text:
The Owl House NYCC panel eulogized a brilliant show cut short: 'We did our best'
Creator Dana Terrace and the cast of the show take to the stage
By Petrana Radulovic Oct 6, 2022, 5:07pm EDT
Share All sharing options for: The Owl House NYCC panel eulogized a brilliant show cut short: 'We did our best'
The Owl House panel was bittersweet from the moment it started; this is the show's first panel since it premiered in early 2020, but also the show's last. With the shortened, three episode final season premiered on Oct. 15, The Owl House is gearing up for an epic finale.
In its two-season run on Disney Channel, The Owl House has amassed a passionate fanbase. It follows a plucky human named Luz who finds herself in a world full of witches and demons. And while the show has also garnered critical acclaim, it did not get renewed for a full third season. So this is the first and last time that the show's cast and crew can revel in that NYCC panel experience.
Creator Dana Terrace took to the stage with some of the show's cast, including Sarah Nicole Robles (Luz), Mae Whitman (Amity), Zeno Robinson (Hunter), Cissy Jones (Lilith), and Alex Hirsch (King and Hooty).
"I had the very rare privilege of watching the show form its inception form when Dana put together the series bible to now," Hirsch said while on stage. "It's rare and rewarding to be part of something so loved."
Hirsch, who personally made a Hooty puppet for the occasion, also shared how The Owl House helped him develop a key voice acting skill.
"I never had to cry on Gravity Falls," Hirsch laughs. "King goes through some rough stuff. The Owl House taught me to cry on command."
The cast also shared some insights into their characters. Whitman, in particular, gushed about Amity's journey from aloof mean girl to a blushing love interest.
"Something I thought is so magical about [Amity] is that she is complex, she's complicated. She has issues. She is dealing with some stuff! You didn't really get to know her vulnerable side for a while," Whitman describes. "When she met Luz she realized she didn't have to be that way, she could tap into her softer side, her more vulnerable side."
The Owl House made Disney animation history by featuring a queer romance at the center of the show, along featuring a nonbinary person as its main character.
"For me, coming out as pan, I felt even more strongly and passionately about this," Whitman explains. "Having a show like this when growing up would've been really cool. I think it's great for everyone to have that visibility, that connection."
In addition to a new clip, Terrace also revealed some concept art of the upcoming season, which includes some new outfits for the characters, Luz's hometown in Connecticut (all decked out for Halloween), and giraffes! (It's a long-running series joke.) Some new footage was also revealed, including a revamped theme song for the final season. Terrace spoke about the moments she was most proud of the show throughout the entirety of production.
"The times that I hold dearest to my heart are the crew screenings we've tried to do over Zoom, or the few times we've tried to watch the finished show... totally legally on the channel," Terrace describes. "To be able to sit there with the crew and be like damn we pulled it off!"
As for the fact that the third season is shortened, Terrace sounded disappointed that she didn't get to dive into Hooty's true origin, or give some more backstory to Raine and Eda — who she calls her favorite characters to write. But she says that the crew went all out when it came to making sure that the animation and story were the absolute best for this last hurrah.
"What can you do at this point?" she says. "We did our best."
The first of the three Owl House finale specials premieres on Oct. 15 on Disney Channel at 9 p.m. EST. The first two seasons are available on Disney Plus.
All the NYCC 2022 news, trailers, and reveals in one place
The Winchesters NYCC panel revealed a Supernatural prequel with more Jensen Ackles than expected
Chris Pratt's Mario voice has a, uh, vaguely Italian thing going on, sure


text:
Tops and flops at the 2019 Tour de France
Julian Alaphilippe (Getty Images)
Thomas 'defied the odds' at TDF, says Brailsford
Egan Bernal wins 2019 Tour de France
Caleb Ewan wins final stage of Tour de France
Paris - A look back over the 2019 Tour de France at those who reached beyond the norm and those who failed to deliver what had been expected of them.
Julian Alaphilippe
Will go down in Tour history for an unrelentingly valiant ride with his bullet like supertuck downhill charge, and his uphill short-climb kick, had a human touch and sheer guts as he thrilled France with his unlikely 14 days in yellow.
The Jumbo-Visma Team
The most improved team of the Tour with a first-day yellow jersey for Mike Teunissen, a sprint win for the grumpy speed king Dylan Groenewegen, rookie Wout van Aert emerging as an all-round man for the future and a team time-trial win all helping to put their man Steven Kruijswijk onto the podium in third place.
Caleb Ewan
After winning his first sprint Ewan said the photo-finish victory was 'almost worth leaving Australia for'. The 22-year-old ended the 2019 edition with three stage wins, one more than either Simon Yates or Julian Alaphilippe. In fact he lives in Monaco, and can put his three wins in the bank and look forward to winning more.
Yates came to the Tour having flopped at the Giro d'Italia and was riding under the radar as sherpa for his twin Adam. He emerged from the shadows to close out a pair of breakaways and come home with his first two Tour de France stage wins. He told AFP he would next target the 2020 Olympic road race in Tokyo before turning his attention to the Tour de France in 2021.
Thierry Gouvenou
The course designer has to be given a certain amount of credit for putting together 21 stages that encouraged the breakaways that ignited such a thrilling Tour and for placing the Alpine trilogy that ultimately decided the race right at the end, maintaining the suspense, even after the weather almost undid his work.
THE FLOPS
Jakob Fuglsang
The Dane came into the Tour de France on the back of a Liege-Bastogne-Liege one-day win where, he said, he had decided to win or die, and a one-week Criterium du Dauphine triumph that suggested he was a potential Tour champion. But the Astana captain built a reputation as a gripe when he moaned after losing time on the stage to Albi saying no-one had warned him about a crosswind, a claim that exasperated his bosses. His disappointing Tour ended when he crashed out, through no fault of his own.
Came to the 2019 Tour looking for a place in the top five or even the podium spot but struggled every time the going got tough on a climb. He was also unable to keep up in a breakaway of lesser riders on the Galibier after the main contenders decided to ignore him and let him go.
In the end, Bardet just about redeemed himself with the king of the mountains jersey, but the man who finished on the Tour de France podium spots in 2016 and 2017 was a flop having apparently overtrained and by Sunday was almost half an hour behind Bernal. After losing more than a minute to the big guns on the first big climb, up La Planche des Belles Filles, he stopped at the finish line, wiped out. He cut a sorry sight as compatriots Alaphilippe and Thibaut Pinot shone.
Read more on: tdf 2019 | cycling
Proteas: Their schoolboy error in PE Proteas: 5 selections to consider for Wanderers Test De Kock replaces Du Plessis as Proteas ODI captain 'Average' Jonty aware of privileged selection Rabada: I've let the team and myself down
What do you enjoy most about the Tour de France?
The stunning views of the countryside
The expert commentators
Watching a sprint finish to a stage
Seeing the riders toil in the mountains
28% The stunning views of the countryside
12% The expert commentators
11% Watching a sprint finish to a stage
49% Seeing the riders toil in the mountains
Andy40_T
Frannamc
Writerem

redpajama_set_name: RedPajamaCommonCrawl


text:
The countdown for the formation of the International Committee of the Mediterranean Games began in 1959 in Beirut during the 3rd edition of the Mediterranean Games.
The Chairman of the Organizing Committee and President of the Lebanese National Olympic Committee, Gabriel Gemayel, proposed the creation of a permanent Committee that would ensure the sustainability of the Games.
The ICMG was officially created on June 16, 1961 in Athens, in the premices of Athens Tennis Club. The meeting of the Executive Committee was held under the chairmanship of Gabriel Gemayel and in the presence of Juan Antonio Samaranch (Vice-President), Ioannis Ketseas (Secretary General), Giulio Onesti, Mohammed Benzelloun, Ahmed D. Touny. During the meeting, Gemayel presented the statute of the ICMG, which was based on the International Olympic Committee statute.
This was followed by the founding meeting of all members of the National Olympic Committees who participated in the Mediterranean Games. Except President Gabriel Gemayel, they were also present, Mohammed Taher Pasha (Honorary President of the ICMG), Juan Antonio Samaranch (Vice-President), Ioannis Ketseas (Secretary General), François Pietri (IOC member – France), Giordio de Stefani (IOC member – Italy), Prince Pierre of Monaco (IOC member – Monaco), Ahmed D. Touny (IOC member – Republic Arab United), Theodosios Papathanasiadis (Greece), Giulio Onesti (Italy), Marcello Garroni (Italy), Bruno Zauli (Italy), Nassif Majdalani (Lebanon), Mohammed Benzelloun (Morocco), Ahmed Elwetidi (United Arab Republic), Salim Nabi (United Arab Republic), Chedly Zouiten (Tunisia), Burhan Felek (Turkey).
The ICMG statute was approved during the meeting and was also accepted, the proposal of the Hellenic Olympic Committee to place the headquarters of the ICMG on a permanent basis in Athens.
The first Chairman of the Committee was Gabriel Gemayel, followed by Mohamed Mzali 1979-1987 (Tunisia), Claude Collard 1987-2003 (France) and from 2003 onwards, Amar ADDADI (Algeria).
Concerning the Secretary General, Ioannis Ketseas was succeded by Epaminondas Petralias, Nikos Filaretos, Minos Kyriakou, Isidoros Kouvelos and Iakovos Filippoussis, who are all Greeks.


Sehen Sie sich das Profil von Rachel Beatty auf LinkedIn an, dem weltweit größten beruflichen Netzwerk. 6 Jobs sind im Profil von Rachel Beatty aufgelistet.
Rachel Beatty of Ball State University, IN. Read 1 publications. Contact Rachel Beatty on ResearchGate, the professional network for scientists.
Rating and reviews for Professor Rachel Beatty from Ball State University Muncie, IN United States.
DALNET STAFF. CONTACT, POSITION, PHONE, EMAIL. Ms. Rachel Beatty, Director, Business Affairs / Treasurer.
Clipping found in The Decatur Daily Review in Decatur, Macon, Illinois on Jan 9, Rachel Beatty Kingsley Dunham a W. will and M. Dunham, w i f e II.
Groups vow to work together to eradicate homelessness among veterans in Dover.
Rachel Beatty is a teacher at Jefferson Academy in Jefferson, GA. Review Rachel Beatty's ratings by students and parents.
Celebrate the life of Ms Ellen Lea Gundersen, leave a kind word or memory and get funeral service information care of Rosar-Morrison Funeral Home & Chapel.
Genealogy for Rachel Beatty (deceased) family tree on Geni, with over 185 million profiles of ancestors and living relatives.
Discover life events, stories and photos about Rachel Beatty ( ) of Cambridge,Russell,Ontario.
Ancestry.ca has at least 1 birth record for Rachel Beatty, among more than 964 birth records for this surname.
TOTAL WARRIOR 2011: PREPARE FOR THE TOUGHEST 10K & THE TOUGHEST 10 MILE EVENTS ON EARTH. Total Warrior brings you Super 10 Weekend.
Junior Hymnbook Book 2. by Rachel Beatty Kahl. Book condition: Good. Book Description. Book Two. Wear to covers. Markings to pages. Binding intact.
Rachel Beatty Riedl (Northwestern University, Illinois). Authoritarian Origins of Democratic Party Systems in Africa. This book investigates why seemingly similar African countries developed very different forms of democratic party systems. innerhalb 1-2 Wochen. Buch. EUR 28,70*. Artikel merken. In den Warenkorb.
The Iron Cage of Democracy - Kellogg Institute for International Read more about riedl, institutional, competitive, electoral, democratic and organizational.
Country two step and swing at the Davis Graduate. Music: "Hey Girl" by Billy Currington - Duration: 2 minutes, 40 seconds views; 4 years ago. 1:48.
Book 1. Composed by Rachel Beatty Kahl. Arranged by Rachel Beatty Kahl. Music Sales America. Designed to be played with student's very first piano book.
Find Rachel Beatty Riedl's articles, email address, contact information, Twitter and more.
Posts about Rachel Beatty Riedl written by dadakim.
Rachel Beatty is a nurse practitioner in Grant, Florida.
Find Rachel Beatty's Social Media accounts, Addresses, Phone Numbers and Background Report (potential Criminal, Court and County Records).
Rachel Beatty hits a home-run and a walk-off double in an 8-7 victory over the SDSU Jackrabbits.
... CideCi's Independent Alternative and the Regeneration of Indigenous Cultural Spaces in Chiapas. Authors. Rachel Beatty, SIT Study Abroad. Home Institution.


text:
JCU euthanaise Council and Cairns Post story
Director of the pro-euthanasia group, Exit International Philip Nitschke, will be speaking in Cairns on Monday morning, contrary to the Cairns Post today.
The four-time nominee for Australian of the Year who holds a PhD in laser physics, is in Townsville this weekend, on route to a planned Cairns function on Monday.
Cairns Regional Council has banned Nitschke from holding his public forum in a meeting room at the city library.
"As soon as I became aware that Dr Nitschke had been denied access to Council-run facilities, I was horrified," Janine Aitken, Education Officer of James Cook University's Cairns Student Association told CairnsBlog.
Aitken, who ran for Council in 2008 against Sno Bonneau, has arranged for Dr Nitschke to speak at James Cook University, instead of the Cairns Regional Council library in Cairns.
"It's amazing that in this day and age the opportunity for open debate and access to information is being denied by Cairns Regional Council," Aitken said. "I see the need for this discussion to be had and am fortunate that I am supported by a Student Council that believes in the importance of free speech."
"We are delighted to be able to provide a venue for Dr Nitschke to speak at."
Nitschke called the Council's decision "farcical and implausible".
JCU Cairns Campus president, Justin Ganzer also warmly welcomes the controversial doctor to speak at his University, that the brain-dead lazy media refer to as 'Dr Death'.
"Although some people may not agree with what he has to say, or the certain ideas that he's putting across, nonetheless he should be able to express them," Justin Ganzer said this afternoon.
"We are approaching this delicately to ensure we're not upsetting anyone by holding this event. We had to talk with the University hierarchy to "make sure it wasn't going to cause any controversy for them," Ganzer says.
"I believe if you're going to have intelligent debate on any subject matter, you need to at least express both sides, or as many sides as possible. Whether you agree with it or not, this isn't a way to debate a topic."
"The [Cairns] Council acted in the best interests of their concerns, however I would assume that if there was concerns like that, there were measures that could be be taken. I guess the Council has their reasons for doing that."
You can listen to my interview with Justin here:
Carenda Jenkin, writing in today's Cairns Post, said that the Cairns city library wouldn't host a event because of security concerns...
[Nitschke's] office was told that "too many people may wish to attend" and "security would need to be involved, as they were at the last gathering".
But Dr Nitschke denied security was needed at a previous meeting in Cairns due to numbers. He said it was due to a power failure.
"We booked this venue in March and we are three days out from our workshop and there's no time to find another place to hold it," he said. "We haven't had any trouble in Townsville and we've been to the Cairns library before and we haven't had any problems in May 2005, when 50 people turned up.
"This mirrors what happened in Mackay when their neighbourhood centre made a last minute cancellation due to the philosophical views of the booking agent.
Cairns library manager Kerrie Still said the booking had not been confirmed but an inquiry had been made by Exit International's Lindy Boyd in March.
"The booking form was referred to me as the meeting purpose stated on the form was for a "public meeting" and in response to a standard question on the form answered "yes, would possibly attract media attention'," she said.
"The terms and conditions of use clearly state that library facilities are not available for public meetings that could exceed maximum venue capacity."
Simple. Only let the first 100 in.
Ms Still said she called Dr Nitschke's office and suggested that a larger facility would better suit their needs. "There was no last minute response or any delay on the part of the library," Ms Still said.
Yeah, sure. I bet some right-wing nut in Spence Street sent you orders when they got wind of it. I recall former Mayor Kevin Byrne banning Puppetry of the Penis from the Cairns Civic Theatre on more than one occasion, because he thought it was a bit too rude for Cairns.
Don't you love it when our politicians try to censor what we're allowed to see and hear?
Queensland Right to Life Cairns branch president Dr Tim Coyle said he was delighted to hear Mr Nitschke's workshop had encountered some problems.
"The usual thing in those workshops is that they give a detailed instruction on how to commit suicide and these kind of workshops are a bad influence," Dr Coyle said.
And you can sit in on a Council meeting and learn how some Councillors can multi-task: txt message their girl-friends and vote on selling off properties, all at the same time!
Nitschke's book, Killing Me Softly, that he co-wrote with Dr Fiona Stewart, was a compelling and radical examination of the euthanasia debate. Janet Homes a Court called said it advanced the discussion on dying painlessly and with dignity.
Nitschke was the first doctor in the world to administer a legal, voluntary, lethal injection.
Come and hear Dr Phillip Nitschke speak on Monday June 1st, from 11:30am to 2:30pm.
McGregor Road, Smithfield
The Refectory, Ground Floor
Building A2
at Saturday, May 30, 2009 Posted by Michael P Moore Labels: Cairns City Council, Cairns Regional Council
Obviously, the answer to those who are opposed to A.S is to give them a dose of cancer or (pick a disease) whose pain cannot be masked adiquitly with morphine - then make them sit by the bed, night after night, clutching their bible and watch ... it's fun. A bit of bed shitting, some screaming, some begging ... night after night ... day after day ,.... it's easy to be brave when you're not sick, it's easy to be morally resolute when it's not someone you love ... let 'em die if they choose, isn't that the whole point of freedom?
Sat May 30, 08:28:00 pm
S. Northy said...
I don't understand the fuss. We swtich off life support machines and watch people struggle to live..the body keeps on trying to breathe etc. Then we give cancer people huge does of morphine which effectivelt kils them...
Dutchie said...
There's two issues here:
1) a civil servant (as far as I am concerned it could be a left-wing nut too) pulling the plug on this last minute;
2) the euthenasia debate.
Ad 1) very worrying that this could have happened - very rude, actually. Dr. Coyle's argument is rubbish: if you want to find out how to kill yourself, just Google and you'll be presented with plenty of ideas.
Ad 2) I believe in the freedom of the individual to decide what it wants to do with him/herself. Or, allowing others to make the decision if that person is unable to do so, after prior authorisation. However, there must be strict conditions under which this euthanasia may be performed (of course!).
In the Netherlands, euthanasia is a criminal offence, unless certain conditions are fulfilled. So, conversely, if euthanasia is performed and complies with the law, it is in fact legal.
There's hardly any debate about this there, and it's no real issue (1.2% of all deaths are due to euthanasia). The majority of cases involve cancer or HIV/AIDS patients.
Please read the following summary outline of how it works in The Netherlands (whether you are for or against it):
Wikipedia: Euthanasia in the NetherlandsBasically, The Netherlands have codified a (guideline for a) practice that happens everywhere in the world ('undercover' euthanasia), thereby decriminalising doctors that comply with the patient's rational wishes.
And no, that didn't result in mass murders!
Pull the Plug on Cairns Blog said...
Typical left-wing claptrap masquerading as "news".
Despite Ms. Still at the Library giving you her story, you've called her a liar, defaming and slandering her.
And with what? A statement "Yeah, sure. I bet. . ." This ain't journalism, pal.
Sun May 31, 04:27:00 am
peterbartholomuse said...
This is has all the hallmarx of a media beat up. Kerry Still is abiding by the rules and has acted within her brief. The last meeting in 2005 was a quiet affair with little media attention... this could have been the same, except that whoever booked the library has gone outside the rules, by declaring it a public meeting that media could well be interested in.
This action has probably had the unexpected effect of giving Nitschke's meeting a higher profile than it would have otherwise gained. The CRC has been put in an invidious position, and the supposed late cancellation is the only issue here ... everything else is pure speculation and hyperbole
Sun May 31, 01:37:00 pm
what is the matter with listening to an argument put by someone knowledgeable. it'd be a sad day indeed if we prevented Mr Coyle from speaking in a public venue because someone might use this as an excuse to create a breach of the peace. Right-to-Lifers and their ilk do this all the time, and in Cairns, too, but we don't ban them.
Lillian at Yorkeys said...
All I have to say - is that if the Old Dog or Cat or the Budgie have gone past their use-by date & are looking very ordinary & sad & weary, & their kidneys/heart/lungs (etc etc) are failing, we go to the friendly vet, who does the Big Green Needle Thingie. Having gone through a fair few of these in my life with much-beloved pets, it takes all of about one minute, little or no pain, & they are released from their bodily suffering. They can go to heaven, & we go cry a river, as you do. Then we get up the next day, bury the beloved & life goes on, or it doesn't.
Why are we not allowed to do this for ourselves? Why are a pro-Christian (Catholic - & in John Howard's context - Protestant faction) hijacking my right to kill myself in a sane, peaceful & calm way, & with legal constraints in place as well, if I wish to do so?
If we as a society accept that we have total rights over what happens with our body, then why are we legally prevented, in this country, from ending our lives if we wish?
Even half a century ago (& many centuries before then) suicides were prevented from being buried in hallowed ground (ie. an agreed religiously-ordained community cemetery) as suicide was thought to be an act against God. I'm sure those who were brought up as Catholics could bring up even more Gothic reasons for this - I'll leave it up to them.
If I want to leave this planet, & go on to my next lifetime, why should some bunch of religious loonies have the right to dictate to me what I want to do?
Erm Unda, I think you mean that "it'd be a sad day indeed if we prevented Mr. Nitsche from speaking in a public venue"? Mr. Coyle is the guy that has the opposing camp (right to life), which of course has every right to speak too.
Jude Johnston said...
Having looked after my Mother during her terminal illness of stomach cancer and melanoma, (a guess as to which one killed her) and with a colostomy from previous bowel cancer, I would sit and hope desparately that her pain and suffering would end. Could I have aided and assisted her to end her life - I can categorically say No I couldn't. As much as I wanted her out of pain there is no way that I could do that. Herein lies the rub, how many of you could? It is all very well talking about it while we are healthy and death seems a long way off. What a huge ask to expect someone you love to end your life for you.
Bryan Law said...
I am forever grateful to the ICU nurse who assisted my father's death (at age 84) by giving him mucho Morphine "to make him comfortable".
He wasn't going to wake up. He had multiple organ failure, and breathed with the aid of a machine. A veteran's gold card ensured the hospital would continue making treatment available for however long the family would tolerate it.
Once the immediate family had gathered from various parts of country, we made our wishes known, and the medical staff assented.
The only fly in the ointment is that a relatively junior medical worker got to do the deed in a less than transparent way, and exposed herself to some personal risk in doing so.
An open system with checks and balances would be better. I've heard Dr Nitsche talk about Seconal, and how to get it. I'm hoping that if required, I too will find sympathetic medical staff when the time comes. If not, I know what to do.
Mon Jun 01, 01:19:00 am
Bryan, you are assuming that you will be in a position to administer Seconal. Do you then gather your loved ones around you, on a chosen date and time, tell them you love them, hold them in your arms and look in their eyes while you end your life. Not an easy call methinks.
thanks dutchie, but i meant what i said. i am trying to highlight the hypocrisy involved here: right to lifers and sundry other zealots demand the right to put their case in public venues(and i might add engage in thuggery - vide their activities in the recent RU 486 debate)but they want to prevent people like mr nitschke from putting his case. the only people likely to cause problems at today's meeting are the right to life goon squads.
Nitschke thanks JCU Cairns students
Blog Boys - 7:35am Monday morning
Watch out when you hear a beep
Wild Rivers heritage legislation, leads to conflic...
Susan Boyle loses 'Britain's Got Talent'
Compost earns its name
Kim Jong is ill
If Chatrooms were real
St Oink College of Cairns
Not the Great Depression
Cairns Post 31, CairnsBlog 71
7 TV News runs a dodgy survey
Kuranda Range Road speed increased
Hands off our Knob
The Chief Extra-spin Officer writes again
Robbing from the roach, giving to the paws
Ethics and conduct of a Councillor
IGA manager slams Cairns Post, Villa owner
Tune in to the Blog Boys
CEO to write a report on the report
The separation of power
Cookie gets a make over
Sick news day, Cairns style
Good time flies, like the good ol days
Maria Ball's killer sought
Council told to close fake Twitter account
Swines enroute to Cairns
Black and white and all over, almost
King is back, oh dear
Some poll thoughts
Cr Cooper says Comments inquiry is over
Missing Marvellous Macca on Monday
LNP office officially opens
Northern Watch goes live
Imitation, the sincerest form of flattery
The 500 worst passwords
How ideas trump economic crises
Council dishes out $116,000 to community
Cairns web guru develops iPhone app
And they're walking...
Jim and Lesley went swimming
Memo to Rupert
Joking journalists
The head of the church
What do you think, Ocker?
Kevin Bryne turned things around
The art of discreet txting
Who pays the ferryman?
Do ask, do tell
Stinger season over
Two degrees of separation
Townsville dengue outbreak over
Normal service
Put it on KB's tab, thanks
Port Carnivale this weekend
Cairns coev is 10 years old
Beach goes bush for Knob festival
We'll go to Townsville instead
Council to assist with Club planning
The best medicine
Healthy volunteers honoured
Cairns Post blames Yachtie collapse on decay!
Obama's first White House Correspondents' Dinner
Nuding it up
Councillor Bonneau caught colluding with developer...
Things are going up in QLD's sex trade
Yacht Club building reconstruction in ruins
Alley Project
Yacht Club building collapses
May's Place out now
Speaker's Corner returns
Foundry's Anti-discrimination Ad
Million Paws walk this Sunday
Budget Review: Ross Parisi
Blakety
Budget review: Dr Darren Delaney
Budget review: Syd Walker
Dear Australia - Love Kevin
Bligh in drag
Goodbye rego
More empty hulls
Cairns tourism website is well below standard
Going Guam again, a junket in fool's paradise
Review: Not Fit to Govern
Google's Larry Page goes back to university
Shock Jock Mackenzie vanishes
It's cold in them thar' hills
Councils focus on core activities
Dyslexics have a humour of sense
Harvesting roof water
'For the North' meeting called historic
Being Australian
DInner without Oliver
Twitter ya fav Blog
Regional Failure
A place for a new Barfly
The Briggs Guide to Life


text:
This photo provided by New York State Police on Saturday, Dec. 15, 2018, shows a rescued dog after it was thrown out of a vehicle in Cortland County, N.Y. A trucker driving nearby said the dogs were thrown from the rear passenger window of a dirty, rusty Dodge Durango. The trucker stopped and rescued the dogs. (New York State Police via AP)
Trucker saves dogs thrown from vehicle on New York highway
NEW YORK (AP) — A pair of beagle mixes are on the mend after authorities say someone threw them out of a moving vehicle on a snowy New York highway. The dogs were rescued by a passing trucker, but one was so badly mangled that a front leg had to be amputated.
New York State Police on Saturday asked for the public's help in finding the suspect or suspects in the incident Wednesday morning on Interstate 81 near Whitney Point, about 16 miles (26 kilometers) north of Binghamton. So far, they said, they have no leads.
"These animals have been through a lot, and people need to understand that this is not OK," said Amberly Ondria, shelter manager for the Broome County Humane Society. "This is not something that should be done."
The trucker told investigators that the dogs were thrown out of the right, rear window of a dirty, rusty Dodge Durango heading north toward Cortland.
State police said the trucker immediately stopped his big rig and brought the dogs to safety, scooping up the one that was severely injured while the other one, unscathed other than a few abrasions, followed on his own.
State troopers bandaged the badly injured dog and splinted his leg on the side of the highway, keeping him warm with a blanket and the trucker's sweatshirt. Meanwhile, the other dog gobbled half a box of dog biscuits.
The dogs were later renamed Trooper, for the state troopers who aided them, and Adam, after the trucker. Trooper is 6 to 8 years old, Ondria said. Adam is about a year old.
Trooper suffered a compound fracture of his distal radius and ulna on the front right leg that was amputated and a hairline fracture of the ulna on the left front leg, as well as broken ribs and contusions to his lungs and shoulder, the humane society said.
Because of the damage to his left leg, Trooper will require assistance getting around and perhaps even a harness to stabilize him, Ondria said.
"He has quite the road to recovery ahead of him," she said.
Follow Sisak at twitter.com/mikesisak and Walker at twitter.com/jwalkreporter


Here is a word to make you wise - you can really hit the fantastic favor mark with this owl design bookmark All of us at BabiesBabies love to sing the praises of bookmarks as favors. They're a great size, liked by everyone and they're destined to be used over and over again. So, when we add an adorable design like we did with this precious owl, we know we have a winner. And that's why this little character surely is a wise choice! Description and details: Each bookmark favor measures 3 " x 2.5" (6 " long including tassel) The charm is made of silver metal in the irresistible shape of a wise old owl with cutout details including big/friendly eyes, a feather-covered belly and more Attached through a loop at the top of the owl's head is a brown satin tassel The charm of the bookmark creates a page marker that slips into the book at the page you want marked, while the decorative tassel is visible from the outside Beautifully packaged in a clear topped box with a wood grain and brown base Box is tied with a white organza ribbon.


text:
<?php

namespace Teapotio\UserBundle\Repository;

use Teapotio\Base\UserBundle\Repository\UserRepository as BaseUserRepository;

use Doctrine\ORM\NoResultException;

use Doctrine\Common\Collections\ArrayCollection;

use Symfony\Component\Security\Core\Exception\UsernameNotFoundException;

class UserRepository extends BaseUserRepository
{

    /**
     * Get a collection of Users by user ids
     *
     * @param  array  $ids
     *
     * @return ArrayCollection
     */
    public function getByIds($ids)
    {
        $queryBuilder = $this->createQueryBuilder('u')
                             ->select(array('u', 'i', 'g', 's', 'fs'))
                             ->leftJoin('u.defaultAvatar', 'i')
                             ->leftJoin('u.groups', 'g')
                             ->leftJoin('u.settings', 's')
                             ->leftJoin('u.forumStat', 'fs');

        $queryBuilder->where($queryBuilder->expr()->in('u.id', $ids));

        return new ArrayCollection($queryBuilder->getQuery()->getResult());
    }

    /**
     * Overriding to include any joins
     *
     * @param  string $username
     *
     * @return UserInterface
     */
    public function loadUserByUsername($username)
    {
        $q = $this
            ->createQueryBuilder('u')
            ->select(array('u', 'us', 'ug', 'ufs'))
            ->where('u.username = :username OR u.email = :email')
            ->leftJoin('u.settings', 'us')
            ->leftJoin('u.groups', 'ug')
            ->leftJoin('u.forumStat', 'ufs')
            ->setParameter('username', $username)
            ->setParameter('email', $username)
            ->getQuery()
        ;

        try {
            // The Query::getSingleResult() method throws an exception
            // if there is no record matching the criteria.
            $user = $q->getSingleResult();
        } catch (NoResultException $e) {
            throw new UsernameNotFoundException(sprintf('Unable to find an active admin AcmeUserBundle:User object identified by "%s".', $username), null, 0, $e);
        }

        return $user;
    }

}

redpajama_set_name: RedPajamaGithub


What kind of gravel do I need?
Limestone is suitable for parking areas driveways and walkways, because it compacts and doesn't shift around as easily as gravel. Material used in these applications would be similar to trying to walk or drive through marbles. For drainage purposes our construction gravels would be best. For landscaping projects our washed gravel would be the best choice.
How do I order a delivery?
Determine what type of Gravel/Limestone/Sand you want to have delivered, the amount, when you want to have it delivered and contact us for delivery by calling 330-453-6365 or using out contact form provided.
Yes, we can. We can also simply dump on the apron of the drive if you prefer. Generally speaking, we pull on thousands of driveways per year with no complications. Rarely, a driveway has cracked. Our trucks weigh at least 10,000 pounds empty. Depending on what you are ordering, a fully loaded truck could weigh over 70,000 pounds. The construction of your drive is the main factor in determining if it can hold that kind of weight. We cannot be responsible for any driveway damage due to delivering material as instructed by you.
Can you "spread" the crushed gravel in my driveway?
Our drivers will do their best to spread your delivery, given the limitations they encounter at your location…. Overhead wires, trees, access, etc.
What is the average coverage per ton?
square feet at a depth of two inches*. Coverage decreases as the size of the aggregate increases.
What is the average coverage per ½ yard scoop?
A ½ yd scoop will cover about 70 square feet at a depth of two inches.
Crushed Run is a crushed limestone that has "fines", or limestone dust, mixed in. Crushed Run packs well and is ideal for driveways or as a substrate to create a level base for patios, walkways and retaining walls.
Which gravel should I use for a French drain?
#57 Limestone or Washed Gravel is commonly used for driveways and French drains. Water flows well through it, and the pieces are large enough so that they won't fall through the drainage holes in the pipe used for this type of drain.
What is the difference between masonry sand & coarse "concrete" sand?
make it a good choice for children's sandboxes or to put underneath the liner of an above-ground pool. Coarse sand is very much like beach sand. Applications vary, but it is used largely as the second layer (on top of the Crushed Run) in the base of a patio or walkway.
Besides driveways, drains and as a basis for patio construction, in what other ways can I use gravel or aggregates for landscaping?
Depending on the size of the aggregate, you can use them in dry creek beds, waterfalls, as garden accents, borders and for dog runs. Use larger river rocks under the eaves of your house to limit runoff and in low spots to reduce standing water. Carefully placed aggregates can reduce or eliminate erosion in areas with heavy water flow. Aggregates are inexpensive and have a variety of functions from practical to cosmetic.


What remains when the day rests in silence und the world holds its breath at night?
When light and sound are swallowed and we are embraced by darkness?
The Nightingale's song is the symbol for this book's overall mood.
Unexpected, sometimes bewildering and disturbingly beautiful, as is the night.
Pieces, fragments, schemes and shadows appear out of dusk before our eyes. Blinking we try to gain hold, try to focus…but too late, the moment passes, the image drowns in dream.


text:
HomePUP Taking Court Action for New Election in San Pedro
PUP Taking Court Action for New Election in San Pedro
/ Mar 09, 2018
/Dorian Nuñez
/ views
Embed video:
In a statement released by PUP Belize Rural South and PUP Mayoral Candidate Andre Perez, he made it clear this afternoon, Friday, March 9, 2018, that his party cannot concede defeat at the municipal elections that were carried out on Wednesday, March 7, 2018.
Attorney at Law Mr. Eamon Courtney stated that after reviewing the official papers that were signed off by the Elections and Boundaries Commission that there are 275 ballots that cannot be accounted for, at minimum. He stated that 275 missing ballots puts the elections at dispute and thus the party will go to court.
"There needs to be a new election in San Pedro and that is what we will be fighting for," commented legal advisor the the PUP, Attorney Mr. Eamon Courtney to Ambergris Today. "Briefing with the party leader, the decision has been taken in consultation with the San Pedro Branch of the Party, that we are moving forwards with the courts because we believe that we have been robbed by the elections in San Pedro."
"Our numbers are showing that we won the elections," continued Courtney. "And so the party is mobilizing all its resources to fight. We are going to fight for every vote and we expect as a result of the recount and the re-election, there will be a PUP Town Council in San Pedro.
Below is a statement given out by PUP Mayoral Candidate Andre Perez
Dear residents of San Pedro,
First of All, on behalf of the PUP7, I would like to say a big thank you and that we are extremely grateful for your overwhelming support on March 7 and all the messages and greetings that continue to pour in.
We want to share with you all that we firmly believe that there is more than enough evidence to support that major discrepancies occurred on Election Day. Because of this, I owe it to the voters of San Pedro to state that we CANNOT concede defeat. Any further decisions or actions to be taken are now in the hands of our National Executive and legal advisors.
Andre Perez
Mayoral Candidate of San Pedro PUP7
Related Article: Will There be a Recount of San Pedro Ballots? PUP Discusses Options
Click Here for More News on Ambergris Today Online
Coastal Zone Management Participates in Plastic Pollution Workshop
Dorian Nuñez
Celebrity Talk Show Hosts of MoJoe on Return Visit to San Pedro, Belize
Summer Camp Activity at Goff's Caye, Belizean Children Enjoy
Kelly McGuire Concerts to Raise Funds for unBELIZEable II 2016 Wheelchair Distribution


text:
\section{Introduction and summary} \label{sec:intro}
When immersed in an external tidal field, a self-gravitating object gets deformed. The ``susceptibility'' to a tidal
deformation is measured by the so-called tidal Love numbers~(TLNs)~\cite{Murraybook,PoissonWill}, which depend on the
internal structure of the deformed body. The TLNs play a crucial role in gravitational-wave (GW) astronomy, most notably
to: i) constrain the equation of state~(EoS) of neutron stars~(NSs) through GW measurements of the tidal deformability
in the last stages of the
inspiral~\cite{Baiotti:2010xh,Baiotti:2011am,Vines:2011ud,Pannarale:2011pk,Vines:2010ca,Lackey:2011vz,Lackey:2013axa,
  Favata:2013rwa,Yagi:2013baa,Maselli:2013mva,Maselli:2013rza,DelPozzo:2013ala,TheLIGOScientific:2017qsa,Bauswein:2017vtn,
  Most:2018hfd,Harry:2018hke,Annala:2017llu,EoS-GW170817,Akcay:2018yyh} (see
Refs.~\cite{GuerraChaves:2019foa,Chatziioannou:2020pqz} for some recent reviews);~ii) constrain alternative theories of
gravity in an EoS-independent fashion~\cite{Yagi:2013awa,Yagi:2013bca} (see Ref.~\cite{Yagi:2016bkt} for a review);~iii)
test the nature of black holes with GW observations~\cite{Cardoso:2017cfl,Pani:2019cyc} (see Ref.~\cite{Cardoso:2019rvt}
for a review).

Clearly, the recent detections of coalescing NSs by LIGO/Virgo~\cite{TheLIGOScientific:2017qsa,Abbott:2020uma} give
strong motivation for further developments on this topic.  In particular, several binary NSs and mixed black
hole-NS binaries will be detected in the future
LIGO/Virgo observation runs, possibly with higher signal-to-noise ratio than GW170817. While this will allow to put
better constraints on the NS TLNs (and hence on the NS EoS), it makes it also urgent to develop waveform models that can
accurately take into account all possible effects related to the tidal deformability of
NSs~\cite{Abdelsalhin:2018reg,Jimenez-Forteza:2018buh,Banihashemi:2018xfb,Dietrich:2019kaq,Dietrich:2020eud,
  Henry:2020ski}.

Surprisingly, more than ten years after the seminal work by Flanagan and
Hinderer~\cite{Flanagan:2007ix,Hinderer:2007mb}, some properties of the TLNs are still being discovered and are still
not totally understood, in particular for what concerns the magnetic\,\footnote{The TLNs can be divided into two
  categories: \emph{electric} (or even parity), which are related to the mass multipole moments induced by the tidal
  field; and \emph{magnetic} (or odd parity), which are related to the induced current multipole moments and do not have
  an analog in Newtonian theory. See below for a formal definition.}
TLNs~\cite{Pani:2018inf,Poisson:2020mdi}. Furthermore, it was recently realized that the magnetic TLNs depend also on
the assumptions on the dynamics of the fluid within the star, namely whether the fluid is irrotational or static (see
Sec.~\ref{subsec:statirr} for explicit definitions), with the former assumption being more physically
sound~\cite{Landry:2015cva,Landry:2015snx,Pani:2018inf}\,\footnote{We shall call static (irrotational) Love numbers
  those associated with a static (irrotational) fluid.}.
In this context, most of previous work on the tidal deformability had focused on nonspinning objects.
In recent years, there has been remarkable progress in extending the analysis to spinning compact objects.
The coupling between the object's angular momentum and the external tidal field introduces new families of so-called ``rotational''
TLNs~(RTLNs)~\cite{Pani:2015nua,Landry:2015cva,Landry:2015zfa,Landry:2017piv,Gagnon-Bischoff:2017tnz}.
Tidal deformations of slowly-spinning black holes were studied in Refs.~\cite{Poisson:2014gka,Pani:2015hfa}, which found
that the (R)TLNs of a black hole are zero~\cite{Binnington:2009bb,Damour:2009vw,Damour:2009va,Gurlebeck:2015xpa,Porto:2016zng,Hui:2020xxx,Charalambous:2021kcz} also in the
spinning case, at least to quadratic order in the spin in the axisymmetric case~\cite{Pani:2015hfa,Pani:2015nua} (see
also~\cite{Landry:2015cva,Landry:2015zfa}). Recently, using analytical-continuation
methods, it has been shown~\cite{LeTiec:2020spy} that the tidal field affects the non-axisymmetric multipole moments of a spining BH, already to linear order in the spin. As remarked in~\cite{Chia:2020yla}, the
non-vanishing quantities found in~\cite{LeTiec:2020spy} are associated with dissipative interactions, usually referred
to as tidal heating~\cite{Hartle:1973zz,PhysRevD.64.064004}. As argued in~\cite{Chia:2020yla}, the non dissipative (R)TLNs of a
Kerr black hole are identically zero, providing an ideal baseline for tests of the Kerr hypothesis with
GWs~\cite{Cardoso:2017cfl}. More generally, recent results~\cite{Poisson:2020mdi,Poisson:2020vap} show that, when the
tidal field depends on time or is not axisymmetric, the general picture of TLNs is more complicated than previously
expected. In this article we shall only consider a stationary, axisymmetric tidally deformed star, leaving the more
general case to a future analysis~\cite{inprep}.

Computing the RTLNs is rather involved, since it requires to work out the linear (gravitational and fluid) perturbations
of a spinning compact object and to solve the corresponding coupled system numerically.  Thus, it might not be
surprising that preliminary numerical computations of the RTLNs by different groups did not agree with each other.  In
particular, the analysis in Ref.~\cite{Gagnon-Bischoff:2017tnz} found disagreement with the RTLNs previously computed by
some of us~\cite{Pani:2015nua} (hereafter, Paper~I), especially for low-compactness NSs. We have found that the source of
disagreement is twofold. First, we have found an error in the numerical implementation of the equations in
Paper~I (now corrected in the computation presented below).
Second, the authors of~\cite{Gagnon-Bischoff:2017tnz} studied the irrotational RTLNs, arguing that in some cases they
coincide with the static RTLNs studied in Paper~I.  However, in general the irrotational RTLNs cannot be computed under
the assumption of stationarity. Properly including (slowly-varying) tidal perturbations allows to resolve the ambiguity
found in Ref.~\cite{Gagnon-Bischoff:2017tnz} and gives different irrotational RTLNs that do not coincide with the static
ones (although the differences are smaller than $5\%$). This point will be discussed in detail in a separate
publication~\cite{inprep}\,\footnote{By correcting the numerical implementation of Paper~I and integrating the field
  equations obtained with the assumptions of~\cite{Gagnon-Bischoff:2017tnz}, we find perfect agreement between the two
  approaches, up to numerical errors.}, while in this article we focus on the {\it static} RTLNs.

Although NS coalescing binaries are expected to have irrotational perturbations, static perturbations are useful to
elucidate a surprising feature of the RTLNs which we unveil in this work. Paper~I introduced \emph{four} independent
RTLNs to fully characterize the (quadrupolar and octupolar) tidal deformability of a spinning NS to linear order in the
spin and in the axisymmetric case, while the effective-field-theory Lagrangian developed in
Ref.~\cite{Abdelsalhin:2018reg} (hereafter, Paper~II) contains only \emph{two} parameters that govern the coupling
between the (quadrupolar and octupolar) tidal deformations of the body, its spin and the external tidal
field.  Thus, as argued in Paper~II, the Lagrangian approach seems to predict that the four RTLNs are not independent:
they should be related by two algebraic relations, and in fact two of them are simply proportional to the other two.

From a Lagrangian point of view it is natural to expect that opposite sectors are
coupled to each other. Indeed, a single interaction term in the schematic form
\begin{equation}
 {\cal L}({\cal A},\partial{\cal A},{\cal P},\partial{\cal P}) \supset  \alpha {\cal A} {\cal P}\,, \label{LagrangianCoupling}
\end{equation}
in the Lagrangian ${\cal L}$ gives rise --~using Euler-Lagrange equations~-- to related
coupling terms in the field equations for ${\cal A}$ and ${\cal P}$ which are both proportional to the single coupling constant
$\alpha$.

It is natural to ask whether similar relations are satisfied by the RTLNs, which are computed by solving the perturbation
equations of a single NS perturbed by a generic tidal source. Our analysis shows that this is indeed the case: we
computed static RTLNs (as we discuss in this paper, the Lagrangian constructed in Paper~II describes only {\it static}
perturbations) with different parities for various choices of the EoS and of the compactness, finding that the algebraic
relations derived in Paper~II are always satisfied, within the numerical errors, for low compactness and for any EoS (see
Fig.~\ref{fig:ratios}). When the compactness is large, there is still an EoS-independent (within numerical errors) relation between the RTLNs, but it deviates from the theoretical value predicted in Paper~II by up to~$6\%$.

These relations --~which are exact for low compactness and any EoS~-- imply the
existence of a ``\emph{hidden symmetry}'' among perturbations with even and odd parities.
We use the term ``hidden symmetry'', which is stronger than ``universal relation'' (see~\cite{Yagi:2016bkt} for a
review) because, besides being EoS-independent within numerical uncertaintys, this symmetry is theoretically predicted by
a Lagrangian post-Newtonian (PN) approach.
Nonetheless, we stress that this hidden symmetry is truly unexpected and nontrivial from a perturbation-theory point of
view: the RTLNs that turn out to be proportional to each other belong to opposite parity sectors, so there is {\it a priori}
no reason why they should be related.
This is analogous to the symmetry between axial and polar
perturbations of a Schwarzschild black hole found by Chandrasekhar~\cite{Chandrasekhar:1985kt}, with the major
difference that the perturbation equations of compact stars depend on the EoS, making an analytical interpretation much
more challenging than in the case of black holes.  We argue that this symmetry should also affect irrotational
perturbations, although in that case it is likely to appear in a more involved form, requiring a more detailed study in
order to be elucidated~\cite{inprep}. In the case of large compactness, the hidden symmetry is only approximate, but an accurate
universal relation is still present.

The rest of this paper is organized as follows. In Sec.~\ref{sec:previous} we review Paper~I --~where the RTLNs are
introduced and the procedure for their numerical computation in terms of perturbations of a stationary NS is
described~-- and Paper~II --~where the effective Lagrangian describing two tidally interacting NSs is discussed. We also
briefly discuss, in Sec.~\ref{subsec:statirr}, the difference between static and irrotational perturbations.  Then, in
Sec.~\ref{sec:results} we discuss the numerical computation of the (static) RTLNs, showing that the afrorementioned
hidden symmetry is satisfied for different choices of the EoSs and of the compactness. We conclude in
Sec.~\ref{sec:conclusions}, where some open issues are discussed. Appendix~\ref{app:RTLNs} gives the explicit
expressions of the coefficients appearing in the perturbation equations, and Appendix~\ref{app:conversion} gives the
conversion factors between different (R)TLNs used in the literature.

\subsection{Notation and conventions}\label{subsec:notation}

We denote the speed of light in vacuum by $c$ and set the gravitational constant $G=1$.
We shall mostly use units such that $c=1$, unless explicitly stated.
Latin indices run over three-dimensional spatial coordinates and are contracted with the Euclidean flat metric
$\delta_{ij}$; the antisymmetric Levi-Civita symbol in the Euclidean space is denoted by $\epsilon^{ijk}$. Greek indices
run over four-dimensional, spacetime coordinates.

Following the notation in~\cite{Thorne:1980ru} (see also~\cite{poisson2014gravity}), we use capital letters in the
middle of the alphabet $L,K$, etc., as shorthand for sets of indices $a_1\dots a_l$, $b_1\dots b_k$, etc. Round $()$,
square $[]$, and angular $\langle\rangle$ brackets enclosing the indices indicate symmetrization, antisymmetrization,
and trace-free symmetrization, respectively.  We call symmetric trace-free (STF) those tensors $T^{a_1\cdots a_l}$ that
are
symmetric on all indices and whose contraction of any two indices vanishes. For a generic vector $u^a$ we define
$u^{ab\cdots c}=u^au^b\dots u^c$ and $u^2=u^au^a$.

Functions and tensor fields on the two-sphere can be expanded in terms of tensor spherical harmonics: the scalar
spherical harmonics $Y^{l m}(\theta,\varphi)$, the vector spherical harmonics with even and odd parity, $(Y^{l
  m}_{,\theta},Y^{l m}_{,\varphi})$ and $(S^{l m}_\theta,S^{l m}_\varphi)=(-Y^{l
  m}_{,\varphi}/\sin\theta,\sin\theta Y^{l m}_{,\theta})$ respectively, etc. They can also be expanded in terms of
the STF tensors $n^L=n^{a_1}\cdots n^{a_l}$, where $n^a=(\sin\theta\cos\phi,\sin\theta\sin\phi,\cos\theta)$. Indeed,
$Y^{l m}(\theta,\phi)={\cal Y}^{l m}_{a_1\cdots a_l}n^{a_1\cdots a_l}$, where ${\cal Y}^{l m}_{a_1\cdots a_l}$
are constant coefficients.  Thus, any function $f(\theta,\phi)$ can be expanded as
\begin{equation}
f(\theta,\varphi)=\sum_{lm}f^{lm}Y^{lm}(\theta,\varphi)=\sum_lf_{a_1\cdots a_l}n^{a_1\cdots
a_l}(\theta,\varphi)\,,\label{eq:harmstf}
\end{equation}
therefore $f_{a_1\cdots a_l}=\sum_mf^{lm}{\cal Y}^{l m}_{a_1\cdots a_l}$.

We denote the Geroch-Hansen multipole moments~\cite{Geroch:1970cd,Hansen:1974zz} by $M^L$ (mass) and $J^L$ (current),
and
the Thorne multipole moments~\cite{Thorne:1980ru} by $Q^L$ (mass) and $S^L$ (current), see
also~\cite{Cardoso:2016ryw}. They are related by~\cite{1983GReGr..15..737G}
\begin{align}
M^L&=(2l-1)!!Q^L\,,\nonumber\\
J^L&=\frac{2l}{l+1}(2l-1)!!S^L\,.
\end{align}
We remind that the Geroch-Hansen multipole moments are defined in a coordinate-independent way, as tensors at infinity
generated by a set of potentials, while the Thorne moments are defined in terms of the asymptotic behvior of the
spacetime metric in asymptotically Cartesian mass-centered coordinates. We shall mostly use the Geroch-Hansen
definition.

When the spacetime is symmetric with respect to an axis $\hat k$, the multipole moments can be written as $M^{i_1\cdots
  i_l}=(2l-1)!!M_lk^{i_1\cdots i_l}$, $J^{i_1\cdots i_l}=(2l-1)!!J_lk^{i_1\cdots i_l}$, and thus
\begin{align}
  Q^{i_1\cdots i_l}&=M_lk^{i_1\cdots i_l}\nonumber\\
  S^{i_1\cdots i_l}&=\frac{l+1}{2l}J_lk^{i_1\cdots i_l}\label{eq:transfmult}\,.
\end{align}
  %
In this case, under the further assumption of symmetry with respect to the equatorial plane, the nonvanishing mass
multipole moments have even $l$, and the nonvanishing current multipole moments have odd $l$. When the spacetime is
axial and equatorial symmetric, the Geroch-Hansen multipole moments can be also computed using Ryan's
approach~\cite{Ryan:1995wh}, in terms of the geodesic properties of the spacetime metric.

The mass of a body and its angular momentum coincide with their $l=0$ mass and $l=1$ current multipole moments,
$M=M^0=Q^0$, $J=\sqrt{J^i J^i}=\sqrt{S^iS^i}$, respectively. We also define the dimensionless spin parameter of the body
as $\chi=J/M^2$, and the compactness as $C=M/R$, where $R$ is the stellar radius, defined by the location in which the
pressure of the fluid inside the star vanishes. Derivatives with respect to $t$ and $r$ are denoted with an overdot and
a prime, respectively.
\section{Review of previous work} \label{sec:previous}
Here we summarize the results of Paper~I and Paper~II. Since the notations and formalisms of these two papers are
different, we need to describe them in some detail, in order to compare, in Sec.~\ref{sec:results}, the results of the
numerical computation of the RTLNs, performed in the framework of Paper~I, with the theoretical predictions of Paper~II.

We remark that RTLNs have also been introduced, with a different notation,
in~\cite{Landry:2015cva,Landry:2015snx,Landry:2015zfa,Poisson:2016wtv,Landry:2017piv,Gagnon-Bischoff:2017tnz}, which
focus on the irrotational RTLNs.  A complete treatment of the irrotational RTLNs requires including slowly-varying
perturbations and will be discussed in details in a forthcoming publication~\cite{inprep}.

\subsection{Pani et al. (Paper~I)}\label{sec:pani}
In Paper~I (see also Ref.~\cite{Pani:2015hfa}), tidal deformations of rotating compact stars are
studied by
considering stationary perturbations of a stationary, rotating star up to linear order in the spin (i.e.
neglecting ${\cal O}(\chi^2)$ terms).
The perturbed metric can be written as $g_{\mu\nu}=g^{(0)}_{\mu\nu}+\delta g_{\mu\nu}$, where $g^{(0)}_{\mu\nu}$ is
the background, whereas $\delta g_{\mu\nu}$ is the tidal perturbation.
The background is described by Hartle's metric~\cite{Hartle:1967he,Thorne:1984mz}):
\begin{align}
  ds^{(0)\,2}&=g^{(0)}_{\mu\nu}dx^\mu dx^\nu=-e^\nu dt^2+e^\lambda dr^2 \nonumber\\
  &-2\sin^2\theta\omega r^2dtd\varphi+r^2d\Omega^2\,,
\end{align}
where $x^\mu=(t,r,\theta,\varphi)$, $d\Omega^2=d\theta^2+\sin^2\theta d\varphi^2$, $e^\lambda=(1-2{\cal M}/r)^{-1}$, and
the (radial) metric functions satisfy the set of ordinary differential equations:
\begin{align}
{\cal M}'&=4\pi r^2 P\,,\\
  \nu'&=\frac{2{\cal M}+4\pi r^2P}{(r-2{\cal M})}\,,\\
    P'&=-\frac{P+\rho}{2}\nu'\,,\\
{\tilde\omega}''&=\frac{4\pi r(P+\rho)(r{\tilde\omega}'+4\tilde\omega)}{r-2{\cal M}}-\frac{4}{r}{\tilde\omega}'\,,
\end{align}
where $\tilde\omega=\Omega-\omega$, $\Omega$ is the fluid angular velocity, $P(r)$ and $\rho(r)$ are the pressure
and energy density of the fluid, respectively. The background four-velocity of the fluid is
$u^{(0)\mu}=e^{-\nu/2}(1,0,0,\Omega)$ and its stress-energy tensor is $T^{(0)\mu\nu}=(\rho+P)u^\mu
u^\nu+Pg^{(0)\mu\nu}$.  In vacuum, ${\cal M}(r)=M$ and $\omega(r)=2J/r^3$.

The perturbations of the metric and of the fluid
four-velocity are expanded in tensor spherical harmonics, and are decomposed in even (or electric, or polar) and odd (or
magnetic, or axial) perturbations: $\delta g_{\mu\nu}=\delta g^{\rm (even)}_{\mu\nu}+\delta g^{\rm (odd)}_{\mu\nu}$,
with
(in the Regge-Wheeler gauge~\cite{regge:1957td})
\begin{align}
  \delta g_{\mu\nu}^{\rm (even)}dx^\mu dx^\nu&=e^\nu H_0^{lm}Y^{lm} dt^2+2H_1^{lm}Y^{lm} dtdr\label{expansion_h}\\
  &+H_2^{lm}Y^{lm} dr^2\,,\nonumber\\
  \delta g_{\mu\nu}^{\rm (odd)}dx^\mu dx^\nu&=(h_0^{lm}dt+h^{lm}_1dr)(S_\theta^{lm} d\theta+S_\phi^{lm}
  d\varphi)\,,\nonumber
\end{align}
and $u^\mu=u^{(0)\mu}+\delta u^\mu$. In Paper~I the perturbations were assumed to be {\it static} (see
Sec.~\ref{subsec:statirr}), i.e. $\delta g_{\mu\nu,0}=0$ and $\delta u^i=0$ ($i=1,2,3$).  Thus, the perturbations with
even parity are described by the functions $(H_0(r)^{lm}(r),H_1^{lm}(r),H_2^{lm}(r),K^{lm}(r))$, and those with odd
parity are described by the functions $(h_0^{lm}(r),h_1^{lm}(r))$. It was also assumed that the perturbations are
axisymmetric, and thus they have $m=0$ (with symmetry axis parallel to the body's angular momentum); we remark that
$m\neq0$ tidal perturbations of a spinning object would induce precession and hence a weak time-dependence of the
perturbed system~\cite{Thorne:1997kt}. Thus, assuming static perturbations implies $m=0$.

The field equations at first order in the spin mix the perturbations having a given (polar or axial) parity and harmonic
index $l$ with those having opposite parity and harmonic index $l\pm1$ (see Ref.~\cite{Pani:2013pert} for a
review). Thus, it is possible to define ``polar-led'' and ``axial-led'' perturbations; the former are induced by a
purely electric tidal field, the latter by a purely magnetic tidal field. The polar-led system has the form (leaving
implicit the index $m=0$)
\begin{align}
{\cal D}^{{\rm pol}\,(l)}[H_0^{l}]&=0\,,\nonumber\\
{\cal D}^{{\rm ax}\,(l+1)}[h_0^{l+1}]&=S_+^{{\rm pol}\,(l)}[H_0^{l}]\,,\nonumber\\
{\cal D}^{{\rm ax}\,(l-1)}[h_0^{l-1}]&=S_-^{{\rm pol}\,(l)}[H_0^{l}]\,
\label{eq:polarled}
\end{align}
where
\begin{align}
  {\cal D}^{{\rm pol}\,(l)} H_0^l &= \frac{d^2 H_0^l}{dr^2} + C_1^{{\rm pol}\,(l)}(r) \frac{d H_0^l}{dr} +
  C_0^{{\rm pol}\,(l)}(r)H_0^l
	\label{eq:dpol}\\
	      {\cal D}^{{\rm ax}\,(l)} h_0^l& = \frac{d^2 h_0^l}{dr^2} + C_1^{{\rm ax}\,(l)}(r) \frac{d h_0^l}{dr} +
              C_0^{{\rm ax}\,(l)}(r)h_0^l\,.
	\label{eq:dax}
\end{align}
The perturbation $H_0^{l}$ is at zero order in the spin, while the perturbations $h_0^{l\pm1}$ are at first order in the
spin, and vanish in the $\Omega\to0$ limit. The other perturbation functions can be obtained from $H_0^{l}$ and
$h_0^{l\pm1}$ through algebraic relations. Similarly, the axial-led system has the form
\begin{align}
{\cal D}^{{\rm ax}\,(l)}[h_0^{l}]&=0\,,\nonumber\\
{\cal D}^{{\rm pol}\,(l+1)}[H_0^{l+1}]&= S_+^{{\rm ax}\,(l)}[h_0^{l}]\,,\nonumber\\
{\cal D}^{{\rm pol}\,(l-1)}[H_0^{l-1}]&= S_-^{{\rm ax}\,(l)}[h_0^{l}]\,.\label{eq:axialled}
\end{align}
In this case $h_0^{l}$ is at zero order in the spin, while the perturbations $H_0^{l\pm1}$ are at first order in the
spin, and vanish in the $\Omega\to0$ limit. The explicit forms of the coefficients $C_{0,1}^{{\rm pol}\,(l)}$,
$C_{0,1}^{{\rm ax}\,(l)}$ and of the sources $S^{{\rm pol}\,(l)}_\pm$, $S^{{\rm ax}\,(l)}_\pm$ is given in
Appendix~\ref{app:RTLNs}.  The other perturbation functions can be obtained from $h_0^{l}$ and $H_0^{l\pm1}$ through
algebraic relations.

The source of the perturbations is an asymptotic tidal field, described by the electric and magnetic tidal tensors,
${\cal E}^{(l)}_m$ and ${\cal B}^{(l)}_m$, respectively. The leading-order asymptotic expansion of the metric (as $r\gg
M$) in terms of these tensors reads:
\begin{align}
g_{tt}&\to-\sum_{l\ge2,m}\frac{2}{l(l-1)}{\cal E}^{(l)}_mY^{lm}(\theta)r^l\nonumber\\
g_{t\varphi}&\to\sum_{l\ge2}\frac{2}{3l(l-1)}{\cal B}^{(l)}_mS_\varphi^{lm}(\theta)r^{l+1}\,.\label{eq:defcEcB}
\end{align}
In the case of an axisymmetric perturbation, only the $m=0$ tidal fields, ${\cal E}^{(l)}_0$, ${\cal B}^{(l)}_0$,
contribute.  Note that the metric~\eqref{eq:defcEcB} is not asymptotically flat. Indeed, it only describes the
spacetime at $r\lesssim r_{\rm ts}$ where $r_{\rm ts}$ is the location of the generic source of the tidal field.

As a result of the tidal field, the mass and current multipole moments are deformed; in linear perturbation theory,
these deformations are proportional to the tidal fields themselves.  At zero-th order in the spin, the electric
(magnetic) tidal field affects the mass (current) multipole moment with the same value of $l$. The proportionality
constants
\begin{align}
  \lambda^{(l)}_E&\equiv\frac{\partial M_l}{\partial{\cal E}^{(l)}_{0}}\,,\nonumber\\
  \lambda^{(l)}_M&\equiv\frac{\partial J_l}{\partial{\cal B}^{(l)}_{0}}\,,\label{eq:defTLN}
\end{align}
are the {\it relativistic TLNs}~\cite{Damour:2009vw,Binnington:2009bb}.  At first order in the spin, the tidal field
with a given parity and harmonic index $l$ affects the tidal field with opposite parity and harmonic index $l\pm1$. The
proportionality constants
\begin{align}
\lambda_E^{(ll')}&=\frac{\partial M_l}{\partial{\cal B}^{(l')}_{0}}\,,\nonumber\\
\lambda_M^{(ll')}&=\frac{\partial J_l}{\partial{\cal E}^{(l')}_{0}}\,,\label{eq:defRTLN}
\end{align}
with $l'=l\pm1$, are called {\it relativistic RTLNs}, see e.g. Paper~I
and~\cite{Pani:2015hfa,Landry:2015cva,Landry:2015zfa}.

Since $[{\cal E}^{(l)}_0]=[{\cal B}^{(l)}_0]=({\rm mass})^{-l}$,
$[M_l]=[J_l]=({\rm mass})^{l+1}$, and the RTLNs are
proportional to the dimensionless spin, the {\it dimensionless} TLNs and RTLNs can be defined as
\begin{align}
\tilde{\lambda}^{(l)}_{E/M}&\equiv\frac{\lambda^{(l)}_{E/M}}{M^{2l+1}}\,,\nonumber\\
\tilde{\lambda}^{(ll')}_{E/M}&\equiv\frac{\lambda^{(ll')}_{E/M}}{\chi M^{l+l'+1}}\,.
\end{align}
Note that the dimensionless RTLNs defined above are also independent of the spin.
In terms of these quantities, the axisymmetric deformations of the quadrupole and octupole
moments, to linear order in the tidal tensor and to linear order in the spin, are:
\begin{align}
  \frac{M_2}{M^3}&=\tilde{\lambda}^{(2)}_E \tilde{\cal E}^{(2)}_0+\chi\tilde\lambda^{(23)}_E\tilde{\cal B}_0^{(3)}\nonumber\\
  \frac{M_3}{M^4}&=\tilde{\lambda}^{(3)}_E\tilde{\cal E}^{(3)}_0+\chi\tilde\lambda^{(32)}_E\tilde{\cal B}_0^{(2)}\nonumber\\
  \frac{J_2}{M^3}&=\tilde{\lambda}^{(2)}_M\tilde{\cal B}^{(2)}_0+\chi\tilde\lambda^{(23)}_M\tilde{\cal E}_0^{(3)}\nonumber\\
  \frac{J_3}{M^4}&=\tilde{\lambda}^{(3)}_M\tilde{\cal B}^{(3)}_0+\chi\tilde\lambda^{(32)}_M\tilde{\cal E}_0^{(2)}\,,
  \label{eq:adiabrelp}
\end{align}
where we defined the dimensionless tidal tensors $\tilde {\cal E}^{(l)}_m ={\cal E}^{(l)}_m M^l$ and $\tilde {\cal
  B}^{(l)}_m ={\cal B}^{(l)}_m M^l$.  Note that if the system is symmetric  with respect to the equatorial plane, $M_3=J_2={\cal
  E}_0^{(3)}={\cal B}_0^{(2)}=0$.

The Love numbers can be computed by solving the systems in Eqs.~\eqref{eq:polarled} and \eqref{eq:axialled} for $l=2,3$
with the tidal sources
${\cal E}^{(2)}_0$, ${\cal E}^{(3)}_0$, ${\cal B}^{(2)}_0$, ${\cal B}^{(3)}_0$. The analytic solution oustide the star
has been explicitly derived in Ref.~\cite{Pani:2015hfa}, in terms of a set of integration constants. Solving the equations
inside the star, with the assumptions of regularity at the center and smooth boundary conditions at the surface $r=R$ of
the star, fixes the integration constants, and thus gives the explicit value of the TLNs and of the RTLNs, which depend
on the EoS of the star.

\subsection{Abdelsalhin et al. (Paper~II)}\label{sec:abdelsalhin}
In Paper~II (see also Ref.~\cite{Abdelsalhin:2019ryu}), the leading-order contribution of the RTLNs to the PN waveform
of coalescing compact binaries was computed, together with the spin corrections to the tidal deformability terms. These
terms appear at $6.5$PN order (i.e., they are suppressed by a factor $v^{13}$, where $v$ is the orbital velocity of the
binary) relative to the leading-order contribution to the GW phase (and by a factor $v^3$ relative to the
leading-order TLN term entering at $5$PN order); they are obtained by generalizing previous
results~\cite{Vines:2010ca,Vines:2011ud}, where the $6$PN tidal term in the GW phase of nonrotating compact coalescing
binaries was derived.

The motion of the binary is described in terms of a Lagrangian function
\begin{equation}
{\cal L}={\cal L}(z^i,{\dot z}^i,{\ddot z}^i,M_A,J_A,Q^L_A,{\dot Q}^L_A,S^L_A,{\dot S}^L_A)\,.
\end{equation}
Here $z^i=z^i_1-z_2^i$ is the relative position of the binary in the harmonic, conformally Cartesian coordinate frame
(defined everywhere outside the strong-field region of the compact bodies) in which the PN approximation is defined; an
overdot denotes a derivative with respect to the coordinate time in this frame; the index $A=1,2$ refers to the two
bodies in the binary\,\footnote{Note that units used in Paper~II are such that $G=1$, while the speed of light $c$ is
retained as a dimensionful quantity in order to keep track of the different PN orders (terms of the $n$-th PN order are
$O(c^{-2n})$).}.

Each body is characterized by its mass $M_A$, by its angular momentum $J_A$ and by the higher-order multipole moments
$Q_A^L$, $S_A^L$ (with $l\ge2$), using Thorne's definition (see Sec.~\ref{subsec:notation}), which are induced by the
tidal field of the companion. The multipole expansion is truncated to the octupole $(l=3)$, and the rotation is included
at first order in the spin. The next-to-leading order quadrupolar contributions are included, whereas the octupolar
contributions are truncated at the leading order. This truncation is sufficient to determine the tidal waveform up to
$6.5$PN order. Moreover, for simplicity the quadrupole and octupole moments of body~$1$ are set to zero, thus including
only the multipole moments induced from body~$1$ to body~$2$; the moments induced from body~$2$ to body~$1$ can be
obtained {\it a posteriori} with a simple exchange of indices. Thus, the quadrupole and octupole moments are simply
denoted as $Q^L\equiv Q_2^L$ and $S^L\equiv S_2^L$, respectively.

The Lagrangian can be written as the sum of an orbital Lagrangian, which depends on the orbital motion and on the
multipole moments, and an internal Lagrangian, which depends on the internal degrees of freedom of body~$2$ only:
\begin{align}
  {\cal L} &= {\cal L}_{\rm orb}(z^i,{\dot z}^i,{\ddot z}^i,M_A,J_A,Q^{ab},{\dot
Q}^{ab},Q^{abc},S^{ab},S^{abc})\nonumber\\
  &+{\cal L}_2^{\rm int}(Q^{ab},Q^{abc},S^{ab},S^{abc})\,.
\label{eq:lagrangian}
\end{align}
We remark that the terms in ${\dot Q}^{ab}$ in ${\cal L}_{\rm orb}$ contribute to the next-to-leading order corrections
to the gravitational waveform. The time derivatives of the other moments are subleading.

The expression of the orbital Lagrangian is uniquely determined by imposing that its variation with respect to the
coordinate separation leads to the PN orbital equations of motion. The variation of the orbital Lagrangian with respect
to the multipole moments gives the electric and magnetic tidal tensors, which are denoted by $G^L$ and $H^L$,
respectively:
\begin{align}
G^{ab}&=\frac{\partial{\cal L}_{\rm orb}}{\partial Q^{ab}}  -\frac{d}{dt}\frac{\partial{\cal L}_{\rm orb}}{\partial
{\dot Q}^{ab}}
\nonumber\\
G^{abc}&=\frac{\partial{\cal L}_{\rm orb}}{\partial Q^{abc}}\nonumber\\
H^{ab}&=\frac{\partial{\cal L}_{\rm orb}}{\partial S^{ab}}\nonumber\\
H^{abc}&=\frac{\partial{\cal L}_{\rm orb}}{\partial S^{abc}}\,,\label{eq:deftidaltensors}
\end{align}
and are defined, as in Paper~I, from the asymptotic behavior of the metric around each of the bodies
composing the system. For each body one can define a ``buffer region'', far enough from the body so that the
gravitational field is weak, but close enough so that the effect of the other body appears as a tidal field. In the
buffer region around the body~$A$, $x^i=z_A^i+y^i$, and the tidal contribution to the metric is (see Eqs.~(1.63), (1.76)
in Paper~II):
\begin{align}
g_{tt}&=\dots+\sum_{l\ge2,m}\frac{2}{l!}G^{lm}Y^{lm}(\theta)r^l\nonumber\\
g_{ti}&=\dots-\sum_{l\ge2,m}\frac{1}{(l+1)!}H^{lm}S_\varphi^{lm}(\theta)r^{l+1}\,,\label{eq:defcEcB2}
\end{align}
where $G^{lm}Y^{lm}=G^{a_1\cdots a_l}n^{a_1\cdots a_l}$, $H^{lm}Y^{lm}=G^{a_1\cdots
  a_l}n^{a_1\cdots a_l}$, see Eq.~\eqref{eq:harmstf}. Note that this is equivalent to Eq.~\eqref{eq:defcEcB} but with a
different notation, see Appendix~\ref{app:conversion}.

At first order in the perturbation, the multipole moments are linear in the tidal tensors which induce them; at linear
order in the spin, they can be written (keeping factors of $c$ for clarity)
\begin{align}
Q^{ab}&=\lambda_2 G^{ab}+\frac{\lambda_{23}}{c^2}J^cH^{abc}\,,\nonumber\\
Q^{abc}&=\lambda_3 G^{abc}+\frac{\lambda_{32}}{c^2}J^{<c} H^{ab>}\,,\nonumber\\
S^{ab}&=\frac{\sigma_2}{c^2} H^{ab}+\sigma_{23}J^cG^{abc}\,,\nonumber\\
S^{abc}&=\frac{\sigma_3}{c^2} H^{abc}+\sigma_{32}J^{<c} G^{ab>}\,,\label{eq:adiabatic}
\end{align}
where $\lambda_l$, $\sigma_l$ are the electric and magnetic TLNs, and $\lambda_{ll'}$, $\sigma_{ll'}$ are the electric
and magnetic RTLNs. They are defined with a different normalization with respect to those introduced in Paper~I and in
Sec.~\ref{sec:pani}; the conversion factors among them are (see Appendix~\ref{app:conversion})
\begin{align}
\lambda_2&=-\frac{4}{3}\sqrt{\frac{\pi}{5}}M^5{\tilde\lambda}^{(2)}_E\nonumber\\
\lambda_3&=-\frac{4}{5}\sqrt{\frac{\pi}{7}}M^7{\tilde\lambda}^{(3)}_E\nonumber\\
\sigma_2&=-\frac{1}{2}\sqrt{\frac{\pi}{5}}M^5{\tilde\lambda}^{(2)}_M\nonumber\\
\sigma_3&=-\frac{1}{5}\sqrt{\frac{\pi}{7}}M^7{\tilde\lambda}^{(3)}_M\nonumber\\
\lambda_{23}&=-\sqrt{\frac{\pi}{7}} M^4{\tilde\lambda}^{(23)}_E\nonumber\\
\lambda_{32}&=-\frac{3}{4}\sqrt{\frac{\pi}{5}} M^4{\tilde\lambda}^{(32)}_E\nonumber\\
\sigma_{23}&=-2\sqrt{\frac{\pi}{7}} M^4{\tilde\lambda}^{(23)}_M\nonumber\\
\sigma_{32}&=-16\sqrt{\frac{\pi}{5}} M^4{\tilde\lambda}^{(32)}_M\label{eq:transf}\,.
\end{align}

Equations~\eqref{eq:adiabatic} are called {\it adiabatic relations} because the TLNs and the RTLNs are assumed to be
constant, neglecting the oscillatory response to a variation of the tidal field; this adiabatic approximation is
violated in the final stages of the coalescence~\cite{Maselli:2012zq,Steinhoff:2016rfi}. Note that (at variance with
Paper~I) in Paper II the multipole moments and the tidal tensor can change with time; so, for instance, the orbital
Lagrangian (but not the internal Lagrangian, see Sec.~\ref{subsec:statirr}) depends on the multipole moments and on
their time derivatives. However, in the adiabatic approximation the time dependence of the tidal fields is neglected.
This implies that the nonaxisymmetric contribution of the tidal fields and of the multipole moments vanishes, since
stationary perturbations must be axisymmetric. In the general case (not discussed in this paper), the TLNs and the RTLNs
are {\it matrices} in the STF framework, which correspond, in the harmonic basis, to Love numbers depending on the
indices $l$ and $m$~\cite{LeTiec:2020spy}.

The internal Lagrangian ${\cal L}_2^{\rm int}(Q^{ab},Q^{abc},S^{ab},S^{abc})$ only depends on the internal degrees of
freedom of the body~$2$, and is determined by imposing that the variation of
${\cal L}={\cal L}_{\rm orb}+{\cal L}_2^{\rm int}$ with respect to the multipole moments yields the adiabatic
relations~\eqref{eq:adiabatic}. This gives
\begin{align}
{\cal L}_2^{\rm
int}&=-\frac{1}{4\lambda_2}Q^{ab}Q^{ab}-\frac{1}{12\lambda_3}Q^{abc}Q^{abc}-\frac{1}{6\sigma_2}S^{ab}S^{ab}\nonumber\\
&-\frac{1}{16\sigma_3}S^{abc}S^{abc}+\alpha J_2^aQ^{bc}S^{abc}\nonumber\\
&+\beta J^a_2S^{bc}Q^{abc}\,,\label{Lintpaper2}
\end{align}
where $\alpha$ and $\beta$ are related to the RTLNs. Indeed, using Eqs.~\eqref{eq:deftidaltensors} the variation of the
Lagrangian with respect to the multipole moments
gives Eq.~\eqref{eq:adiabatic}, with
\begin{align}
&\lambda_{23}=2\lambda_2\sigma_3\alpha~~~~~\lambda_{32}=6\lambda_3\sigma_2\beta\nonumber\\
&\sigma_{23}=3\lambda_3\sigma_2\beta~~~~~\sigma_{32}=8\lambda_2\sigma_3\alpha\,.\label{eq:identifications}
\end{align}
Remarkably, Eqs.~\eqref{eq:identifications} lead to
\begin{equation}
\sigma_{32}=4\lambda_{23}\,,~~~~~\sigma_{23}=\frac{1}{2}\lambda_{32}\,,\label{eq:prop}
\end{equation}
which, in the notation of Paper~I (see Eqs.\eqref{eq:transf}), gives
\begin{eqnarray}
{\tilde\lambda}^{(32)}_M&=&\frac{9}{4}\sqrt{\frac{5}{7}}{\tilde\lambda}^{(23)}_E\,,
\label{eq:prop2}\\
\tilde{\lambda_M^{(23)}} &=& \frac{1}{3}\sqrt{\frac{7}{5}}\tilde{\lambda}_E^{(32)}\,. \label{eq:prop2b}
\end{eqnarray}
We stress that the above relations among the RTLNs follow from the use of the Lagrangian formulation, which is also
instrumental to obtain the gravitational waveform. Remarkably, the magnetic-led RTLN $\sigma_{32}$ (i.e.,
${\tilde\lambda}^{(32)}_M$) and the electric-led RTLN $\lambda_{23}$ (i.e., ${\tilde\lambda}^{(23)}_E$) are obtained from
equations involving perturbations with \emph{opposite} parities. Therefore, from the perturbation theory point of view,
there is {\it a priori} no reason to expect these pairs of RTLNs to be related. Nonetheless, in the next section we will
confirm that Eqs.~\eqref{eq:prop2} and \eqref{eq:prop2b} hold true by computing the RTLNs of a spinning NS.  As
discussed in the introduction, this relation reveals the existence of a new type of hidden symmetry in the structure of
compact stars: a universal relation satisfied for \emph{any} EoS, which is exact for small compactness and weakly
violated at large compactness.

\begin{figure*}[th]
\includegraphics[width=0.48\textwidth]{fig1a.pdf}
\includegraphics[width=0.48\textwidth]{fig1b.pdf}
\caption{Electric-led and magnetic-led RTLNs for a static fluid with polytropic
	EoS with $n=1$. These results are obtained after correcting the numerical implementation of Paper~I.}
\label{1love}
\end{figure*}

\subsection{Static and irrotational relativistic TLNs}\label{subsec:statirr}
In Paper~I it was assumed that the fluid is {\it static}, i.e. $\delta u^i=0$. More recently, it was found that the
appropriate stationary limit of a time-dependent compact star has an irrotational fluid~\cite{Landry:2015cva}, in which
$\delta g_{\mu\nu,0}=0$ as for static perturbations, but $\delta u^i$ can have an azimuthal component. In the
irrotational case, the perturbation of the vorticity tensor,
\begin{equation}
  \omega_{\alpha\beta}=\nabla_{\alpha}(hu_\beta)-\nabla_\beta(hu_\alpha)\,,
\end{equation}
(with $h=(\rho+P)/n$, $n$ baryonic number density) identically vanishes.
Conversely the static fluid, although mathematically
consistent (it is an admissible solution of the field equations), cannot be retrieved as the static limit of a
time-dependent solution, and thus should not be considered as physically sound.

For a non-rotating NS the irrotationality condition simply reduces to the vanishing of the covariant velocity
perturbation, $\delta u_i=0$~\cite{Landry:2015cva,Pani:2018inf}, leading to $\delta u^\phi\propto \delta g_{t\phi}$.  As
discussed in Ref.~\cite{Pani:2018inf}, this choice corresponds to the magnetic TLNs computed by Damour and
Nagar~\cite{Damour:2009vw}. For a rotating star the irrotational condition is much more involved, it does not reduce to
a simple condition on the four-velocity components (see e.g.~\cite{Lockitch:2000aa}).

As noted in~\cite{Gupta:2020lnv}, this characterization of static and irrotational fluid configurations can be easily
rephrased in a Lagrangian framework. If the internal Lagrangian does not depend on time, its variations yield the static
perturbations. The irrotational perturbations, instead, are the zero-frequency limit of the equations obtained from a
time-dependent Lagrangian.

In Paper~II it was assumed that the Lagrangian ${\cal L}_{\rm int}$, describing the internal degrees of freedom of the
star, depends on the multipole moments but not on their time derivatives: ${\cal L}_{\rm int}={\cal L}_{\rm
  int}(Q^L_A,S^L_A)$, see Eq.~\eqref{Lintpaper2}. Therefore, the adiabatic equations~\eqref{eq:adiabatic}, arising from the
variations $\partial{\cal L}/\partial Q^L_A$ and $\partial{\cal L}/\partial S^L_A$, correspond to {\it static
  perturbations}. Thus, the hidden symmetry~\eqref{eq:prop2}-\eqref{eq:prop2b} refers to static perturbations as well.
In order to extend the results of Paper~II to {\it irrotational} perturbations, we should consider an internal
Lagrangian which depends (like the orbital Lagrangian) to ${\dot Q}^L_A,{\dot S}^L_A$ as well, compute the variations
with respect to the multipole moments, and finally consider the zero-frequency limit; we leave this computation for
future work~\cite{inprep}.
\begin{figure*}[th]
\includegraphics[width=0.47\textwidth]{fig2a.pdf}
\includegraphics[width=0.47\textwidth]{fig2b.pdf}
\caption{Ratios of RTLNs ${\cal R}_1$ (left panel) and ${\cal R}_2$ (right panel) [see Eq.~\eqref{eq:prop2r}]
  as a function of the compactness $C$, for a polytropic EoS with $n=0.5$,
  $n=1$, $n=2$ and for the APR4 EoS. The horizontal line denotes the theoretical prediction
  from the Lagrangian formulation [Eq.~\eqref{eq:prop2r}].}
\label{fig:ratios}
\end{figure*}

\section{Hidden symmetry of the RTLNs} \label{sec:results}
We shall now explicitly compute the static RTLNs for different EoSs. We shall then verify whether the
relations~\eqref{eq:prop2}, \eqref{eq:prop2b} are satisfied.
\subsection{Computation of the static RTLNs}
In order to compute the magnetic RTLNs~\eqref{eq:defRTLN}
\begin{equation}
  \lambda_M^{(ll')}=\frac{\partial J_l}{\partial{\cal E}^{(l')}_{0}}
\end{equation}
with $l'=l\pm1$, and the rescaled quantities ${\tilde\lambda}_M^{(ll')}=\lambda_M^{(ll')}/(M^{l+l'+1}\chi)$,
we have to determine the current multipole perturbations $J_l$
induced by an electric tidal field ${\cal E}^{(l')}_0$~\eqref{eq:defcEcB}; thus, we have to find the axial parity
perturbations $h^l_0$ induced by polar parity perturbations $H_0^{l'}$, by solving the polar-led
equations~\eqref{eq:polarled}. For ${\tilde\lambda}^{(23)}_M$, we have to consider the perturbations $h_0^2$ induced by
$H_0^3$, and Eqs.~\eqref{eq:polarled} reduce to
\begin{align}
  {\cal D}^{{\rm pol}\,(3)}[H_0^{3}]&=0\label{eq:3Estat}\\
{\cal D}^{{\rm ax}\,(2)}[h_0^{2}]&=S_+^{{\rm pol}\,(3)}[H_0^{3}]\,,\label{eq:23Mstat}
\end{align}
while for
${\tilde\lambda}^{(32)}_M$, we have to consider the perturbations $h_0^3$ induced by $H_0^2$, and Eqs.~\eqref{eq:polarled}
reduce to
\begin{align}
  {\cal D}^{{\rm pol}\,(2)}[H_0^{2}]&=0\label{eq:2Estat}\\
{\cal D}^{{\rm ax}\,(3)}[h_0^{3}]&=S_+^{{\rm pol}\,(2)}[H_0^{2}]\,.\label{eq:32Mstat}
\end{align}
Similarly, to compute the electric  RTLNs~\eqref{eq:defRTLN}
\begin{equation}
\lambda_E^{(ll')}=\frac{\partial M_l}{\partial{\cal B}^{(l')}_{0}}
\end{equation}
with $l'=l\pm1$,  and the rescaled quantities ${\tilde\lambda}_E^{(ll')}=\lambda_E^{(ll')}/(M^{l+l'+1}\chi)$,
we have to determine the mass multipole perturbations $M_l$ induced by a magnetic
tidal field ${\cal B}^{(l')}_0$~\eqref{eq:defcEcB}.
Thus, we have to find the
polar parity perturbations $H^l_0$ induced by axial parity perturbations $h_0^{l'}$,
by solving the axial-led equation~\eqref{eq:axialled}. For ${\tilde\lambda}^{(23)}_E$, we have to consider the perturbations
$H_0^2$ induced by $h_0^3$, and Eqs.~\eqref{eq:axialled} reduce to
\begin{align}
  {\cal D}^{{\rm ax}\,(3)}[h_0^{3}]&=0\label{eq:3Mstat}\\
{\cal D}^{{\rm pol}\,(2)}[H_0^{2}]&=S_+^{{\rm ax}\,(3)}[h_0^{3}]\,,\label{eq:23Estat}
\end{align}
while for
${\\tildelambda}^{(32)}_E$, we have to consider the perturbations $H_0^3$ induced by $h_0^2$, and Eqs.~\eqref{eq:axialled}
reduce to
\begin{align}
  {\cal D}^{{\rm ax}\,(3)}[h_0^{2}]&=0\label{eq:2Mstat}\\
{\cal D}^{{\rm pol}\,(3)}[H_0^{3}]&=S_+^{{\rm ax}\,(2)}[h_0^{2}]\,.\label{eq:32Estat}
\end{align}
The explicit form of Eqs.~\eqref{eq:32Mstat}-\eqref{eq:32Estat} is given in Eqs.~\eqref{eq:dpol}, \eqref{eq:dax} and in
Appendix~\ref{app:RTLNs}.

For concreteness, let us consider a quadrupolar electric tidal perturbation, $\mathcal{E}_0^{(2)}$ (the computation of
other multipoles follows straightforwardly).  In practice, we start by solving Eq.~\eqref{eq:2Estat} and then use
its solution to source Eq.~\eqref{eq:32Mstat}. Outside the star, we can solve the entire system analytically, obtaining
a solution that satisfies the asymptotic behavior~\eqref{eq:defcEcB}.  The full treatment of the separation of the tidal
and response parts of the solutions, as well as the definition of the solutions' free constants, is the same as in
Paper~I.

The interior solutions have to be computed numerically. We start by performing an asymptotic expansion of
Eq.~\eqref{eq:2Estat} at $r=0$ to obtain the initial conditions (up to an overall constant) and integrate up to the
radius of the star.  We then match the two (interior and exterior) solutions and their first radial derivatives at the
radius $R$, obtaining values for the free constants of the exterior solution (specifically, $\gamma_2$ and $\alpha_2$ as
defined in Paper~I) with which we compute the ($l=2$, electric) TLN of the non-spinning star,
${\tilde\lambda}_E^{(2)}$. Solving Eq.~\eqref{eq:32Mstat} follows a similar procedure, with the difference that --~being
an inhomogeneous equation~-- its full solution is obtained as a linear combination of a particular solution and the
solution of the corresponding homogeneous equation. The arbitrary multiplicative factor in front of the homogeneous part
--~as well as the value of the free single constant of the exterior solution ($\gamma^*_{32}$ as defined in Paper~I)~--
can be obtained via the matching at the radius of the star $R$. After this procedure one can simply extract the
corresponding RTLN, ${\tilde\lambda}_M^{(32)}$.

We compute the electric and magnetic RTLNs with $l,l'=2,3$ and $l,l'=3,2$ for different values of the compactness
$C=M/R$, for a sample of EoS consisting in the polytropic EoS with $n=0.5,1,2$\,\footnote{Note that, at variance with
  Paper~I, we use the polytropic EoS of the form $P=K\rho_0^{1+1/n}$, $\rho=\rho_0+nP$}, and the APR4
EoS~\cite{Akmal:1998cf}. The results of the computation (multiplied by $C^6$) are shown in Fig.~\ref{1love}. We stress
that the computations presented here correct some errors in the numerical implementation of Paper~I.

\subsection{The hidden symmetry}
Equations~\eqref{eq:prop2}, \eqref{eq:prop2b} imply that the ratios of the RTLNs ${\tilde\lambda}^{(ll')}_E$,
${\tilde\lambda}^{(ll')}_M$ with $l,l'=2,3 $ and $l,l'=3,2$, are constant
\begin{align}
  {\cal R}_1&\equiv\frac{{\tilde\lambda}^{(32)}_M}{{\tilde\lambda}^{(23)}_E}=\frac{9}{4}\sqrt{\frac{5}{7}}\simeq1.902\,,\\
  {\cal R}_2&\equiv\frac{{\tilde\lambda}^{(23)}_M}{{\tilde\lambda}^{(32)}_E}=
  \frac{1}{3}\sqrt{\frac{7}{5}}\simeq0.394\,,\label{eq:prop2r}
\end{align}
regardless of the NS mass and of the EoS. In Fig.~\eqref{fig:ratios} we show the ratios ${\cal R}_1$, ${\cal R}_2$ as
functions of the compactness, for the sample of EoS considered in this paper (polytropic EoS with $n=0.5,1,2$ and APR4
EoS), together with the theoretical prediction~\eqref{eq:prop2r}.

Note that the theoretical prediction from the Lagrangian PN approach [Eq.~\eqref{eq:prop2r}] is precisely satisfied in
the small-compactness limit. When $C\lesssim0.1$, the ratios ${\cal R}_1$, ${\cal R}_2$ coincide with the theoretical
prediction within $1\%$, whereas for $C\sim0.2-0.3$, the discrepancy increases (approximately) quadratically in $C$ up
to $\sim6\%$. We have verified that this discrepancy is significantly larger than the numerical errors, so it does not
look as a numerical artifact. Moreover, for any compactness the ratios ${\cal R}_1$, ${\cal R}_2$ are independent on the
EoS within $0.2\%$ (i.e., within the numerical error).

\section{Discussion} \label{sec:conclusions}
Our results imply that a hidden symmetry among the static RTLNs with opposite parity actually exists, as suggested by
the PN Lagrangian formulation of Paper I. This symmetry is exaclty satisfied in the small-compactness limit,
and is therefore stronger than other approximately EoS-independent relations between the (spin- and tidal- induced)
multipole moments of a NS~\cite{Yagi:2016bkt}.  For large values of the compactness the hidden symmetry is
weakly violated, but an EoS-independent (within numerical errors) relation is still present.

The very existence of this hidden symmetry is highly nontrivial and deserves further studies. In particular, it is not
clear which is its underlying reason. From a Lagrangian point of view it is natural to expect that opposite sectors are
coupled to each other, since a single interaction term in the form of Eq.~\eqref{LagrangianCoupling} gives rise to related
coupling terms in the field equations for ${\cal A}$ and ${\cal P}$ which are both proportional to the single coupling constant
$\alpha$. On the other hand, justifying the origin of this symmetry from a pertubation-theory point of view is
challenging, since there is {\it a priori} no reason why perturbations belonging to opposite parity sectors should be
related to each other.  This symmetry is somehow reminiscent of the relation between axial and polar perturbations in
Schwarzschild black holes found by Chandrasekhar~\cite{Chandrasekhar:1985kt}, although in this case it involves the
matter sector as well.

Another point that deserves future investigation is the dependence on the compactness. The latter does not enter
directly in the Lagrangian formulation of Paper~II, being encoded in the (R)TLNs. Our results suggest instead that the
prediction from the PN expansion is valid only for low-compactness objects, and it acquires small corrections at large
compactness.

Finally, in agreement with the framework of Paper~II, we have focused on {\it static} perturbations. We anyway expect
that  qualitatively similar (but quantitatively different) relations exist among the
\emph{irrotational} RTLNs. In order to extend our results to the more realistic, irrotational case, one should include
time dependence (and, possibly, nonaxisymmetry) in the tidal field, both in the Lagrangian and in the
perturbation-theory formulations. This interesting problem will be discussed in a future work~\cite{inprep}.

\begin{acknowledgments}
P.P. acknowledges financial support provided under the European Union's H2020 ERC, Starting
Grant agreement no.~DarkGRA--757480. We also acknowledge support under the MIUR PRIN and FARE programmes (GW-NEXT,
CUP:~B84I20000100001), from the Amaldi Research Center funded by the MIUR program "Dipartimento di
Eccellenza" (CUP:~B81I18001170001), and networking support by the COST Action CA16104.
\end{acknowledgments}

redpajama_set_name: RedPajamaArXiv


Quite surprising that nothing has been said when last Friday, the Australian government debt ticked just over $475 billion. For the last twelve months, the government on average has been borrowing $6.35 billion each month, so what happens when they hit the debt ceiling of $500 billion? Will that then bring an end to Australia's prized membership of the AAA – rated club?
Standard & Poor's, Moody's and Fitch have just 9 countries in the AAA club – Australia, Canada, Denmark, Germany, Luxembourg, Norway, Singapore, Sweden and Switzerland. Should our membership be revoked that would mean that borrowing costs would increase overnight, which is not a good sign for the Australian economy. The Australian Taxation Office (ATO) currently estimates that Australian small businesses currently owe $13 billion in unpaid tax debts. Obviously, there is no impact on existing debt although when it comes time to refinance then that would be an entirely different story.
With the federal government recently weighing into the housing affordability debacle there are two things that I would immediately implement to critique our housing markets.
1. The ATO has taken over responsibility for being Australia's biggest property manager so land banking must be the first point of call. It is estimated that Sydney now has well over 100,000 permanently vacant apartments so they should be rented out to ease the rental crisis. Look at the lost revenues the ATO is missing out on with these land banked properties, where the clear majority are owned by overseas investors. Land banking in Australia must be outlawed.
2. Reverse the ridiculous off – the – plan ratio back to 50 per cent from 100 per cent to overseas buyers. We are now going into the ninth year of 100 per cent and the only clear impact we are seeing is that foreign investors have become a most dominant player. In 2016, Chinese developers acquired almost 40 per cent of the Australian residential sites that were offered to the marketplace. All these properties are offered exclusively to Asia and these properties are not available for local buyers. Reducing the ratio back to 50 per cent would have a big impact on housing affordability.
A recent survey by Roy Morgan Research found that approximately 7 per cent of Australian mortgage holders have little or zero equity in their homes in the twelve months to October 2016. That would equate to approximately 300,000 properties across Australia. Western Australia has the highest number with 54,000, followed by South Australia with 27,000, Queensland with 63,000, Melbourne has 50,000, Victoria has 65,000, NSW has 73,000 and Sydney has 33,000. Tasmania came in with 5,000 – these are concerning numbers when you consider the east coast has enjoyed unprecedented capital appreciation.
Since 2009, Sydney home values have doubled and Melbourne have climbed 85 per cent. In 2011, less than 10 per cent of investors held multiple investment properties, according to Digital Finance Analytics. This has now grown to 16 per cent nationally, and on the east coast multiple investment properties is now approximately 18 per cent.
Really makes one wonder, just what data our elected politicians and policy makers are actually looking at or quite possibly, they don't even understand this data?
The most recent data from CoreLogic shows that the rental yields in Sydney and Melbourne are on the decline. For Sydney, houses yield is 2.8 per cent and units are 3.8 percent. In Melbourne, houses are 2.7 per cent and units are 4.0 per cent. It will be most interesting to see just how low these yields will go with all the new developments entering the market. It is quite clear that investors have been enjoying the unprecedented capital growth over rental yields in Sydney and Melbourne, although this is about to change.
With very few alternate investment opportunities, we don't at this particular point in time expect to see investors retreating out of the market, although we do expect to see carnage in the CBD markets. This should not come as a great surprise as these markets have introduced thousands and thousands of new apartments, and many suburbs have constructed less than one hundred new apartments.
Whatever the case, if you like watching real estate machinations 2017 will keep you highly entertained.
To add to this, the Commonwealth Bank advised mortgage brokers this week, that from February 13, it will cease accepting refinancing applications for investment home loans. Will the other major lenders then follow suit?
Any idea what the government are spending the $6B a month on?
It would be fascinating to see exactly what the $6.000 billion breakdown is although we both know we will never see that. Maybe the Opposition Leader might ask? He has been devoid of intelligent questions this week.
Yes agree 100% Robert, land banking needs to stop and that will force affordability in the market.
On the debt, we elected muppets and they are true to form.
what exactly do you mean by 'carnage in the CBD markets?' and when do you expect to see it?
In some areas there will be a massive oversupply of apartments all chasing tenants so it will be difficult for all these properties to secure tenants. What we have already see is rents at much lower figures than what was initially anticipated. In some developments there are thousands of apartments which might explain why in some areas the banks have shut – down all future funding.
The government should turn this into a benefit for Australians. Let Australians buy their first three homes stamp duty free. Permanent residents buy their first one with 10%, the second 20% and the third 25%. And foreigners pay 20% stamp duty on the first dwelling and then 25% on the second and then 50% on the third. Cap all individuals at 3 dwellings max. Then tie the tax raised to improving infrastructure – public transport, roads etc….
Then get rid of this nonsensical low density housing mere 5kms from the city. Rezone it all high density within 5 kms and medium density within 10. That will improve supply.
That will slow demand, raise revenue, and improve public infrastructure. It's not really rocket science.
Oh yeah, get rid of either local or state government so the government stop paying politicians for nothing really. That will help with the government spending/debt and hence help with maintaining the triple A rating.
certainly Australian land banking has a huge effect on the rental market.
As for National debt (still rising).
Well it started with the Kevin 07. the Labour Party has to be held accountable for wreckless spending.
To fix it? Simple but extremely difficult.
Welfare spending is out of control and 3 times that of its next villain.
The public Service is too large and sluggish, it literally is , adult day care in the main,Excepting those in essential services of course) for those who wish to contribute nothing to the good fortune of this nation.
Sadly, the Nation has developed a mind set of expectation and selfishness. Caused by left wing , social engineers,apologists.Labour, Greens and some independents. (in politically incorrect oldspeak, they are called , " bludgers" ).
Essentially, to have half a chance of real Australia, saving itself. We need to start with a major overhaul of the Electoral System. That is , one vote one value, and shock horror, eliminate compulsory voting.