jessica will stop and the council will spend every waking moment fixing the budget mess and doing the work the voters elected them to do.
So, last month Tim Wood from Loop Weekly asked me to come on his show "Looped in Live" to talk about local Methuen issues. Almost immediately after he announced on Facebook that I would be his guest, the Duggan-haters tried to kill my appearance by intimidating him into canceling me as a guest because, obviously I'm just evil! I have to give Wood credit though, he didn't buckle under the pressure and the show went on as planned. And it was a great discussion where we agreed on some things, disagreed on others, and were able to do so in a civil and mature way. It's great to have someone like Tim in the local news business who understands what friendly rivalry is all about and knows how to stand up to the insider bullies in politics. You should go to the Loop Weekly's video gallery on Facebook and check out Looped in Live. And while you are there make sure you patronize his advertisers, because they are the reason we have yet one more voice on the political scene who is completely independent and isn't afraid of the corrupt insiders who try to silence dissenting voices.
Two months ago, Lawrence Police Chief Roy Vasque appeared on the Paying Attention Podcast where he talked about (among other things) the need to reconstitute a K9 unit to help Lawrence Police fight crime. Within a few days of his appearance Mayor Dan Rivera and Chief Roy Vasque issued a press release announcing that the Lawrence Police Department will be re-establishing the Department's K-9 Unit.
"At the direction of Chief Roy Vasque, the Department applied for a grant on May 17th from the Stanton Foundation for the K-9 First Dog Program. Both Mayor Rivera and Chief Vasque are happy to announce that the Department was awarded the grant on May 29th. The $25,000 grant will cover the cost of purchasing a dog, training costs, kennel facilities at the officer/handler's home, retrofitting a cruiser for the exclusive use of the K-9 unit, and food and veterinary care for the first three years of K-9 ownership. The process of selecting the Police Officer who will be the dog's handler, as well as the selection of the dog will begin immediately. The Stanton Foundation K-9 First Dog Program supports the creation of new K-9 Units in cities and towns in Massachusetts. The Department will be applying for a similar grant to add a 2nd dog to the Unit in the very near future.
NECC CONCERT – Tickets are available for "Barbra & Frank: The Concert that Never Was," a musical tribute celebrating the works of Barbra Streisand and Frank Sinatra. The event, hosted by the Northern Essex Community College Foundation, Inc., will take place from 7 to 9 p.m. on Saturday, Sept. 29th, at the Collins Center for the Performing Arts, 100 Shawsheen Road, Andover.
The concert is open to the public. Tickets are $50 per person and are now on sale. For more information, or to reserve seats, please contact Lori Smerdon at lsmerdon@necc.mass.edu or at 978-556-3870. Tickets can also be purchased through MKTix.com.
FARMERS MARKETS – The Lawrence and Methuen Farmers Markets are officially open! From July 6 to October 27 on Wednesdays, Fridays, and Saturdays from 10am – 3pm, you can find fruits and vegetables, freshly caught fish, crafts from local artisans, musical performances, and so much more.
The GWL Wednesday Farmers Market opens on July 11. It's located in Lawrence on Campagnone (North) Common across from the Lawrence Senior Center, 155 Haverhill Street.
Holy Family Hospital's Methuen Farmers Market managed by Groundwork Lawrence starts on July 6. It's open every Friday at 254 Broadway in Methuen, conveniently located on Rt. 28 next to Methuen Federal Credit Union.
The GWL Saturday Farmers Market opens on July 7 and is located in Lawrence on Sullivan Park on Rt. 114, at the intersection of North Parish Road and Winthrop Avenue.
In an effort to meet the ever-growing demand of support services and dignified housing for older adults with dementia, Edgewood senior living community in North Andover has completed The Woodlands Inn, a $17 million, 4-building, 40- residence expansion that caters primarily to seniors with Alzheimer's and other forms of dementia. Three of the four buildings will serve residents with dementia while the other will cater to enhanced living, or residents who need some general assistance throughout the day.
Each building accommodates 10 residents and is designed to encourage greater interaction and socialization. This "small house model" sees private rooms surround a central common area that includes an open-hearth kitchen, dining area, living room and den with a natural stone fireplace. Here residents can participate in activities, play games, read, watch TV or simply catch up with friends and neighbors. Other amenities in each household include a spa and private courtyard, as well as dedicated health professionals and other staff – called innkeepers – on site at all hours to assist with meal preparation, laundry, housekeeping and other daily tasks. Last year, the Alzheimer's Association estimated that 5.5 million Americans were living with Alzheimer's, and that 1 in 10 people age 65 and older have the disease. In Massachusetts, approximately 120,000 people ages 65 and older had Alzheimer's in 2017, and by 2025 that figure is expected to increase by 25 percent to 150,000 people.
CLEAN RIVER PROJECT NEEDS YOUR HELP! Have you got a community service requirement you need to fill? Court ordered? High School and college service requirements for graduation? National Honor society? Human Resource day of service requirement with your office? Well, Clean River Project has just what you need to help you fill those hours!
Whatever the reason you do community service it can foster a sense of civic pride and give you hands-on experience and valuable insight into the trades while teaching important life skills needed to obtain gainful employment. It offers an opportunity to help others and you'll leave with the knowledge you improved someone's life or situation and make your community a little bit better. Go down to1022 Riverside Drive in Methuen. Do your required service hours in a friendly, informative atmosphere. You'll spend your time outdoors, cruising the Merrimack River and become part of an initiative that has been ongoing for 14 years now.
Call 978-590-9374 and talk to Rocky Morrison about how you can fill the terms of your service requirements and help keep this beautiful resource clean!


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Wild Boar were once widespread throughout the country, but became extinct in the wild some time during the 13th century. Hunting was responsible for their eventual demise. In more recent years, Wild Boar were increasingly imported from European stock to be farmed under license. It is these boar that are the ancestors of the wild population living in the Forest of Dean today, through a combination of escape and deliberate release. The Forest of Dean is not unique in being home to Wild Boar in Britain, nor was it the first place for them to repopulate, as Kent, Sussex and Dorset host marginally older populations, whilst further small populations have continued to emerge all around Britain.
The reintroduction of Wild Boar in the Forest of Dean has proven divisive amongst the residents and businesses of the forest. Perhaps it is this notoriety that has resulted in the Dean population becoming perhaps the most well known on a national level. Many welcome their return, recognising that although their presence isn't the result of a formal reintroduction strategy, the result is the same – a native species has returned to its former range, bringing with it a valuable contribution to the ecology and biodiversity of the forest. Conversely, many oppose the return of the boar, primarily citing damage and public safety concerns as their reasons. Interestingly, some of the most vocal contributors to both sides of the debate seem to have relatively little interest in wider aspects of natural history – the species seems to have the ability to inspire passion in people who are otherwise content to not notice the majority of the rest of the natural inhabitants of the forest.
The size of the population in the Dean has been hard to define, due to the characteristics of both the boars' behaviour and their habitat, though attempts are often made. The population has a high propensity to fluctuate as the rate of breeding is highly dependent on the harvest of food produced by the forest each year. The majority of young will be born in the spring, with a smaller peak in the autumn, but piglets have been observed in all months of the year. An individual sow will only tend to produce one litter a year. There's no doubt that Wild Boar provide a valuable service to the ecology of the forest, excavating and dispersing dormant seeds, aerating the forest floor, and increasing the biodiversity of the woods. Perhaps one of the main benefits they provide is reducing the bracken under-storey by feeding on rhizomes, allowing more light to reach the forest floor, thus promoting new growth of species unable to compete with the fast growing bracken. Whilst they don't damage the woodland in the same way that deer species can do, and although their breeding rates are naturally managed to a degree by food availability, there's certainly a possibility that if left unmanaged, a 'tipping point' could be reached, and an adverse effect could be experienced by other species in the forest (e.g flora, ground-nesting birds). Perhaps a more likely scenario is that before the population could reach such a stage, more boar would disperse from the forest on to agricultural land, where they would be equally comfortable, but where they would no doubt soon meet an untimely end. A lack of natural predation of the Wild Boar means that the Forestry Commission carry out a cull in an attempt to cap the population.
Evidence of the presence of Wild Boar is easy to find throughout virtually all areas of the forest. At certain times of the year, the forest floor will show signs of rooting by the boar, in search of food – perhaps the most obvious field sign. Wallows can be found all over the forest – regularly used to cool down and remove parasites, usually with a convenient tree nearby, which the animals will use to rub against. In addition to the tell-tale mud on the trunk, these trees will often exhibit territorial markings in the form of notches, carved in to their trunks by the tusks of male boar.
Wild Boar are largely nocturnal creatures. Much of the daytime will be spent in the cover of dense, young conifer plantations, or in the summer under the shade of a tree or nestled within tall bracken. Daytime excursions are more frequent when young boar are present, due to the constant demands for feeding and the need for the parent sows to keep well fed. Nocturnal by nature, it is at dawn or dusk that boar are most likely to be seen, when they will leave their cover in search of food amongst the deciduous woodland, foraging for acorns, chestnuts, bracken rhizomes, beech mast, invertebrates, even carrion. For such large mammals they possess an impressive ability to go unnoticed, but will often betray their presence by the sound of leaf litter being shovelled away as they dig the forest floor, or by the squeal of a wayward piglet, often quickly followed by an admonishing grunt from their mother.
The domesticated heritage of the Forest of Dean's Wild Boar is clear – they descend from farmed stocks. As such, the original boar would have been used to being fed in the daytime by their keepers, and would have had no inherent fear of man. Their behaviour in the wild did not necessarily correlate with the species blueprint. Over successive generations however, there has been a clear tendency towards reverting to their wilder characteristics, but certain individuals and groups have still demonstrated a tendency to quickly become tolerant of, or even welcoming of, human contact – something that is exploited by some photographers. Some of these boar have attracted much media coverage in the past. This has usually occurred as a result of irresponsible, but usually entirely innocent, encouragement from people. For better or for worse, what with the rise and fall of industrialisation of the Forest of Dean, and the subsequent growth and continuation of the tourism and leisure industry, the home of the Wild Boar has changed significantly since it last lived here. The people and the boar of the Forest of Dean are still learning to co-exist.
Wild Boar are social creatures, and tend to move about in transient matriarchal groups. Collectively known as sounders, a group of boar will typically consist of at least one sow and her offspring, but frequently a small group of sows will collaborate with parental duties, leading to impressively sized groups. Male boar are larger than the females, and have tusks that, once sufficiently mature, can grow large enough to become permanently visible, protruding from under the upper lip. Such individuals are rarely observed in the Dean, as their natural lifespan isn't normally fulfilled, but occasionally one may be privileged to meet such a beast! Males are much more solitary creatures, though they will socialise with other males at times outside of the breeding season, and are generally harder to find. Their rutting season often correlates with the timing of the Fallow Deer rut. At this time, male boar are much more territorial and aggressive. Their testosterone fuelled urge to mate is often evidenced by frothy spittle forming around the mouth, and the apparent loss of their otherwise inherent shyness – whilst it is possible to responsibly observe the boar of the Forest of Dean, a male boar in rut is best avoided!
Whilst there is no single location that can be guaranteed to produce sightings of Wild Boar with any degree of consistency, there are a number of steps that can be taken to increase the chances of seeing them. Look for areas of thick cover (dense, young conifer plantations are ideal) that border more open areas of mature deciduous woodland. Whilst it's not uncommon to see boar in areas of relatively high human traffic, it's best to seek areas further off the beaten track, where the boar are less likely to have been previously disturbed, and where more natural behaviour will generally be observed. Field-signs are well worth looking out for, but it's best to ignore all but the most fresh footprints, droppings and excavations. Dawn and dusk are ideal times to see Wild Boar, but regardless of the time, it's essential to remain as quiet and non-intrusive as possible.
A short film made for BBC Springwatch…
Springwatch 2013 Wild Boar from Ben Locke on Vimeo.
During a trip to the west coast of Scotland and its islands, I planned to try to see Basking Sharks. After the Whale Shark, the Basking Shark is the world's second largest fish. Colossal but gentle giants that grace our western shores in the warmer months. From May, they can ... Read more
Nightjars & their allies
The concept of having a 'favourite bird' is a strange one, but if pushed, I would have to say that the Nightjar, or any number of its allies around the world, is mine. We only have the one species of Nightjar in Britain (European Nightjar) but I've been lucky enough ... Read more

redpajama_set_name: RedPajamaCommonCrawl


Matthew J. Metzger is an asexual, transgender British author juggling books, an office job and a love of travel with the human need for sleep once in a while. He writes both adult and young adult books focusing on LGBT+ characters and their relationships, particularly those from the less salubrious areas in which he was dragged up over the years.
You can follow Matthew on Facebook and Twitter and also check out his website.
#amwriting today. Need to finish this series. Blergh.


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Here is something you might never have seen before! A clever combination of a scarf/snood and a hat! Why has no one ever thought of this! The perfect thing to wear on a cold and windy day – maybe even to go skiing! Nice and quick to knit, the Icicle Hood requires 2 balls of Purl Alpaca Fine yarn.
Tension: 20 sts and 29 rows to 10 cm square over Stocking Stitch using larger needles.
Please note, if using a different yarn, correct tension must be obtained to make sure Icicle fits properly.


Not all software, of course, and not all all the time. Software certainly has its good points as well; so much of what we take for granted today is like a science fiction fantasy from when I was growing up. A powerful computer in my pocket with maps of everything and the world's biggest encyclopedia available almost wherever I go? Yeah, that's a good thing. But still. It could be so much better.
So much of the software I use has aggravating features that just don't make any sense. Very often it seems like it was designed for people who see the world differently from me. A lot of it forces me into tradeoffs I don't want to have to make. I don't like the way most of it looks. Where's the beauty? And don't even get me started on the bugs!
Imagine software that values emotion, intuition, compassion, purpose, empowerment, fluidity, multiplicity, interconnectedness, sustainability, and social justice.
Contrast that with today's software, and you can see that we've only just started to explore what's possible.
Software embeds the perspectives of the teams who create it, and historically the software industry has been dominated by analytical people who focus on efficiency and haven't paid much attention to these other "softer" concerns. New software builds on the platforms, tools, languages, and processes that have already been created, so it leads to a self-reinforcing cycle.
Another way of looking at the change that's coming is to focus on diversity. Today, most software is created by relatively-homogeneous teams, mostly made up of cis techie white and Asian guys without disabilities. Software tends to work best for people similar to the creators, so at some level it's not too surprising how much software today embeds racial biases – and ignores best practices for accessibility and gender HCI. And once again, there's once again a self-reinforcing cycle: the tools, languages, and platforms we use to build software don't give a lot of help here.
The good news is that it's possible to do much better. While there's still a lot to learn about different ways of creating software, we know more than enough to get started — for example, see the reference pages on the Open Source Bridge wiki that Tammarrian Rogers and I put together for our talk there back in June. Even though today's platforms, tools, languages, and processes embed biases, by being conscious of them we can compensate for their limitations – while working on the next generation of infrastructure.
The way I think of it is that we've only explored a tiny fraction of the design space. There are other solutions out there that are better for everybody. There's a huge under-served market out there – which means there are huge opportunities for the companies and open-source projects that take the lead here.
So yes indeed, a change is coming to the software world. And a good thing too!


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text:
Ireland's Johnny Sexton named World Player of the Year
Joe Schmidt wins Coach of the Year as Ireland are named as Team of the Year for 2018
Sun, Nov 25, 2018, 22:11
Ireland captain Rory Best performs Johnny Sexton's acceptance speech for World Player of the Year after the Leinster and Ireland outhalf lost his voice to laryngitis. Video: World Rugby
Ireland's Johnny Sexton is interviewed before the World Rugby awards ceremony in Monte-Carlo. Photograph: Dan Sheridan/Inpho
Johnny Sexton has been crowned World Rugby Player of the Year on a night of sweeping success for Ireland.
Joe Schmidt scooped the coach of the year award, with Ireland named team of the year in a triple win for the 2018 Six Nations Grand Slam winners at the World Rugby Awards.
Schmidt has guided Ireland from eighth to second in the world rankings in five years at the Test helm. He has proved as measured as it has rapid, and has earned the taskmaster boss the coach of the year prize. The Kiwi native will release a statement on Monday, revealing whether or not he intends to extend his tenure beyond next year's World Cup.
British and Irish Lions outhalf Sexton has become the first northern hemisphere winner of World Rugby's top accolade since France's Thierry Dusautoir in 2011.
The 33-year-old is just the second Irishman to land the gong, following in the footsteps of former Ireland hooker Keith Wood, in 2001.
"It's been an incredible year for Irish rugby, to win everything we could, really," Sexton said at the ceremony in Monte-Carlo.
"It's been very special, and a few of us have ended up here tonight. There are areas we've definitely highlighted to improve, which will be important in World Cup year.
"Teams try to peak for World Cup years. People ask have we peaked too soon? Well we haven't peaked, so we're just getting better and hopefully we can continue to do that.
Conor Murray comes off the bench to help Munster to victory
Lydia Thompson hat-trick sees England down Ireland
Joe Schmidt bracing for 'tight game' against the USA
Congratulations to Johnny Sexton, who has won the World Rugby Men's 15s Player of the Year 2018 award in association with @Mastercard #WorldRugbyAwards pic.twitter.com/eYOWaKLJ0o
— World Rugby (@WorldRugby) November 25, 2018
"You have to improve ahead of the general curve. We know everyone else is going to get better.
"We'll be going into a lot of games now as favourites after what's happened this year, so that will be a challenge for us.
"We've got to deal with being favourites and I'm sure we can do that."
The Irish contingent at World Rugby awards in Monte-Carlo. Photograph: Dan Sheridan/Inpho
Sexton's stunning drop-goal on the 41st phase of the final play secured Ireland a 15-13 win over France in Paris, as Schmidt's men set the ball rolling on just their third-ever Grand Slam.
The linchpin playmaker also guided Leinster to the Pro14-Champions Cup double, before starring when Ireland toppled back-to-back world champions New Zealand 16-9 in Dublin earlier this month. However, despite losing only once in 20 starts for his province this year, the award is based solely on achievements in international rugby in the calendar year.
Sexton has won 12 and drawn one of his last 13 tests for Ireland and the Lions. His only defeat in an Ireland jersey in 2018 came when he was named on the bench for the first test against Australia in Brisbane. In all he started nine of Ireland's 10 wins this year, scoring 96 points.
The shortlist of five players (Sexton, the All Blacks pair of Barrett and Reiko Ioane, and the Springboks duo of Faf de Klerk and Malcolm Marx), was drawn up after members of the International Rugby Players submitted their nominations for their Player of the Year, which numbered several hundred, on foot of which supporters were asked to vote on social media.
A panel of eight - Maggie Alphonsi (ENG), Fabien Galthié (FRA) George Gregan (AUS), Richie McCaw (NZL), Brian O'Driscoll (IRE) Agustín Pichot (ARG), John Smit (RSA) and Clive Woodward (ENG) - then took all this into consideration before conducting a conference call this week to agree upon their choice.
Having landed 39 out of 50 kicks at goal for Ireland this year - for a ratio of 78 per cent - Sexton is only the sixth European winner of the award. Fellow nominee Beauden Barrett - who landed 34 out of 48 of his kicks in 2018 (71 per cent) - was aiming to become the first man to win three in a row. An All Blacks player had won the award in each of the previous six years.
South Africa's Aphiwe Dyantyi pipped Ireland's Jordan Larmour to the Breakthrough Player of the Year award.
France's Jessy Tremouliere is World Rugby Women's 15s Player of the Year, with New Zealand's Michaela Blyde claiming the Women's Sevens award.
Australia's Angus Gardner picked up the Referee Award, with Doddie Weir scooping the Award for Character.
Jamie Armstrong of charity The Clan was handed the Spirit of Rugby Award, while Stephen Moore and DJ Forbes both picked up the IRP Special Merit Award.
Barrett Beauden
Brian O Driscoll
Clive Woodward
Joe Schmidt
Johnny Sexton
Ringrose to start for Ireland against the USA
Fiji stun France with historic victory at the Stade de France
Depleted Ulster facing a difficult assignment
Liam Toland: Beirne's edge is ability to play the system or invent his own
Ireland cap rewarding month with comfortable victory over USA
Paul Boyle seals the deal as Connacht claim bonus in South Africa
Joe Schmidt will announce future plans early next week
This month's rugby fixtures The final two rounds of European action take centre stage ahead of the start of the Six Nations
Pro14 Table & Fixtures
A Conference
Leinster 10 10 0 0 364 137 7 47
Ulster 10 7 0 3 311 216 8 36
Glasgow 10 5 0 5 225 198 4 24
Cheetahs 8 4 0 4 234 181 5 21
Dragons 10 4 0 6 186 273 2 18
Zebre 10 2 0 8 180 286 2 14
Ospreys 10 1 0 9 126 281 5 9
B Conference
Edinburgh 10 7 0 3 289 166 6 34
Scarlets 10 7 0 3 226 182 3 31
Munster 10 6 0 4 227 203 6 30
Connacht 10 5 0 5 192 231 5 25
Cardiff Blues 10 5 0 5 202 208 4 24
Benetton Treviso 10 4 0 6 219 265 7 23
Southern Kings 8 1 0 7 135 289 2 6
European Champions Cup Pools
Knock-out rounds & Results
Pool 1 Fixtures & Results
Dublin Marathon 2019 - In Pictures
Ireland v New Zealand
4 Mystery of former Ryder Cup star Anthony Kim rumbles on
5 FAI to allow Limerick apply for licence to play in First Division
Here is your handy guide to sport on television this week
Monday – Sunday, January 13th – 19th


Following the first 50 years of history, the Tecniseco Ingenieros group is proud to see its Fisair brand grow. The manufacturer of air humidity control systems has grown in international presence and resources. As a result, and for synergistic reasons, it has unified under the name of its FISAIR brand. All the expert engineers in humidity control, who have been working for many years in the Spanish market, will now continue to cooperate with the entire international FISAIR network to give greater support to its air conditioning and industrial process customers around the world. We will celebrate these 50 years of history during the next edition of the C&R fair in Madrid from February 26 to March 1. We hope to see you there so that we can continue celebrating it together.


text:
\section{Introduction}
\label{sec:intro}

The detection of planets around young stars offers a direct way of testing theories of planet formation and migration. Observations of such planets remain difficult because of the strong stellar activity of their parent (T Tauri) stars, and the presence of an optically-thick disc, which can cause additional variabilities. In this context, the young ($\sim2~{\rm Myr}$) system CI Tau is of particular interest. Recently, \citet{johnskrull16} reported radial velocity detection of a short-period companion to the star. With a projected mass of $M_{\rm p}\sin I\simeq 8 M_{\rm J}$ and a period of 9 days, it represents a rare example of young hot Jupiters co-existing with protoplanetary discs. Moreover, the radial velocity data from \citet{johnskrull16} suggests a non-zero eccentricity for this object. Further measurements by \citet{flagg19} gave a planetary eccentricity of $0.25\pm0.16$, and a mass of $11.6\pm^{\tiny 2.9}_{\tiny 2.7}~M_{\rm J}$.
In addition \citet{biddle18} reported photometric variability of the star with a 9 day period, while also recovering a 6.6 day signal, presumably corresponding to the stellar rotation. The authors suggested that although the planetary companion is likely not transiting, it can still cause photometric variability by driving pulsed accretion of disc material onto the star. This is the scenario that we will examine in this paper.

The origin of the significant eccentricity of CI Tau b could be found in planet-disc interactions. A large body of hydrodynamical simulations have explored the possibility of eccentricity excitation of planets embedded discs \citep[see, e.g.,][]{papaloizou01,dlb06,rice08}. More recently, long-term simulations by \citet{rbctfm16} and \citet{ragusa18}, especially tailored for the CI Tau system, have found that the growth of planetary eccentricity is indeed possible, albeit on time-scales longer than what was previously suggested. On the theoretical side, it has long been argued that disc-planet interactions can result in a growth of eccentricity under the action of Lindblad resonances \citep{gt80,gs03,ol03,to16}. In particular, the linear analysis of \citet{to16} showed that Lindblad resonances can overcome the damping effect of corotation resonances and viscosity, and allow for the growth of eccentricity of both the disc and the planet. One important numerical result of planet-disc interactions that remains poorly understood is the fact that planets on circular orbits seem to only excite eccentricity in the disc when the planet-to-star mass ratio exceeds $\sim 0.003$ \citep[see, e.g.][]{kd06,regaly10,to17,muley19}.

The photometric variability observed by \citet{biddle18} can also find its origin in planet-disc interactions. The variability of mass accretion in the presence of a companion can strongly differs from that of a disc around a single star. In the case of circumbinary accretion, both numerical simulations \citep[e.g.,][]{mm08,dorazio13,ml16,mml17,mml19} and observations \citep[e.g.,][]{jensen07,muzerolle13,bary14,tofflemire17,biddle18} show that accretion is variable on time-scales comparable with the binary orbital period. One interesting finding is that while circular binaries (with mass ratio of order unity) lead to a pulsed accretion at 5 times the binary period $T_b$, eccentric binaries lead to pulsed accretion with a dominant period of $T_b$ \citep[][]{ml16,mml19}. Because observations suggest that the companion to CI Tau is on an eccentric orbit, it is necessary to address the issue of pulsed accretion driven by eccentric short-period planets. In this paper we explore, by mean of hydrodynamical simulations, the accretion of disc material onto a star in the presence of an eccentric planetary companion.

This paper is organized as follows: We detail the problem setup and numerical methods in Section \ref{sec:methods}, and introduce some necessary diagnostic tools in Section \ref{sec:diagnostic}. We present results relevant for CI Tau in Section \ref{sec:resq10}, and explore a larger parameter space in Section \ref{sec:resparam}. Finally we discuss the implications of our results and conclude in Section \ref{sec:summary}.

\section{Problem setup and numerical methods}
\label{sec:methods}

The problem of interest consists of a viscous hydrodynamics accretion disc around a star (mass $M_*$), which is also orbited by a short-period giant planet (mass $M_{\rm p}$). We denote $q$ the planet-to-star mass ratio, and $a_{\rm p}$, $\Omega_{\rm p}$, $T_{\rm p}$ and $e_{\rm p}$ the semi-major axis, Keplerian mean motion, orbital period and eccentricity of the planet, respectively. The disc radial extend goes from $r_{\mathrm{in}}$ to $r_{\mathrm{out}}$.

We assume that the disc is locally isothermal with a pressure scale height $H$, and a constant aspect ratio $h=H/r$. Our fiducial setup uses $h=0.05$. The relation between the vertically-integrated pressure $P$ and surface density $\Sigma$ is therefore $P=c_{\rm s}^2\Sigma$, where $c_{\rm s}=H\Omega_{\rm K}$ is the sound speed, and $\Omega_{\rm K}$ the Keplerian frequency. We parametrize the kinematics viscosity through  the $\alpha$-prescription, i.e., $\nu=\alpha c_{\rm s} H$; we use $\alpha=0.1$ throughout the paper.
The code units are chosen such that $G(M_*+M_{\rm p})=a_{\rm p}=\Omega_{\rm p}=1$. Unless mentioned otherwise, we set $r_{\mathrm{in}}/a_{\rm p}=0.65$ and $r_{\mathrm{out}}/a_{\rm p}=10$.

Our initial and boundary conditions are similar to those of \citet{mml17}. The initial disc surface density is initially set to be:
\begin{equation}
\Sigma(r)=\Sigma_0 \left(\frac{r}{a_{\rm p}} \right)^{-1/2}\left[1-\left(\frac{r_{\mathrm{in}}}{r}\right)^{1/2} \right] \exp\left[-\left(\frac{r}{r_{\mathrm{edge}}}\right)^{-2} \right].
\end{equation}
The exponential factor creates a cavity, speeding up the process of the cavity opening by the planet, and therefore allowing for a quicker relaxation. We chose $r_{\mathrm{edge}}=2a_{\rm p}$.

The initial radial fluid velocity is
\begin{equation}
u_{\rm r} = -\frac{3}{2} \frac{\nu}{r} \left[1-\left(\frac{r_{\mathrm{in}}}{r}\right)^{1/2} \right] ^{-1},
\end{equation}
while the azimuthal velocity is
\begin{equation}
u_\phi = r\, \Omega.
\end{equation}
The initial orbital frequency $\Omega$ is set by the balance between the pressure force and gravity, including the quadrupole force from the planet:
\begin{equation}
\Omega^2(r) = \Omega_{\rm K}^2 \left[1 + \frac{3}{4}\frac{q}{(1+q)^2}\left(1+\frac{3}{2}e_{\rm p}^2 \right)\left(\frac{r}{a_{\rm p}}\right)^{-2} \right] + \frac{1}{r\Sigma}\dd{P}{r}.
\end{equation}

At the inner edge, we use the same ``diode'' boundary condition as \citet{mml17}, which allows mass to leave the domain at the inner edge, but prevents it from re-entering. This is done by applying a zero-gradient condition ($\partial u_r/ \partial r=0$) on $u_r$ whenever it is negative, but a reflective condition on $u_r$ when it is positive. Zero-gradient conditions are imposed on $\Sigma$ and $u_\phi$. These boundary conditions mimic the loss of mass at the inner edge as the gas is accreted onto the star at the magnetospheric radius.

At the outer disc edge, we assume that mass is injected into the domain at a constant rate $\dot{M}_0$. We apply a wave-killing zone that extend from $(r_{\mathrm{out}}-1)$ to $r_{\mathrm{out}}$ \citep[see, e.g.,][]{dvb06}. In this zone, all fluid quantities (generically denoted by $X$) are relaxed towards their initial value $X_0$ via:
\begin{equation}
\dd{X}{t}=-\frac{X-X_0}{t_{\rm damp}}R(r).
\end{equation}
Here $t_{\rm damp}$ is a damping time-scale, which we take to be the orbital period at the outer edge, and $R$ is a quadratic function that increase from 0 at $(r_{\mathrm{out}}-1)$ to 1 at $r_{\mathrm{out}}$. In code units, we chose $\Sigma_0=1$, and therefore we have $\dot{M}_0=3\pi\alpha h^2$.

The simulations are carried out on a grid centred on the centre of mass of the star-planet system. The planet is kept on a fixed eccentric orbit with $a_{\rm p}=1$. A fluid element with coordinates $(r,\phi$) feels the total potential $\Phi$ given by
\begin{align}
\Phi(r,\phi) &= -\frac{GM_*}{\left[r^2+r_*^2-2rr_* \cos(\phi-\phi_*) \right]^{1/2}} \nonumber \\
&-\frac{GM_{\rm p}}{\left[r^2+r_p^2-2rr_p \cos(\phi-\phi_p)+\epsilon^2\right]^{1/2}} ,
\end{align}
where $(r_*,\phi_*)$ and $(r_p,\phi_p)$ are the coordinates of the star and planet, and $\epsilon$ is a smoothing length. We take $\epsilon=0.6 H$. The star and planet do not feel the potential from the disc, and we compute their positions at each timestep by solving Kepler's equation, following the method outlined in \citet{md99}.

Finally, we follow \citet{kley99} and allow mass to accrete onto the planet. At each time-step $\Delta t$, the gas density inside the Roche lobe of the planet (radius $=a_{\rm p}(q/3)^{1/3}$) is reduced by a factor $(1-0.5\Omega_{\rm p}\Delta t) $. Note that the ``accreted'' mass is not added to the mass of the planet, but simply removed from the domain. Finally, the mass of the planet is smoothly increased from 0 to $M_{\rm p}$ over the first $10T_{\rm p}$ of the simulation.

We use the {\sc pluto} code \citep{mignone12}, with a two-dimensional cylindrical grid. We use the \textit{hll} solver with a linear reconstruction method and a second-order Runge-Kutta time-integration scheme. Our fiducial grid has a resolution of $384\times 886$ in radius and azimuth, respectively. As we use a logarithmic grid in radius, this resolution ensures nearly square cells with a constant aspect ratio across the computation domain. Additional runs carried out at a higher resolution show no significant differences in accretion variabilities at the inner disc edge compared to the ones carried out at our fiducial resolution \cite[see][for more details on convergence tests for simulations with similar setup]{to17}.

\section{Diagnostic tools}
\label{sec:diagnostic}

\begin{figure}
    \begin{center}
    \includegraphics[scale=0.8]{ekr_mdot_q10.eps}
    \caption{Time evolution of the total radial kinetic energy of the disc (top panel, in units of the Keplerian energy at $r=1$) and accretion rate at the inner edge (bottom panel).}
    \label{fig:ekr_mdot_q10}
    \end{center}
\end{figure}

The goal of this paper is to determine the accretion variability at the inner edge of the disc in the presence of a massive planetary companion. It is important to insure that the disc has reached a quasi-steady state (independent of the initial conditions). To this end, we first need to insure viscous relaxation of the inner disc region. The viscous time-scale at radius $r$ is $t_\nu=(4/9)(r^2/\nu)$. Thus after a time $t$, the disc is viscously relaxed up to a radius $r_{\rm relax}$ given by
\begin{equation}
r_{\rm relax}(t)=\left(\frac{9}{4}\alpha h^2 \Omega_{\rm p} t \right)^{2/3}a_{\rm p}.
\end{equation}
With $\alpha=0.1$ and $h=0.05$, after $4000$ orbits, the disc is viscously relaxed up to $r\sim 6a_{\rm p}$, which is adequate for the purpose of this study.

Secondly, pulsed accretion onto the star is driven by eccentric motion. It is therefore important to insure that the disc's eccentricity has reached a quasi-steady state. The simulations of \citet{kd06} and \citet{to17} have shown that for mass ratios of $q \gtrsim 0.003$, the outer disc would develop a significant eccentricity, which will eventually saturate. A useful quantity to measure eccentricity growth and saturation is the radial kinetic energy:
\begin{equation}
K_r=\int_{r_{\mathrm{in}}}^{r_{\mathrm{out}}}\int_0^{2\pi}\frac{1}{2}\Sigma u_r^2 \mathrm{d}\phi r\mathrm{d} r.
\end{equation}

Figure \ref{fig:ekr_mdot_q10} shows an example of the time evolution of the radial kinetic energy $K_r$ and the accretion rate at the disc inner edge. The latter is computed from
\begin{equation}
\dot{M}(r,t)=-\int_0^{2\pi}r\Sigma u_r \mathrm{d}\phi.
\end{equation}
In practice we use a sampling of 20 measurements of the accretion rate per orbit of the planet. We see that after 4000 orbits, neither $K_r$ nor $\dot M$ show long-term variation, and the system has reached quasi-steady state. Of course, variabilities of $K_r$ and $\dot M$ on orbital timescales still exist, and we study these variabilities in the following sections.
Note that although the simulations have reached a quasi-steady state, the time-averaged accretion rate at the inner edge is not equal to the mass supply rate at the outer edge, $\dot{M}_0$. This is because some of the mass is ``accreted'' onto the planet and removed from the computational domain.

\section{Results for $\lowercase{q}=0.01$}
\label{sec:resq10}

\begin{figure*}
    \begin{center}
    \includegraphics[scale=0.8]{density_snapshots_q10.eps}
    \caption{Disc surface density (zoomed-in to the inner part of the disc) for a planet-to-star mass ratio of $q=0.01$ and two different planet eccentricities, $e_{\rm p}=0$ (left) and $e_{\rm p}=0.2$ (right). In the right panel, the planet is at the pericentre.}
    \label{fig:density_snaps}
    \end{center}
\end{figure*}

To illustrate the accretion onto the inner edge, we begin with a fiducial example with $q=0.01$, and varying the planet eccentricity. This setup is similar to the observed properties of the candidate planet around CI Tau. A snapshot of the disc surface density after several thousand orbits is shown in Figure \ref{fig:density_snaps}, where the planet is at pericentre, for two different planet eccentricities: $e_{\rm p}=0$ and $e_{\rm p}=0.2$. The main morphological difference is that the eccentric planet carves out a large eccentric cavity, which does not appear when the planet is on a circular orbit.

This feature appears even more clearly in Figure \ref{fig:esa_q10}, where we show azimuthally averaged profiles for the disc eccentricity, surface density, argument of pericentre and angular momentum deficit (AMD). These quantities were calculated using azimuthally averaged components of the eccentricity vector of each grid cells, following \citet{to17}. In the case where $e_{\rm p}=0$, the outer disc ($r>a_{\rm p}$) is not eccentric; the inner disc appears to have some residual eccentricity, but since it is depleted in material, its effect is negligible (as can be seen from the fact that the AMD is nearly zero everywhere in the disc). For higher planet eccentricities, the outer disc becomes clearly eccentric, and the cavity becomes larger. The outer part of the disc also precesses nearly-rigidly.

\begin{figure}
    \begin{center}
    \includegraphics[scale=0.45]{esa_q10.eps}
    \caption{Azimuthally averaged radial profiles for disc eccentricity, surface density, argument of pericentre, and angular momentum deficit for different planet eccentricities.}
    \label{fig:esa_q10}
    \end{center}
\end{figure}

The accretion rate at the inner edge, and the corresponding periodogram are shown in Figure \ref{fig:mdot_per_q10} for various planet eccentricities. As the planet eccentricity increases, the modulated accretion rate becomes more  pronounced, with a period that matches the planet's orbital period. This is confirmed when taking the Lomb-Scargle periodogram of the time-varying accretion rate. The periodogram clearly shows a main peak at the planet's orbital frequency. The amplitude of the accretion rate modulation increases with eccentricity for the range of eccentricities we consider, as shown in Figure \ref{fig:max_q10}.

\begin{figure*}
    \begin{center}
    \includegraphics[scale=0.8]{mdot_periodogram_q10.eps}
    \caption{\textit{Top:} Accretion rate at the inner disc radius over the last 10 planetary orbits of the simulations, for $q=0.01$ and different planetary eccentricities. For comparison, the grey dashed curved shows the radial position of the planet over time. \textit{Bottom:} the corresponding periodogram. The amplitudes of the periodograms are normalized so that the amplitude of the largest signal ($e_{\rm p}=0.2$) is 1, and all the other ones are scaled by the squared amplitude of the accretion rates. They are arbitrarily offset from each others for clarity.}
    \label{fig:mdot_per_q10}
    \end{center}
\end{figure*}

\begin{figure}
    \begin{center}
    \includegraphics[scale=0.8]{max_amplitude_q10.eps}
    \caption{Peak-to-trough amplitude of the accretion rate for different eccentricities of the planet. The corresponding accretion rate time series are shown in Figure \ref{fig:mdot_per_q10}.}
    \label{fig:max_q10}
    \end{center}
\end{figure}
In Figure \ref{fig:flow_q10e0} and \ref{fig:flow_q10e2} we show the accretion flow morphology for the circular and $e_{\rm p}=0.2$ cases, at different phases of the planet's orbital trajectory. The circular case exhibits a constant flow morphology at all phases, thus a flat accretion curve in Figure \ref{fig:mdot_per_q10}. However, when the planet is eccentric, the accretion rate clearly varies as the planet goes over its orbit. The two bottom panels of Figure \ref{fig:flow_q10e2} show the two episodes of maximum accretion observed in Figure \ref{fig:mdot_per_q10}: A first burst occurs when the planet enters a region of higher density and launches material inwards, closely followed by a second burst as the planet approaches the pericentre.

\begin{figure*}
    \begin{center}
    \includegraphics[scale=0.75]{velocity_snapshots_q10e0.eps}
    \caption{Streamlines overplotted on top of the surface density, for a planet-to-star mass ratio of $q=0.01$ and planet eccentricity $e_{\rm p}=0$. We show four different snapshots taken over a single orbit of the planet, at different orbital phases of the planet. The position of the planet is highlighted by the white circle. The planet is at pericentre at $\phi=0$, and at apocentre at $\phi=\pi$. The corresponding $\dot{M}$ at the inner disc edge is indicated on top of each panel. In this case, the planet on a circular orbit does not cause any time variation of the accretion rate at the inner disc edge.}
    \label{fig:flow_q10e0}
    \end{center}
\end{figure*}

\begin{figure*}
    \begin{center}
    \includegraphics[scale=0.75]{velocity_snapshots_q10e2.eps}
    \caption{Same as Figure \ref{fig:flow_q10e0}, but with a planetary eccentricity of $e_{\rm p}=0.2$. In this case, the morphology of the flow and the accretion rate at the disc inner edge vary over the planet's orbit.}
    \label{fig:flow_q10e2}
    \end{center}
\end{figure*}

From this set of simulations, the following picture emerges: when eccentric, the giant planet drives a pulsed accretion onto the star, with a period matching the orbital period of the planet; the amplitude of the pulsation depends on the eccentricity. It is worth pointing out that in several previous works, planets on fixed circular orbits with $q=0.01$ were able to excite eccentricity in the outer disc \citep[see][]{kd06,regaly10,to17,muley19}, a feature not observed in our simulations. This is likely caused by the high viscosity used in our simulations, which results in a strong eccentricity damping. Only when the planet is eccentric can it force some eccentricity in the disc and overcome viscous damping.

\section{Exploring the parameter space}
\label{sec:resparam}

\subsection{Planet mass}
Although our study was motivated by the photometric variability observed in CI Tau, it is useful to consider other planet masses. We therefore carry out simulations for planet-to-star mass ratios ranging from $q=0.001$ to $q=0.01$.

In Figure \ref{fig:mdot_per_qe2} we show the accretion rate evolution and periodogram for a planet with eccentricity $e_{\rm p}=0.2$ and various planet-to-star mass ratios. For $q=0.001$, the accretion rate at the inner disc edge does not exhibit significant variations compared to the larger mass ratio 	cases. Interestingly, for $q=0.002$, large-amplitude variability at twice the planet's orbital frequency appears. As the planet mass increases, the two pulses per orbit gradually merge, and pulsed accretion at the planet's orbital frequency occurs. To illustrate this further, we plot in Figure \ref{fig:max_qe2} the peak-to-trough amplitude of the accretion rate time series shown in Figure \ref{fig:mdot_per_qe2}, with additional data points to resolve the transition around $q=0.002$. We have also added a point for $q=0.008$, where the accretion rate variation amplitude has the largest amplitude of all our simulations. This is possibly because as the planet becomes too massive, it starts accreting more mass than it lets go through the boundary, hence reducing the accretion rate variation at the inner edge.

We have also run simulations (not shown here) with $e_{\rm p}=0$ for two additional mass ratios, $q=0.005$ and $q=0.001$. We find that the accretion rate is constant over time, without any large-amplitude modulations, similar to what is shown in Figure \ref{fig:mdot_per_q10} for the case of $q=0.01$ and $e_{\rm p}=0$.

\begin{figure*}
    \begin{center}
    \includegraphics[scale=0.8]{mdot_periodogram_qe2.eps}
    \caption{Same as Fig.~\ref{fig:mdot_per_q10}, but for $e_{\rm p}=0.2$ and different planet-to-star mass ratio (as indicated). In the top panel, the grey dashed curve (which indicates the radial position of the planet) is offset and in arbitrary units. All the curves are offset for clarity.}
    \label{fig:mdot_per_qe2}
    \end{center}
\end{figure*}

\begin{figure}
    \begin{center}
    \includegraphics[scale=0.8]{max_amplitude_qe2.eps}
    \caption{Peak-to-trough amplitude of the accretion rate for different planet-to-star mass ratios. The corresponding accretion rate time series are  shown in Figure \ref{fig:mdot_per_qe2}.}
    \label{fig:max_qe2}
    \end{center}
\end{figure}

\subsection{Separation between the planet's orbit and the disc's inner edge}
\label{sec:ap}
We now examine the effect of placing the planet further away from the inner edge. We consider the case of $q=0.004$ and $e_{\rm p}=0.2$. In addition to our fiducial run with $r_{\mathrm{in}}/a_{\rm p}=0.65$, we have carried out two simulations with $r_{\mathrm{in}}/a_{\rm p}=0.35$ and $r_{\mathrm{in}}/a_{\rm p}=0.5$. Figure \ref{fig:density_snaps_q4a} shows snapshots of the disc surface density after several thousand orbits for the three cases. Because of the high viscosity, the planet does not open a clear gap, and a lot of material is able to accrete onto the inner disc edge. The corresponding periodograms show a transition from pulsed accretion at the planet's orbital frequency (when the planet is close to the edge) to twice its orbital frequency (when the planet is far for the edge). Interestingly, the variation amplitude is smaller for $r_{\mathrm{in}}/a_{\rm p}=0.5$ than for $r_{\mathrm{in}}/a_{\rm p}=0.35$ and 0.65.

\begin{figure*}
    \begin{center}
    \includegraphics[scale=0.65]{density_snapshots_q4a.eps}
    \caption{Disc surface density snapshots for a planet-to-star mass ratio of $q=0.004$, planet eccentricity $e_{\rm p}=0.2$, and three different disc inner edge locations: $r_{\mathrm{in}}/a_{\rm p}=0.35$ (left), $r_{\mathrm{in}}/a_{\rm p}=0.5$ (centre), and $r_{\mathrm{in}}/a_{\rm p}=0.65$ (right).}
    \label{fig:density_snaps_q4a}
    \end{center}
\end{figure*}

\begin{figure*}
    \begin{center}
    \includegraphics[scale=0.8]{mdot_periodogram_q4a.eps}
    \caption{Same as Fig.~\ref{fig:mdot_per_q10}, except for $q=0.004$ and $e_{\rm p}=0.2$, with $r_{\mathrm{in}}/a_{\rm p}=0.35$ (blue), $r_{\mathrm{in}}/a_{\rm p}=0.5$ (orange), and $r_{\mathrm{in}}/a_{\rm p}=0.65$ (green).}
    \label{fig:mdot_per_q4a}
    \end{center}
\end{figure*}

In order to understand why the $r_{\mathrm{in}}/a_{\rm p}=0.35$ case is dominated by the variability component at twice the planet's orbital frequency, it is useful to consider time evolution of the Fourier components of the surface density, integrated over the inner parts of the disc (between $r_{\mathrm{in}}$ and $a_{\rm p}$):
\begin{equation}
\tilde\Sigma_m(t)=\frac{1}{2\pi(a_{\rm p}-r_{\mathrm{in}})}\int_{r_{\mathrm{in}}}^{a_{\rm p}}\int_0^{2\pi}\Sigma(r,\phi,t)~\mathrm{e}^{-\mathrm{i} m \phi} \mathrm{d}\phi\mathrm{d} r.
\end{equation}
In Figure \ref{fig:fourier} we plot $\tilde\Sigma_m$ for $m=1$, 2 \& 3, showing that the $m=2$ component indeed dominates the inner disc. We speculate that this mode is dominant for $r_{\mathrm{in}}/a_{\rm p}=0.35$ because it corresponds to the density wave launched at the 3:1 inner Lindblad resonance, which is an $m=2$ mode excited at $r_{\mathrm{in}}/a_{\rm p}=0.48$ \citep{papaloizou01}.

\begin{figure}
    \begin{center}
    \includegraphics[scale=0.8]{fourier_comp_035.eps}
    \caption{Time evolution of the first three Fourier components of the inner disc surface density for the case of $r_{\mathrm{in}}/a_{\rm p}=0.35$ shown in Figure \ref{fig:density_snaps_q4a}.}
    \label{fig:fourier}
    \end{center}
\end{figure}

This feature may have important observational consequences, as it suggests that observing pulsed accretion alone is not enough to deduce the orbital period of the planet. It is necessary to break this degeneracy by other means, for instance using radial velocity measurements as was done for CI Tau.

\subsection{Planet inside the cavity}
\label{sec:inside}
So far we have considered the case where the planet's orbit lies outside the inner disc edge, i.e. $a_{\rm p} (1-e_{\rm p})> r_{\mathrm{in}}$.  This is consistent with the observed stellar rotation period (6 days) for CI Tau if we assume that the inner disc is truncated at the corotation radius. Indeed, if $r_{\mathrm{in}}$ is determined by magnetosphere truncation, then the disc rotation rate at $r_{\mathrm{in}}$ is expected to be close to the stellar rotation rate \citep[e.g.,][]{lai14a}.

However, it is possible that the inner disc radius of CI Tau is larger than the corotation radius. Indeed modelling of the CI Tau disc by \citet{mcclure13} has suggested an inner disc edge at 0.12 au, which would put CI Tau b inside the inner cavity of the disc. More generally, it is useful to consider the case of a planet orbiting inside the inner edge of the disc; such a case may occur at the end-stage of disc migration, as disc torques may push the planet slightly inwards of the disc inner truncation radius.

We therefore ran additional simulations with $a_{\rm p}(1+e_{\rm p})<r_{\mathrm{in}}$. The numerical setup is the same, the only difference being that the planet is no longer in the computational domain. We still observed the pulsed accretion phenomenon. The accretion rate time series and the corresponding periodograms look similar to the case where the planet orbits in the disc. Since these plots are similar to Fig.~\ref{fig:mdot_per_q10}, we simply summarize our findings in Table \ref{tab:inside}, which lists the ratio $\dot{M}_{\max}/\dot{M}_{\min}$ (similar to what is plotted in Figures \ref{fig:max_q10} and \ref{fig:max_qe2}), as well as the dominant frequency of the pulsed accretion. We see that larger mass planets lead to larger amplitude pulsed accretion (for $q=0.001$, the amplitude of the pulse is almost zero, regardless of whether the planet is eccentric or not). For planets on circular orbits we did not observe any pulsed accretion. In almost all cases where pulsed accretion is observed, the dominant frequency of the pulsation is the planet's orbital frequency. The only exception is the case $q=0.001$, $r_{\mathrm{in}}/a_{\rm p}=1.5$ and $e_{\rm p}=0.2$, where two peaks of equal amplitude are observed at $\Omega_{\rm p}$ and $2\Omega_{\rm p}$, although in this case the amplitude of variation in the accretion rate is very small.

\begin{table}
	\centering
	\caption{Results of simulations for a planet inside the disc's inner edge. For each planet-to-star mass ratio $q$, separation between planet and disc inner edge $r_{\mathrm{in}}/a_{\rm p}$, and planet eccentricity $e_{\rm p}$, we give the peak-to-trough amplitude of the accretion rate at the inner edge $\dot{M}_{\min}/\dot{M}_{\min}$, and the dominant frequency of the pulsed accretion (in units of the planet's orbital frequency).}
	\label{tab:inside}
	\begin{tabular}{lcccc}
		\hline
		$q$ & $r_{\mathrm{in}}/a_{\rm p}$ & $e_{\rm p}$ & $\dot{M}_{\max}/\dot{M}_{\min}$ & Dominant frequency ($\Omega_{\rm p}$) \\
		\hline
		0.010 & 1.35 & 0.2 & 3.68 & 1 \\
		0.010 & 1.50 & 0.2 & 2.54 & 1 \\
		0.010 & 1.65 & 0.2 & 2.39 & 1 \\
		0.004 & 1.35 & 0.2 & 1.40 & 1 \\
		0.004 & 1.50 & 0.2 & 1.40 & 1 \\
		0.004 & 1.65 & 0.2 & 1.39 & 1 \\
		0.001 & 1.35 & 0.2 & 1.13 & 1 \\
		0.001 & 1.50 & 0.2 & 1.06 & 1--2 \\
		0.001 & 1.65 & 0.2 & 1.06 & 1 \\
		0.001 & 1.35 & 0.0 & 1.00 & -- \\
		0.001 & 1.50 & 0.0 & 1.00 & -- \\
		0.001 & 1.65 & 0.0 & 1.00 & -- \\
		\hline
	\end{tabular}
\end{table}

\section{Summary and Discussion}
\label{sec:summary}

In this paper we have used hydrodynamical simulations to study the
accretion variabilities at the inner edge of a protoplanetary disc in
the presence of a hot Jupiter. This is motivated by the recent
observations of the T-Tauri star CI Tau with a young hot Jupiter
candidate. We have shown that a giant planetary companion
(planet-to-star mass ratio of $\sim 0.005$) on an eccentric orbit can
drive pulsed accretion onto the star with a period matching the
orbital period of the planet, in agreement with the observation. We
have also found that an equally massive but circular planet would not
produce such a large-amplitude pulsed accretion.  This suggest that
the candidate giant planet around CI Tau is indeed eccentric.

More generally, we have systematically investigated how the accretion variabilities
depend on the planet mass, orbital semi-major axis and eccentricity.
For the typical disc parameters adopted in this paper (aspect ratio $H/r=0.05$
and viscosity $\alpha=0.1$), we find the following trends:

(1) An eccentric planet can drive large-amplitude pulsed accretion onto the
central star, with the dominant variability frequency given by one or
two times the planet's orbital frequency $\Omega_p$.  The variability amplitude
generally increases with the planet's eccentricity.  A circular giant
planet produces a small or negligible accretion variability (see
Figs.~\ref{fig:mdot_per_q10}-\ref{fig:max_q10}).

(2) More massive planets tend to drive accretion variability with large amplitudes,
although the dependence may not be strictly monotonic (see Figs.~\ref{fig:mdot_per_qe2}-\ref{fig:max_qe2}).

(3) The accretion variability depends in a non-trivial way on the planet's semi-major axis
relative to the inner disc radius (Sections \ref{sec:ap} and \ref{sec:inside}). For a given planetary mass
and eccentricity, the dominant variability frequency may change from $\Omega_p$ to
$2\Omega_p$ and the amplitude may change non-monotonically as $r_{\mathrm{in}}/a_{\rm p}$ changes
(see Fig.~\ref{fig:mdot_per_q4a}).

We emphasize that some of our more quantitative results (such as the
non-monotonic trends) must be considered tentative. An important
limitation of the work reported here is that our simulations only
covered the region outside the inner disc truncation radius ($r_{\mathrm{in}}$).
We used an inflow ``diode'' boundary condition at $r=r_{\mathrm{in}}$
(see Section 2), and this boundary condition cannot be justified
rigorously without actually simulating the flow inside $r_{\mathrm{in}}$.
A real protoplanetary disc is likely truncated
by the magnetic field of the central star. So an ``authentic'' numerical
study of the accretion variability induced by a planet would involve full 3D MHD
simulations of magnetosphere accretion, a complicated
task that is beyond the scope of the paper
\citep[see][for a review]{lai14a,romanova14}. In any case, the long-term
simulations required to attain ``quasi-steady'' results, as well as the coverage of
a large parameter space, as we have attempted in this
paper using viscous hydrodynamics, would be difficult to replicate
in full MHD simulations. Overall, despite the caveats of the simulations reported in
this paper, we believe that our general results and trends are valid,
at least qualitatively \citep[see][for a similar problem
of circumbinary accretion]{mml17,mml19}. These results can serve as a guide for ongoing
observations of young hot Jupiters in protoplanetary discs and for future
more sophisticated numerical simulations.

\section*{Acknowledgements}
This work has been supported in part by NASA grants NNX14AG94G and 80NSSC19K0444, and NSF grant AST-1715246. The research done in this project
made use of the SciPy stack \citep{scipy}, including
NumPy \citep{numpy} and Matplotlib \citep{matplotlib}, as well as Astropy,\footnote{http://www.astropy.org} a community-developed core Python package for Astronomy \citep{astropy:2013, astropy:2018}.

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


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text:
Search - Mozart, Beethoven, Bruggen :: Symphony 40
Mozart, Beethoven, Bruggen
Symphony 40
Track Listings (7) - Disc #1
Symphony No. 40 in G minor, K. 550: 1. Molto allegro
Symphony No. 40 in G minor, K. 550: 2. Andante
Symphony No. 40 in G minor, K. 550: 3. Menuetto (Allegretto)
Symphony No. 40 in G minor, K. 550: 4. Allegro assai
Symphony No. 1 in C major, Op. 21: 1. Adagio molto - Allegro con brio
Symphony No. 1 in C major, Op. 21: 2. Andante cantabile con moto
Symphony No. 1 in C major, Op. 21: 3. Menuetto (Allegro molto e vivace)
Symphony No. 1 in C major, Op. 21: 4. Finale (Adagio - Allegro molto e vivace)
All Artists: Mozart, Beethoven, Bruggen, 18th Century
Title: Symphony 40
Styles: Historical Periods, Classical (c.1770-1830), Symphonies


text:
Esmond Mills Photos
Where the world famous Esmond Bunny Blankets were made.
Photos courtesy of Marsha Croce.
Click on images to enlarge.
Filed Under: Photos Tagged With: Esmond blankets, Esmond Bunny Blanket, Esmond Mill, Esmond Mill Esmond R.I., Esmond Rhode Island, New England Mill History, Rhode Island Industrial History, Rhode Island Mill History, Rhode Island Woolen Mill, Smithfield Rhode Island Mill History
Esmond Mill Under Construction – Photos
These pictures were made from glass negatives showing the Esmond Mill under construction. They were donated to the Smithfield Preservation Commission by the Bromberg family.
Filed Under: Photos Tagged With: Enfield R.I., Esmond blankets, Esmond Mill Smithfield R.I., Esmond Mill Smithfield Rhode Island, Esmond Mills, Esmond Mills Smithfield R. I., Esmond Rhode Island, New England Manufacturing History, Rhode Island Manufacturing History, Rhode Island Mill History, Smithfield R. I. History
Woonsocket R. I. Fires – 1800s
Unknown Newspaper
Filed Under: Articles Tagged With: Edward Harris Woonsocket RI, Elliot's Mills Woonsocket R. I., George C. Ballou Cotton Factory, George C. Ballou Smithfield R. I., Lippett Woolen Company Woonsocket R. I., New England Fire Fighting History, Rhode Island Fire Fighting History, Rhode Island Manufacturing History, Rhode Island Mill Fires, Rhode Island Mill History, Social Mills Fire Woonsocket R. I., Social Mills Woonsocket R. I., Woonsocket Fire Department History, Woonsocket Fire History
The Stillwater Grain Mills
The Stillwater Grain Mill(s) was located on Capron Road across from the trail head of the present-day Stillwater Scenic Walkway. Cement foundations can still be seen. The mill was in operation as early as 1893, and was still in operation in 1916. No further information is known.
The Olneyville Times
Filed Under: Articles Tagged With: A. St. Onge Georgiaville R. I., Adin M. Capron of Smithfield, F. C. Latham Smithfield R. I., Grist Mills In Rhode Island, Pratts Animal Regulator, Pratts Disinfectant, Rhode Island Mill History, Smithfield R. I. Grain Mill, Stillwater Grain Mills Centerdale R. I., Stillwater Grain Mills Harrisville R. I., Stillwater Heights Stock Farm, Stillwater R. I. History
Esmond Blanket Card – Early 20th Century
Printed on thin paper and about the size of a business card,, this item was placed in the boxes that the Esmond blankets were sold in, and was usually disposed of, thereby making them rare today.
Filed Under: Photos Tagged With: Esmond blankets, Esmond Bunny Blanket, Esmond Mills, Esmond Mills History, Rhode Island Mill History, Rhode Island Textile History, Rhode Island Textile Industry, Smithfield R. I. Textile History
Slatersville, Rhode Island
From the book Picturesque Rhode Island – 1881
Filed Under: Photos Tagged With: Industrial Revolution, New England Mill History, North Smithfield R. I., North Smithfield R.I. History, North Smithfield Rhode Island, Rhode Island Mill History, Slatersville Rhode Island History
Stillwater Worsted Mill, Greenville, R. I.
The Stillwater Worsted Mill, also known as the "Levy Mill" should not be confused with the Stillwater Mill, also known as the Lister Mill, which once stood on Stillwater Road in the Stillwater section of Smithfield. The mill pictured here was located on Austin Avenue in Greenville, and is today an assisted living residence.
Filed Under: Photos Tagged With: Levy Mill Rhode Island, Rhode Island Manufacturing History, Rhode Island Mill History, Rhode Island Textile Industry, Stillwater Mill Rhode Island
Lorain Mill, Pawtucket, R. I.
Filed Under: Photos Tagged With: Lorain Mill Pawtucket R. I., Rhode Island Manufacturing History, Rhode Island Mill History
Woonsocket, R. I. Mills
Filed Under: Photos Tagged With: Alice Mill Woonsocket R. I., American Wringer Woonsocket R. I., Blackstone River History, Globe Bridge Woonsocket, Globe Village Rhode Island, New England Manufacturing History, Rhode Island Manufacturing History, Rhode Island Mill History, Social Mill Woonsocket, Taft Pierce Mill Woonsocket, Woonsocket Mill History, Woonsocket R. I. History, Woonsocket R. I. Mill District, Woonsocket Rhode Island Mills
Forgotten Industries of Spragueville & Mountaindale
First published in the Smithfield Times, March, 2020
1895 Map of Spragueville & Mountaindale.
Spragueville is an area of Smithfield with no clearly defined borders located on the Greenville side of town. It includes the Gallagher Middle School, and extends eastward down Spragueville Road to Mountaindale Road, then follows Mountaindale Road to where it crosses the reservoir at the bottom of Wolf Hill. On the opposite side of the water is another undefined area that in the 1800s was known as "Mountain Dale". One wouldn't know it today, but there was a time during America's Industrial revolution that the area was a bustling commerce center.
Spragueville was settled in 1733 by Abraham Smith who erected a grist mill and two houses. However, the area is named for Thomas Sprague, a former sea captain who came to Smithfield nearly a century later. Sometime after 1824 Sprague built a large granite cotton mill which measured 80 by 120 feet, and established "T. Sprague & Sons". According to old maps of the town, the mill stood on the north side of Mountaindale Road in the area now occupied by present-day Richard Street. The mill originally drew its power from the Stillwater River, but in 1870 steam turbines were installed.
In 1847 the mill was purchased by Wanton Vaughan who incorporated under "The Granite Mill Company". The enterprise later passed to Christopher Vaughan, Esquire, who became the sole proprietor.
The mill was part of what was known as "The Granite Mill Estate", on which property also sat the private homes of the Vaughan family and possibly lodging for some of the workers.
The Granite Mill Company was very successful, and by the 1870s had 112 looms and 5,000 spindles in operation. However the mill fell inactive from 1886 to 1889.
By the 1890s the mill was back in operation under the direction of the Mercer brothers. What ultimately became of the mill is uncertain, but no remains of it can be found today.
Another large mill which once existed in the area was the Mountain Dale Hosiery Mill, which as its name would imply, was in Mountaindale. According to old maps it stood to the south side of Mountaindale Rd. at the base of Wolf Hill. The remains of this mill can still be seen today.
The hosiery mill was owned by William Steere of Greenville, and then others over the following years.
Mills would at times become inactive for various reasons, from low water levels and machinery problems, to fluctuations in cotton prices.
On March 31, 1871, the following news snippet appeared in the Woonsocket Patriot. "The Mountain Dale Hosiery Mill, which has been stopped for more than two years, has been recently leased by Pierce Kane, Esq., of Saratoga Co., New York, and he is now starting it up. He will make a class of goods similar to those formerly manufactured at the same mill by Wm. A. Steere."
At some point afterwards the property came to be operated by J. P. & J. G. Ray, (Full names unknown), but it appears that the mill once again fell idle, and shortly before midnight on November 1, 1877, it was destroyed by fire. The loss amounted to $9,000, and the property was not insured.
The mill was evidently rebuilt for it and three other large buildings next to it were still indicated on 1895 maps of Smithfield. Today these structures are gone.
A lesser known Mountaindale enterprise involved a small factory established by Waterman Smith and Thomas Harris in the 1820s, which is said to have been located near the junction of the Stillwater River and Reaper's Brook. Smith and Harris manufactured parts for cotton mills such as spindles and shuttles which were needed for the many textile mills being built along the Blackstone Valley.
In the days before modern refrigeration people kept food cold with ice, which made "ice harvesting" a lucrative business. In the early 20th century a large ice house belonging to the East Providence Ice Company stood on the shoreline of the reservoir at the bottom of Mountaindale Road.
The "harvesting" took place during the winter, when the water froze thick enough to support men and horses. Ice saws were used to cut blocks of ice which would be brought to the ice house and taken inside by on a conveyer belt. There workers would pack the ice in sawdust which helped to prevent melting, and the ice house itself was constructed with thick walls also insulated with sawdust.
The East Providence Ice Company went out of business sometime during World War II, as did many other ice businesses with the advent of electric refrigerators.
Today a modern industrial park is located in the heart of Spragueville, but unfortunately the historic factories which gave the area a page in Rhode Island history are gone.
Filed Under: Articles Tagged With: Christopher Vaughn Esquire Spragueville R.I., East Providence Ice Company, Ice House History, Labor History Rhode Island, Mountain Dale Hosiery Mill, Mountaindale Rhode Island, New England Mill History, Rhode Island Mill History, Smithfield R.I. Mill History, Spragueville R. I. Mill, Spragueville Rhode Island, The Granite Mill Company Smithfield R.I., The Granite Mill Company Spragueville R.I., Thomas Harris Smithfield R.I., Waterman Smith of Smithfield R.I., William Steere Greenville R.I., William Steere Smithfield R.I.


The way Charlie Heebner remembers it, being aboard the passenger train that hurtled off an overpass in Washington state Monday morning was "like being inside an exploding bomb."
Heebner, 79, and his wife, Beverly, had looked forward to this trip aboard the Amtrak Cascades 501 train in its inaugural journey from Seattle to Portland, Oregon. The Heebners, longtime train riders, wanted to be on the first run, they told CNN affiliate KOMO.
A jolt and shattered glass interrupted their eagerly awaited trip.
"All of a sudden it was just, crash ... the train went like this," Beverly Heebner, 78, told KOMO, slanting her arms to illustrate.
The train derailed off an overpass near the city of DuPont, sending some of the cars onto a busy Interstate 5.
At least three people were killed, and more than 100 others -- including some highway motorists -- were injured.
"After getting myself upright and my legs unfolded, I saw (my wife's) legs," Charlie Heebner told KOMO. "I reached down and I shook one, and she shook it back. I said, 'Are you all right?' And she said, 'I think so.' "
The couple crawled out of a window of the train, which had been carrying more than 80 people. They told KOMO their harrowing story after they were treated at a hospital for minor injuries and released.
The train, after running parallel to I-5, went into a curve of the highway. It apparently ran off the track while approaching or crossing the trestle over I-5, with some falling to the road below, landing on vehicles. One rail car dangled precariously over the highway.
The cause of the wreck hasn't been determined. The train was traveling 80 mph in a 30-mph zone, but it's not clear why, National Transportation Safety Board member T. Bella Dinh-Zarr said.
Chris Karnes, a passenger, said he boarded the train between Seattle and Tacoma and took a seat on the third or fourth car.
Karnes said the train was moving at a "pretty good pace," passing cars on the highway while the train was running parallel to the road before it went into the curve over the interstate.
"We felt a little bit of a jolt and then at a certain point we could hear crumpling of the train car, and we were catapulted into the seats in front of us," said Karnes, who also is the chairman of the Pierce Transit Community Transportation Advisory Group.
Amtrak 501: Amtrak 501, emergency, emergency, emergency. We are on the ground! We are on the bridge (unintelligible) on the freeway. We need EMS, ASAP. It looks like they're already starting to show up.
Dispatcher: 501, come in. ... Hey guys, what happened?
Dispatcher: ... Is everybody OK?
Army 2nd Lt. Robert McCoy says he hit the brakes of his truck just in time.
He heard a noise as he was driving on I-5, and glanced ahead to see the train crash through the overpass.
"It hit three vehicles that were in front of me," including a tractor-trailer, McCoy told CNN affiliate KCPQ.
McCoy, assigned to the nearby Joint Base Lewis-McChord, took a tourniquet and a CPR mask from his truck and headed toward the wreck.
People had been ejected from the train onto the pavement, he said. He carried some of them out of the road to safety, and eventually he and another person went on top of the damaged semi and climbed into a suspended rail car.
"There were people yelling. There were people looking for each other, loved ones," he told KCPQ.
He said he helped a woman who was dangling out of the train.
"Her daughter kind of pulled her out backwards and ... I just reached under her, and just kind of got to a point where I could pick her up and just kind of put her down on some form of semi-safe structure," he told KCPQ.
Another motorist, Daniel Konzelman, was driving with his girlfriend on I-5 headed to work when he saw the train "hanging off of the bridge like you've seen in all the pictures," he told CNN on Monday night.
Konzelman, who told The Seattle Times he was an Eagle Scout who'd been trained in first aid, said he got off the freeway and parked his van. Dressed in a suit, he retrieved an emergency head lamp and boots from the back of his van and rushed to the wreck, he told CNN.
He said he tried to give wreck survivors direction, and helped some of them off the train, until first responders arrived.
"Initially, I climbed into the train car that was positioned sideways on the bridge and made sure that everybody in there was stable, and if they could get out, helped them out," he told CNN. "And if they had an injury, (I) made sure that there was people there to tend to them and stay with them.
"And (I) just kind of systematically worked my way through the cars until the first responders got there, and probably was able to help, I would say, 15 people get out before the firefighters or police officers arrived."
Passenger Anthony Raimondi had been on plenty of rail rides before -- he worked for 17 years for Amtrak as a ticket agent in Minnesota.
He was in business class Monday when the car "started to lean."
"Then all of the sudden everything went dark, and stuff started flying around inside the car" before the train came to a stop, he told CNN's "New Day" on Tuesday.
"(We) picked ourselves (up) and shook ourselves off, and one of the passengers pushed out the window," he said.
Raimondi climbed through the window and helped someone else out.
"I feel very, very lucky that I came out with just a bruise here and there," he said.


Atrial fibrillation is the most common cardiac arrhythmia – a disorder where the person has an irregular heartbeat – and it is growing worldwide. Atrial fibrillation raises the risk of stroke by nearly four times and is associated with a higher risk of death. However, at the moment it is unclear whether atrial fibrillation is associated with a higher risk of other cardiovascular diseases, such as coronary heart disease or peripheral vascular disease (clots in the leg).
In a new study published in the International Journal of Epidemiology, researchers at The George Institute UK have examined the relationship between blood pressure and atrial fibrillation, and the relationship between atrial fibrillation and the development of cardiovascular disease in a cohort of 4.3 million adults in the United Kingdom.
"We found that higher blood pressure was linked to a higher risk of developing atrial fibrillation; a 20 mm Hg higher systolic blood pressure increased the risk of atrial fibrillation by 21%," said Connor Emdin, one of the researchers in the study.
Other researchers involved the study were Simon Anderson, Reza Khorshidi, Mark Woodward, Stephen MacMahon, and Terrence Dwyer.


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