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Victory Records Signs UK's Continents
Victory Records, in Chicago, IL (USA), welcomes dynamic South Wales, UK Metal/Hardcore outfit Continents, to its roster. Kerrang magazine describes Continents sound as, "Energy-fueled epic-core with lots of aggression, a healthy blend of raw shouts and low end growls and foot stomping hooks." Their music and intense stage presence has separated them from the ever-growing UK Metal/Hardcore scene.
"We've always tried to put our own passion for our music before external influence, the most important thing for us is that we enjoy the music we play, and if other people enjoy it too then that's awesome," said Vocalist, Philip Cross. "We like to mix elements of our favorite styles and influences, and then put our own perspective on things to see where it takes us."
Watch the bands announcement video here: http://www.youtube.com/watch?v=sQcq3OZATqM
Formed in 2010, Continents quickly established themselves within the UK music scene. They are five self-proclaimed "lads with a party attitude who love getting groups of people into a room who share their passion for music." In concert, this UK bunch throws a blistering barrage of songs and energy at the crowd which is evident in their first music video from the band's self-released single "Trials"; which received over 10,000 views on YouTube, in just the first few days. Thanks to "Trials", in November the band was voted as a favorite YouTube UK Metal Act and was featured on the YouTube home page.
Labels: continents signing victory records


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Deflated Balls and Other Nonsense – 10 Ridiculous Reasons to Hate The Patriots
January 28, 2015 January 28, 2015 / LM Pampuro
I missed a deadline and really hate to waste this one…
The lead story on the national news has been Deflate Gate; a story that centers around under deflated footballs in the New England Patriots win over the Indianapolis Colts in the National Football League's AFC championship game. Stress put on the word game. This was/is the lead story on ABC, NBC, CBS, CNN, Fox News, etc the past few days. Are there more pressing things for legitimate news organizations to concentrate on than a game?
Ok – so this is professional sports, but the lead story? One has to wonder how I.S.I.S., the Keystone Pipeline, and other world happenings feel about getting spiked. There must be many Patriots haters out there in the news industry. Let's take a look…
Now let's get Spy Gate out of the way. The Patriots were found videotaping the opposing coach's signals at games in September of 2007. Once caught the team proceeded to run the table and have an undefeated regular season, the first since the '72 Dolphins who only played a 14 game regular season. (The Patriots lost to the Giants in the Superbowl in game number 18. The Dolphins are credited with a perfect 17 game season.)
Now seven years later retired NFL Bill Cowher on a national sports show admitted that The Patriots were not the only team used videotaping, they were the only team to get caught.
The NFL changed the rules for Tom Brady. Several prominent journalists insist that the NFL rule changes regarding hitting the quarterback came in the wake of Bernard Pollard's hit on Tom Brady at the start of the 2008 season. However we should note that concerns started to be raised in 2005 with a hit on Carsen Palmer's knee. The rule was then changed to read "A rushing defensive player won't be allowed to forcibly hit a quarterback below the knees." The only change made after the Brady hit was to include "The clarification specifically prohibits a defender on the ground who hasn't been blocked or fouled directly into the quarterback from lunging or diving at the quarterback's lower legs."
In other words, let's have defenders avoid hitting quarterbacks in the knees. This really isn't a bad idea considering quarterbacks are usually the face of a NFL franchise.
Here is one I will give to Raider's Fans yet the rule existed on the books far before the Snowball playoff game: the tuck rule. Fans of The Raiders, Redskins, and yes, the Patriots too, have had fumble recoveries over turned because of the tuck rule. The Patriot's turnover in their favor, and some say the start of their dynasty, is the most prominent because it happened during a playoff game against the Raiders. One should note, however that in addition to The Patriots, both the Jets and the Broncos have taken advantage of this obscure rule during the regular season. So The Patriots have been both benefited and cursed by the tuck.
It is important to note that the NFL voted to eliminate the tuck rule in2013.
Bill Belichick, a.k.a. the winningest coach in NFL history. If he hasn't got the title yet he will have it soon. It is understandable not to like someone who avoids answering the questions he doesn't want to answer. It is also understandable not to like someone who has a habit of winning. Think about Don Shula, Bill Parcells, and Tom Landry along with their respected teams of dominance. There is a reason Terry Bradshaw, Lawrence Taylor, and others are obnoxious – they are winners.
Belichick's form of style is a combination of someone who is uncomfortable with small talk and the unintelligent. One cannot imagine him speaking about nothing and can understand why his response to ignorance is a glare, maybe a smirk, and then a non-answer.
Outside the required press conference Belichick is known to have a sense of humor. Those close to him claim he regularly will crack jokes and actually be personable. His players love him as do a lot of opposing team players. If one is observant before and after the coach's handshake at the end of a game, viewers will see opposing team players seek out the hoodied one for a quick word or two. Why would a player seek out an opposing coach if they didn't have some sort of respect for the man?
Winning is an expectation in New England and no one represents that expectation more than the head coach of The Patriots. Fans of opposing teams may hate Belichick yet given the opportunity to have him as your coach, I bet those fans would jump at the chance.
Tom Brady, Tom Brady, Tom Brady. Same as the coach – if he is your quarterback you love him yet if not…well there could be a bit of man envy going on. Why shouldn't there be? He is part of the winningest coach-quarterback combination in NFL history. The guy has a supermodel wife, adorable children, three Superbowl rings, and let's not forget the guy is pretty good looking.
Tom Brady cannot help how much media attention he gets. If you ever wonder how often his name is mentioned during non-Patriot NFL broadcasts, play the Tom Brady drinking game. (To play the game, one would take a sip of an adult beverage every time a broadcaster says his name. If watching a national sports show on ESPN or Fox Sports, even outside of New England, one could become quickly intoxicated. 21 and older please to play.) The man-love this man gets can be nauseating for the non-Patriot fan. (Pats fans think Peyton Manning try to play the same game.)
The one fact most sports fans will admit to is he is one of the best to ever play the game. Brady's name is spoken with the same reverence as Montana, Elway, Marino, Unitas, and in the modern football era, we must of course add Manning (Peyton, and maybe Eli too). The future Hall Of Famer is on his way to a sixth Superbowl appearance, most in the NFL by a quarterback and will certainly hold other records before his playing career is complete.
Deceptive formations and other such feces. Isn't the entire point of football to out maneuver your opponent in order to score more points and win the game? After the Raven's lost to The Patriots in a playoff game Raven's coach Jim Harbaugh claimed that Belichick used deceptive formations to win the game. Harbaugh went on to say that having a player who is usually eligible to catch a pass signal ineligibility is not a legal maneuver. Come to find out this tactic has been used several times by NFL and college teams and the technique is completely legal.
Doesn't one find this interesting that only the losing team complain about these things?
Speaking of loser's The Indianapolis Colts have to be the biggest bunch of poor sports on the planet. First a bit of history – way back in Brady's early years he and Belichick schemed to beat then quarterback and NFL pretty boy Peyton Manning on a regular basis. When The Patriots started to employ the no huddle offense, Indianapolis complained to the league that they didn't have time to react with substitutions and it wasn't fair. The league's response was to create a rule that stated both teams must have time to substitute players. Now let's jump ahead to Deflate-Gate. Which NFL team cried to the league? Could it be the one who lost by 38 points to The Patriots the day prior?
Former Colts G.M. and now ESPN commentator Bill Pollian cannot even enunciate the word Patriot correctly, let's not even go into the snide comments he usually makes following this mispronunciation. We can also look to owner Jim Irsay's recent Twitter campaign and wonder if this is just his way of getting back at the organization his teams have had little success against? Can you say poor sports?
Since we are on the subject of poor sports, there are too many ex-NFL players turned commentators to list here who have suddenly become ball experts. They can't get over their losses, whether it is a regular season, divisional, or Superbowl game. This goes back to The Patriots first Superbowl victory and although I refuse to give the guy any ink here – "Dude, you lost the game. Build a bridge and move on!"
Whiners of course are not limited to former opponents. Both broadcasters and institutions known for exceptional journalism have jumped on the anti-Patriot bandwagon. We will skip over ESPN for now, although their lines between commentators and journalists have pretty much disappeared, and look at a sports magazine tradition: Sports Illustrated. Recently S.I. ran a piece by Michael Rosenberg that claimed other teams have complained about the Patriots cheating for years with some coaches going as far as putting padlocks on the visiting team's locker room at Gillette. He also went on to accuse The Patriots of still videotaping, cheating by using a giant television outside the stadium (which contents are blurred from a sideline view), and Robert Kraft getting a favorable schedule from the NFL every year. When pushed on a Boston radio show Rosenberg could not name a source and kept answering any questions with "Well people say." Mr. Rosenberg, people say a lot of things.
Journalists are supposed to get as close to the truth as possible before publishing. "People say" just doesn't cut it. Sports Illustrated readers deserve better.
#1. This is easy. The haters exist because of jealousy. All The Patriots do is win consistently. They have a team first approach with players putting egos aside for the betterment of the organization and they get rid of their embarrassments (Aaron Hernandez was let go before his fingerprints dried.)
Haters will hate because at some point this country switch from getting excited about winners, to finding excuses for why they win. Hard work and dedication isn't enough in our "everybody gets a trophy" world.
We will see what is said after Sunday – Go Pats!
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E.S. SHANKAR
MURDERED IN MALAYSIA : THE ALTANTUYA STORY
TO BUY EBOOK @US$0.99 only
Author's Foreword
Foreword by Clare Rewcastle-Brown of Sarawak Report
Abdul Razak Baginda's (In)famous Bail Affidavit
Altantuya Videos
Americk Singh Videos
PI Bala Videos
Deepak Videos & Books
PI Bala SD1
Najib/ Razak Baginda Videos
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RPK's 'Let's Send The Altantuya Murderers To Hell'
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Sirul Videos
Murdered in Malaysia:The Altantuya Story – Interviews
Sirul's Sworn Confession. 9th November 2006
Sirul's signed unsworn statement read from the dock (English). 4th February 2009
Sirul's signed unsworn statement read from the dock (Bahasa Melayu). 4th February 2009
About Tiger Isle – Synopsis
Other Writings & Articles
Prizes/Nominations
Publisher/ISBN
To Buy Book
Malaysian Origins – A Brief History of The Peoples of Malaysia
Hitler Parody & Other Videos
1MDB AUDITOR GENERAL AND PAC REPORTS
Sirul's Signed Unsworn Written Statement Read By Him From The Dock. 4th February 2009
"On 18 October 2006 I was on duty at Unit Tindakan Khas (UTK), Bukit Aman , Kuala Lumpur. I attended the morning briefing there and was assigned the duty of standby driver for that day. Should any officer or staff be required to go anywhere on official matters, it was my duty to drive them there. At mid-morning on 18 October 2006, Azilah Hadri (Chief Inspector of Police 1) called me on my cellphone and asked me to meet him. Azilah asked me about my duties for the day and I informed him about my assignment as standby driver. During our cellphone conversation, I asked Azilah where he was and he replied he was in Ampang Road near Ampang Point (shopping mall) and was heading towards Central Market . Azilah wanted me to meet him at Malaya Hotel and asked me whether I knew of its location. I told Azilah I had not heard of that hotel even though I had lived in Kuala Lumpur for about 10 years. I next told Azilah that I was busy at that time and would not be able to meet him. However, I told him that I would be able to meet him after my duties were over. At that point in time, I was driving DSP Khairi to Gombak district to buy some supplies for the UTK . A short while later, Azilah telephoned me and asked me to meet him after I had finished the UTK office supplies buying job.
After I completed my work with DSP Khairi, I returned to the office and telephoned Azilah, asking him the exact whereabouts of our meeting place. Azilah confirmed the meeting place would be at the taxi/bus stop by the side of the Central Market. When I reached that taxi/bus stop at 2.00 p.m. 18 October 2006, Azilah was already waiting there. I slowed down my car near the kerb and Azilah got into the vehicle. I was driving a Proton Satria car. Then Azilah ordered me to drive and search for Malaya Hotel, but after driving around for some time, we were unable to locate it. Azilah then ordered me to drive to Damansara area. I asked Azilah the purpose of searching for Malaya Hotel and the purpose of going to Damansara. Azilah replied he had some work to do and to just follow his instructions. On the way to Damansara, Azilah told me that DSP Musa Safri had related to him that a friend of his was facing some "woman problems". Azilah ordered me to drive to DSP Musa's friend's house in Damansara. According to Azilah, DSP Musa's friend was a person who held a high position, a businessman and well-connected. During the drive, Azilah related that a woman and a man, believed to be her brother, both Chinese, had created a disturbance and caused a commotion in front of DSP Musa's friend's house. According to Azilah, the woman was a long-time lover of Musa's friend. As we reached Bukit Damansara, Azilah directed me towards a bungalow in a housing estate. Azilah asked me to slow down as we reached the front of the bungalow, and told me that was the house DSP Musa had referred to. As we drove away from the bungalow, Azilah told me to remember the route to it. According to Azilah, he had promised to help DSP Musa's friend by patrolling the bungalow area from time to time to prevent the Chinese woman and man from creating further disturbances and commotions in front of that house. On this premise, Azilah requested my help and asked me if I was prepared to do the patrolling work whenever I was free of my official duties and he was called away for duty outside Kuala Lumpur. I agreed to it as I knew DSP Musa, my superior. I regarded my agreement to help Azilah as actually a service to help my superior.
From Bukit Damansara, Azilah ordered me to drive back to Central Market as he had parked his car there. On the way, Azilah told me that the Chinese woman and man were staying at Malaya Hotel. It was then that I realised that Azilah's aim in searching for Malaya Hotel was to confirm the whereabouts of the Chinese woman and man. All the time I was with Azilah, he did not show me any document, paper or note which contained an iota of information about the identity of DSP Musa's friend, his residential address, hotel address, telephone number or the identity of the Chinese woman and man. As we neared Central Market, Azilah asked to wait in the car with the engine running, as he wanted to ask an artist friend of his at Central Market for the exact directions to Malaya Hotel. I waited for about ten minutes in the car park, when Azilah knocked on my window and told me Malaya Hotel was in nearby Petaling Street. I switched off the car engine and walked with Azilah to Malaya Hotel. When we reached Malaya Hotel, we entered the lobby. Azilah asked me to get some pamphlets, catalogues and leaflets from the lobby information corner. Next, Azilah entered the lift and asked me to follow him up. I am not sure which floor we got out on, but if I am not mistaken, it was the seventh. I followed Azilah to the closed door of a room. I cannot recall the room number. Azilah did not say anything. I asked Azilah what he wanted to do. Azilah replied he was hoping he would meet the Chinese woman and man, to advise them not to create disturbances and commotions in front of DSP Musa's friend's house. Then Azilah told me he was not sure that was the room occupied by the Chinese woman and man. Next, Azilah beckoned me to leave the place. We took the lift down to the lobby. We exited Malaya Hotel through its main entrance and walked back to Central Market. Azilah asked me to return to my office, and that if he needed my assistance, he would telephone me. I drove back to my UTK office.
At approximately 8.45 p.m. on 19 October 2006 when I was at my home in Kota Damansara, I received a call from Azilah asking me to go to DSP Musa's friend's house which we had visited the previous evening. According to Azilah, he had received information that the Chinese woman and man were in front of the house, and he needed my support if the duo resorted to violent action. I told Azilah I would go there immediately. I left my house within five minutes and headed for Bukit Damansara via the Kota Damansara-NKVE toll highway, in my jeep. I lost my way and was forced to call Azilah for directions. A short while later Azilah called me to ask if his directions were clear for me to follow. I replied that I was almost there. When I reached the area, I parked my vehicle by the roadside near a T-junction, and walked to the house. As I neared the house, I saw Azilah in animated conversation with a Chinese woman and an Indian man. When Azilah saw me nearing the house, he signalled with his hands as if asking me to get into a red Proton Wira car parked near the bungalow. I followed his directions and got into the front passenger seat, and noticed that a Malay woman in the driver's seat. Shortly after that, the Chinese woman walked over and got into the back seat of the car. The Malay woman then got out and also moved to the back seat. Azilah then got into the driver's seat. As he was about to drive off, a Chinese man knocked on Azilah's window. The Chinese man wanted the Chinese lady to settle the fare for his taxi cab. Azilah extended a RM50 note to the taxi driver, but the taxi driver it was insufficient as the actual fare was RM150. Azilah extended two more RM50 notes to the taxi driver. Next, we departed from the bungalow area. I asked Azilah to drop me off at the T-junction.
As I was driving off in my car, I noticed Azilah's car following me. As I reached the Damansara Road heading towards Duta Road, Azilah called me to pull over by the roadside, which I did. At that time I was driving in the vicinity of the old Amanah Raya Building. Azilah pulled up behind me. Azilah got out of his car and walked over to mine. I wound down my window and Azilah told me that the Chinese woman had responded well to his advice. Then Azilah asked me where I was heading. I told him as the situation was under control, and there was nothing more for me to do, I was going home. Azilah said 'ok.' I then drove along Damansara Road and turned left heading towards Duta Road and the NKVE past the Duta Road Government Complex. Before I headed left towards the NKVE, I called Azilah and asked him if he wanted me to patrol the bungalow area the following day, considering he would be on duty at Putrajaya then. Azilah replied he was in conversation with the Chinese woman, and asked me to call back in 5 minutes. As I was in the commercial district of Sri Hartamas on the way to the NKVE via the Pencala Tunnel Link, I called Azilah again. According to him, he had advised the Chinese woman, and it would be unnecessary for me to patrol the area of DSP Musa's friend's house. If he received reports of any new disturbances or commotions there, he would liaise with me. After this conversation, I pulled over at Devi's Restaurant in the commercial district of Sri Hartamas, for tosai . I left about 20 minutes later and reached home via the NKVE at about 10 p.m. Later at about 12.00 p.m., I drove from my home in Kota Damansara to Kampong Baru in Kuala Lumpur for early morning breaking of fast meal.
Before 31 October 2006, I received instructions from ACP Mastor that I was to serve duty with the Prime Minister's security contingent during his visit to Islamabad, Pakistan for 10 days from 31 October 2006 to 9 November 2006. Before leaving for Pakistan, I left my car at the compound in Bukit Aman and the car keys in my office in-tray. I had instructed Sergeant Rosli to switch on and rev the engine now and then when I was away. Before leaving for Pakistan, I had the car and its interior thoroughly cleaned. One of the objects which I had tightly wrapped up in a plastic box and kept in the boot was a pair of red slippers. During this trial, I noticed an exhibit, photo no.12 (P25), of a red pair of slippers, size 8, which is my foot size. During this trial, I also noticed exhibit photos 35-41 (P25), a pair of white slippers with writing 'BNA' on its wrapping and 'HEAT ADSAWD' on its container. I have never seen or worn this (white) pair of slippers ever before. When I left my car in Bukit Aman, this (white) pair of slippers was not in it. It is not my foot size either.
On the morning of 5 November 2006, I was on duty as the personal aide to the prime minister while he was in his hotel meeting room in Islamabad. All of a sudden, DSP Fisal arrived and ordered me to go upstairs to prepare food for a Dato. I went upstairs to meet a colleague to exchange duties. I surrendered my revolver to him, then took a rest while waiting further orders to prepare food. Not long after, there was a knock on the door and ACP Mastor appeared, followed by Sergeant Jelima and Corporal Zamri from UTK. ASP Mastor ordered me to return to Malaysia with the explanation that my ex-wife had lodged a police report against me and I was required to attend to this problem. I, ASP Mastor, Sergeant Jelima and Corporal Zamri boarded a plane from Islamabad. We landed in KLIA on 6 November 2006, where we were met at the aerobridge by officers and members of UTK. I was driven in the squad vehicle to IPK Kuala Lumpur. When we arrived there, ACP Mastor handed me over to DSP Chan of Section D9 of the IPK KL. At the D9 office, I was interrogated for about half an hour. Shortly thereafter, a man whom I knew as Sergeant Amran handcuffed me to himself. Then ASP Tonny appeared and ordered me to be taken to the Squad's Pajero. I was escorted downstairs via a lift by ASP Tonny, Janagaren, ASP Zulkarnain, several members of D9 and a video cameraman with a large camcorder on his shoulder. I was ordered to board the Pajero. I was seated in the middle at the backseat of the Pajero, with Sergeant Amran on my right and ASP Zulkarnain on my left. The driver was Corporal Khairuddin with ASP Tonny seated beside him. Seated in the same row as I were Janagaren and the video cameraman. The Pajero proceeded as part of a convoy via Hang Tuah Road, Old Airport Road, crossing Dewan Bahasa dan Pustaka, Istana Road across Istana Negara, National Museum, Jalan Duta and via the NKVE toll highway exiting at Kota Damansara. We followed the other vehicles and stopped at the UITM campus at Puncak Alam. Throughout that journey, I did not notice anyone asking for directions. I did not give directions either. Then the convoy moved towards Klang. As the convoy reached a 4-way junction, the Pajero turned right into a jungle track. At this search site, ASP Tonny ordered me to alight from the Pajero. We hung around the place for about 20 minutes before ASP Tonny ordered us to board the Pajero again. We drove off from that area. Suddenly ASP Tonny's cellphone rang and I saw him answering it. Following that, ASP Tonny told ASP Zulkarnain and the driver that this was the wrong road. ASP Tonny then instructed the driver to go back to the 4-way junction, where he turned left and stopped. ASP Tonny then answered his cellphone again, following which he ordered the driver to keep left and enter the jungle again. The vehicle went uphill until it reached a rest area. There, I noticed that a blue Pajero was already waiting there ahead of us. Before I alighted the vehicle, I saw Azilah, Chief Inspector (CI) Koh Fei Chow (KFC) , DSP Zainuddin and several plainclothed men hanging about the rest area. ASP Tonny ordered me to stand behind the Pajero. As it approached dusk, I was asked to board the Pajero which headed back to IPK KL.
At about 11 a.m. on 7 November 2006, I was taken from my lock-up to the Kuala Lumpur Magistrates Court for a remand hearing. After the remand hearing, I was taken to ASP Zulkarnain's office at D9 IPK KL. I was taken there handcuffed and saw CI KFC there as well in the room. There were only two narrow chairs in the room. ASP Zulkarnain was seated in his chair at his table, while I was ordered to sit in front of him. CI KFC stood by ASP Zulkarnain's side. CI KSC left and re-entered the room several times. During that meeting, ASP Zulkarnian was always with me with me throughout that period, from start to finish. As I recall, CI KFC left and came back several times, and was once away for 4-5 minutes. In the room, ASP Zulkarnain asked me many questions, and I replied those to which I knew the answer to and said no to those questions I did not know the answer to. During our meeting, I did not say to ASP Zulkarnain that I wanted to reveal anything. I also did not once say to him that I wished to provide any information. I know what 'Caution' means. In our meeting, never once did ASP Zulkarnain read a 'Caution' statement to me. Once when I answered that I did not know to his question, he raised his voice, and on another occasion he told me in a loud voice, "You tell the truth, tell me what you know, you are a member, we will help you, this matter will not be taken to Court." I kept quiet. On another occasion, ASP Zulkarnain raised his voice and in a firm and angry tone said, "Don't make me treat you like other OKI's." At that time his face showed anger and he stood up and then sat down. I was frightened. I was afraid he would beat me like other OKI's. I imagined that had I not been a member, I would certainly have been beaten up by ASP Zulkarnain. ASP Zulkarnain then directed many questions at me the answers to which I did not know. When I quickly replied I did not know, ASP Zulkarnain stood up, banged his desk and said, "It's like this Sirul, if you agree you follow me, identify those items, hold them up so that the cameraman can take pictures, then I can help you so that this matter will not be brought up in the Courts." When he said this, CI KFC was not in the room. At that moment, ASP Zukarnain's voice was soft and I believed he would help me. I kept silent and did not ask any questions about where I would be taken to and what ASP Zulkarnain meant when he said he wanted me to show some items.
While in ASP Zulkarnain's room, I did not see anyone typing anything, except towards the end of our meeting, when ASP Zulkarnain flipped open his laptop and typed something. This happened after he had spoken in a soft one and asked me to follow him to identify some items. I did not see CI KFC for some time until he appeared with an A4 sheet of paper on AZP Zulkarnain's instructions. Five minutes after ASP Zulkarnain had finished typing, I was escorted to a D9 meeting room by CJ KFC and left there alone for about 20 minutes. I was then escorted by Corporal Chiam, ASP Zulkarnain, CI KFC and CI Shawal into a Pajero. I followed them without asking any questions. Corporal Khairuddin drove us to Kota Damansara. I felt they were heading towards my house. A Volvo car with a RMP badge trailed the Pajero. When instructed by ASP Zulkarnain, the Pajero driver stopped the car in front of my flat. During this journey, no one asked for directions to my home. The members in the Pajero and I only talked about our duties in UTK and overseas. I also had not revealed my home address to the officers and members. I noticed a Unit Pemushanan Bom (UPB) vehicle together with the Volvo parked behind each other in the compound where my flat was. Next, ASP Zulkarnain, CI KFC, members and I, all got out of the Pajero. Throughout the walk to my flat, I was handcuffed to Corporal Chiam. I saw below my flat UTK officers DSP Yusri, Sergeant Rosli and Sergeant Zafri also waiting there. I saw Sergeant Rosli taking out a bunch of keys and handing them over to CI KFC. The bunch of keys were strung together in a single chain. I have several keys for my house, and not a chain of three keys as shown at the court. I noticed Sergeant Rosli submitting to CI KFC another chain of keys which I recognized to be mine as they were faded, unlike the shiny ones shown to me in court. This set of keys had been handed over to ASP Mastor in my flight from Islamabad to KLIA. CI KFC then handed over the keys to ASP Zulkarnain. After that, ASP Zulkarnain directed us upstairs. CI KFC, DSP Yusri and Sergeants Rosli and Zafri were followed by me handcuffed to Corporal Chiam. As we were going upstairs, ASP Zulkarnain did not ask me for my house address. Cameraman Kamarulzaman, Khairuddin and the UBP officers were still downstairs. CI Shawal followed us up. Then I was brought to my house, number 5-3-7. The door was unlocked by ASP Zulkarnain and all the others entered my house. ASP Zulkarnain entered the house first and asked Corporal Chiam and I to sit on the dining table chairs in the living room. The cameraman Kamarulzaman was not there yet. While I was seated at the dining table, ASP Zulkarnain entered the master bedroom followed by CI's KFC and Shawal, and Sergeants Rosli and Zafri. The bedroom door was shut. They were in there for about 10 minutes while Corporal Chiam and I were outside. While the master bedroom door was still shut, the cameraman Kamarulzaman entered the living room, while the UPB officers stayed outside the flat. About 10 minutes later, DSP Yusri and Sergeants Rosli and Zafri emerged from the master bedroom and had with them one large bag and two other bags which they took out of my house. The shut the master bedroom door behind them. About 3 minutes later, ASP Zukarnain opened the master bedroom door and asked me to enter. Corporal Chiam and I entered and we were asked to stand next to my clothes almari .
ASP Zulkarnain then asked the cameraman Kamarulzaman to enter the room. ASP Zulkarnain then said, "this is your jacket, hold it." When I entered the room, I noticed that the bedsheets were disarranged, the almari doors were open and the ceiling fan had been switched on. I then held the jacket and all our actions and poses were photographed by cameraman Kamarulzaman. While holding the jacket, I did not say anything. After that, I was asked to stand beside the bed. I saw ASP Zulkarnain take back my jacket and then remove some items from inside it. The jacket was spread out on the bed and ASP Zulkarnain placed the items on it. ASP Zulkarnain asked me to point towards to the items. He said, " Point your fingers." I said, "what is this, Sir?" I did not want to point, but ASP Zulkarnain asked me to "just point only, Sirul." It was then that picture of me pointing was taken. Other than pointing at the items with my fingers, I did not say anything. After that, I was asked to go and sit at the dining table. From the time I entered the room until the time I left, no officer read me any 'Caution' statement. After that, I was taken straight from my home to Bukit Aman.
Before I complete my statement, I must clarify that I have never met the victim in this case and have had no personal dealings whatsoever with her. I also do not know Abdul Razak bin Abdullah (Baginda) and have had no dealings with him before this case. I appeal to this Court to take into account that throughout this hearing, I have followed the proceedings and note that many important prosecution witnesses, principally those from D9 IPK cooked up stories, lied and always changed their stories when cross-examined. I note this with concern because, for me, their actions are done with the deliberate intention of implicating me so that I will be the black sheep who has to be sacrificed to protect the plans and evil intentions of those who are not in Court today to face the outcome of their treatment and schemes. I have not a single reason to hurt, what more, take the life of the victim in such a cruel manner. I appeal to this court which is in session and has the power to determine whether I live or die, so that I will not be hung, to, once and for perfectly complete the agenda they have for me.
Statement from the dock by the Accused
SIRUL AZHAR BIN HAJI UMAR
INTERVIEW WITH THE SUN DAILY
2013 – A WATERSHED YEAR? E.S.SHANKAR AT BUSINESS TODAY, MALAYSIA
TIGER ISLE-A GOVT OF THIEVES REVIEW BY SUSAN LOONE
Non-fiction murder conspiracy and cover-up involving the prime minister of Malaysia, Najib.


text:
\section{Introduction}
Roughly twenty percent of the cold classicals in the Kuiper belt are binary systems \citep{2008Icar..194..758N} with a mass-ratio of the components being close to unity. A well-known example is the Pluto-Charon system \citep{1978AJ.....83.1005C} located at an orbital distance from the Sun of around 39 au. With Pluto being roughly eight times as massive as Charon, it is often categorised as a nearly equal mass binary. Recent studies show with increasing certainty that equal mass binaries are not rare in the Kuiper Belt, their occurrence rate is estimated to be at least several percent \citep{2008Icar..194..758N} \footnote{The authors classify it as "equal size binaries". The internal densities are very similar for cold classicals making it equivalent to the definition of equal mass binaries.}.

Also, the Asteroid belt features numerous objects with companions \citep{2002aste.book..289M}.  Some of these binaries have similar masses (e.g. 90 Antiope, 2006 VW139, 2017 YE5, and 69230 Hermes \citep{2008Icar..196...97M,2004DPS....36.4602M,Agarwalletal2017,2012Icar..221.1130M}, others have large mass ratios, so that calling the smaller objects asteroid moons or satellites, and the larger ones planet or primary, seems more correct.

The Earth-Moon system is a binary with a relatively large mass ratio as well, although here the definition of equal mass binary reveals its ambiguity. The most recent definition of "equal-mass", to "near-equal-mass" is the need for the barycenter to lie outside both companions \citep{AlanLevison2002}. Another way of categorising the mass equality of binaries is the Tug-of-War ratio, expressing the planetary gravity over the solar gravity for a satellite. Equal mass planet binaries are often also called "double planets", making the definition of an equal mass binary even more vague; the Moon ticks off all the criteria for being a planet on its own, the Tug-of-War ratio for the Earth-Moon system is $0.46$ \citep{Herschel} but the barycenter lies within the body of the Earth making the Earth-Moon system a double planet system, an equal mass binary or a primary (Earth) and secondary (Moon) system, respectively \citep{Russel2017}.

The formation of binary planets is still an open question, and a number of channels have been proposed. In the classical model it is thought, at least in the case of Pluto-Charon \citep{2005Sci...307..546C,2011AJ....141...35C} and the Earth-Moon systems, that they formed by giant impacts on the primaries, smashing debris into stable orbiting secondaries \citep{1976LPI.....7..120C,2012Sci...338.1052C}. This scenario requires specific impact parameters that ensure sufficient angular momentum in the ejected debris in order to allow for the formation of an object outside the Roche limit.

A second viable mechanism to create binary planet(esimals) is capture via 3-body interactions in an early, dense phase of the solar system, where such interactions were much more frequent than they are today \citep{Goldreichetal2002,2005MNRAS.360..401A,2007MNRAS.379..229L,2008ApJ...673.1218S}. This might be the case for the dynamically hot classicals in the Kuiper Belt, which are more scattered due to perturbations by Neptune and have relatively wide mutual separations. They also show a broad and more chaotic distribution in orbital parameters, are subject to Kozai-Lidov effects \citep{Kozai,Lidov1962} and show a much lower equal mass binary occurrence than the cold classical population because disruption is relatively easy \citep{Morbinesv2020}. The objects in this population thus have a dynamical profile that fits a random capture process which suggests a different formation process than the cold classicals. The cold classicals have strong color correlations indicating the same composition \citep{Benechietal2009}, have close to unity mass ratios and show a clear preference for prograde orbits (80 \%) versus retrograde orbits (20 \%) \citep{Grundyetal2019}, strongly disfavouring a capture event.

Finally, a recently proposed mechanism to form planetary binaries is the Streaming Instability (SI) \citep{Youdin_2005,2011EM&P..108...39J,2021A&A...647A.126V}. In this scenario dust clumps together by interaction with the disk gas and, when becoming gravitationally bound, collapses on a dynamical timescale to form comets, planetesimals, and protoplanets \citep{2010AJ....140..785N,2019NatAs...3..808N}. Depending on the amount of angular momentum present in the clump before the collapse \citep{2021PSJ.....2...27N} and possibly added to it intrinsically during the collapse \citep{VisserandBrouwers2022}, the forming object will become a binary in order to absorb excess angular momentum. In this scenario, the disk is expected to be loaded with pebble-sized objects, with Stokes numbers between $10^{-2}$ to unity.

Regardless of the process of formation, if these binary systems have formed early in the disk, its further evolution and growth is non-trivial. The presence of nebular gas and/or solids might cause the binary components to spiral closer and merge if they are aerodynamically small within a Myr \citep{Lyraeal2021} or start wide and merge through secular effects \citep{Rozneretal2020}. If the binary components form early and start massive enough however for gravity to dominate, they might continue to grow through co-accretion. The growth of such a binary system is well-known to lead to a convergence in mass-ratio, if the satellite and primary accrete from a planetesimal swarm under the right conditions. A satellite would grow significantly faster than its primary due to its higher surface-to-mass ratio, and by exploiting the gravitational focusing of the primary \citep{HarrisKaula1975}, provided that the mutual separation is small enough \citep{MorWat2001}.

While this co-accretion scenario for binaries has been studied for planetesimal accretion, it has not been applied in the case of pebble accretion. In pebble accretion, massive bodies efficiently accrete solids through the interplay of gravity and the presence of nebular gas \citep{Ormel_Klahr_2010,LJ2012}. As the gas drag removes relative velocity and angular momentum from the solids, they are efficiently captured into the gravitational potential, leading to largely enhanced accretion cross-sections. Pebble accretion has only been invoked explicitly for a single pebble-accreting body, to explain many observational difficulties in planet formation with great success, such as size distributions of asteroids and Kuiper Belt objects  \citep{Johansenetal2015}, forming the cores of gas giants \citep{Levisonetal}, the TRAPPIST system architecture \citep{ormel-trappist,Schormel2019}, the spin axis of solar system bodies \citep{Visser_2020}, the formation of terrestrial planets \citep{Johetal2021}, and many other applications.

\myrev{Of course, pebble accretion will not be relevant for all planetary binary objects. The Earth-Moon system formed later, after the disk gas had already been dispersed - so pebbles would no longer drift inwards and the accretion of small rocks would not be enhanced by the interaction with the gas. Also, low-mass binary objects like most Kuiper Belt binaries will not have sufficient gravity to get pebble accretion started in a serious way. The process is, however, applicable for bodies that are sufficiently massive and form so early, that the gas disk and pebbles are still around.}

In this study, we investigate the evolution and growth of a planetary binary subject to pebble accretion. We subdivide the total mass $M$ of a single body in two masses $M_1$ and $M_2$ such that $M = M_1 + M_2$ with an increasingly diverging mass fraction $f_m = M_1 / M_2 \in [1,8]$. We determine the timescale to $e-$fold the mass of the binary compared to the growth time of a single body with the same mass. We then quantify the $e$-folding time needed to converge the mass ratio to unity by looking at the individual efficiency of accretion from the flux of pebbles swept up by the system. In many cases we find that, in the "die-hard" pebble accretion regime, the lower mass body (in this case $M_2$) grows faster than the more massive one for, in essence, the same reasons as in the planetesimal accretion case described above. As a result, the mass-ratio can converge back to unity, well within the disk lifetime of $\sim$1 Myr. Pebble accretion provides an explanation for the significant fraction of (near) equal mass observed planetary binaries.

The paper is organised in the following way. In section \ref{sec:1}, we discuss the model setup and the assumptions we use.  In section \ref{sec:2}, we describe the results of the numerical simulations. In section \ref{sec:3}, we discuss the outcomes and results, after which we summarise the implications and conclude in section \ref{sec:4}.
\section{Setup and assumptions}
\label{sec:1}
\subsection{Disk model}

In order to see how these binary systems evolve, we begin with a general description of the planet-forming disk in which the binary resides. For the gas temperature and surface density, we assume power law profiles given by \citep{WeidenschillingB} and \citep{Hayashi1985}:
\begin{align}
        \label{eq:T} T(r_0) &= 170\ \mathrm{K}\left(\frac{r_0}{1\ \mathrm{ au}}\right)^{-1/2}\\
        \label{eq:Sigma}\Sigma(r_0) &= 1700\ \mathrm{g\ cm}^{-2} \left(\frac{r_0}{1\ \mathrm{au}}\right)^{-3/2},
\end{align}
where $r_0$ is the radial distance to the central star. We assume hydrostatic equilibrium whereby the vertical density structure forms as a Gaussian:
\begin{align}
    \label{eq:rho} \rho(r_0, z) &= \frac{\Sigma(r_0)}{\sqrt{2\pi}H(r_0)}e^{-\frac{1}{2}\left(\frac{z}{H}\right)^2},
\end{align}
with $H = c_\mathrm{s}/\Omega_0$ the scale height, $\Omega_0$ the Keplerian frequency, $c_\mathrm{s} = \sqrt{k_\mathrm{B}T/\Bar{m}}$ the local isothermal sound speed, $k_\mathrm{B}$ Boltzmann's constant and $\Bar{m}$ the mean molecular weight. The gas moves at a slightly lower velocity than Keplerian, $v_\mathrm{K} = \sqrt{GM_\star/r_0}$ where $G$ is the gravitational constant and $M_\star$ the mass of the star. \citep{WeidenschillingA} gives a dimensionless constant relating $v_\mathrm{K}$ and the headwind particles travelling in Keplerian orbit feel. This dimensionless constant $\eta$ can be estimated by looking at the $r$-dependencies of equations \ref{eq:T}-\ref{eq:rho}:
\begin{align}
    v_\mathrm{hw} &= \eta v_\mathrm{K}\\
    \eta &= \frac{r_0}{2v_\mathrm{K}^2\rho}\frac{\mathrm{d}P}{\mathrm{d}r_0} = -\frac{13c_\mathrm{s}^2}{8v_\mathrm{K}^2},
\end{align}
where $v_\mathrm{hw}$ is the headwind and $P$ the pressure governed by the ideal gas law. For the adopted disk profile, the headwind has a numerical value of $v_\mathrm{hw} = -32$ m s$^{-1}$ downward in the co-moving local frame. In our parameter study the Epstein regime for pebble stopping time is the relevant one and we calculate it from the Stokes number ($\tau_\mathrm{s}$), relating the stopping time ($t_\mathrm{s}$) to one orbital timescale:
\begin{equation}
    \tau_\mathrm{s} = t_\mathrm{s} \Omega_0.
    \label{eq:stok}
\end{equation}

\begin{table*}
\centering
\label{Tab:tablepars}
\caption{Overview of the parameter study used in the simulations. The ranges between brackets are logarithmically spaced containing 30 values for $\tau_\mathrm{s}$ and 10 values for $a_\mathrm{b}$. Since we simulate 2 different mass ratio's $f_m$ at 2 different orbital distances $r_0$ we have 30x10x2x2 = 1200 simulations in total. The boldfaced quantities indicate the parameter set of the fiducial model.}
\tabcolsep=0.1cm
\begin{tabular}{llllll}
\hline
\hline
$r_0$ {[}au{]} & $\tau_\mathrm{s}$                                & $a_\mathrm{b}$ $[R_\mathrm{H}]$              & $f_m$ & N    & $M_\mathrm{total}$                     \\ \hline
2.5            & {[}$10^{-2}$-0.4{]}                              & {[}0.0075-0.05{]}                            & $2,8$    & 8100 & $M_\mathrm{Pluto} + M_\mathrm{Charon}$ \\
$\mathbf{39}$  & {[}$5 \times 10^{-4}$-0.1{]}, $\mathbf{10^{-2}}$ & {[}$10^{-3}$-$10^{-2}${]}, $\mathbf{0.0025}$ & $2,\mathbf{8}$    & 8100 & $M_\mathrm{Pluto} + M_\mathrm{Charon}$ \\ \hline

\end{tabular}
\end{table*}

\subsection{Pebble and binary dynamics}

\begin{figure}[!tp]
    \centering
    \includegraphics[width=0.45\textwidth]{Figures/binarysketch.pdf}
    \caption{An overview of the binary planetesimal system in the co-moving frame. The star is located on the left side of the frame. The binary components are denoted with their masses $M_1,M_2$ and radii $R_1, R_2$, travelling around their barycenter in circular orbit at distance $a_1$ and $a_2$ respectively. Pebbles are released from a distance $y_0$ between the edges of the impact range $x_1,x_2$ for a given initial phase angle of the binary $\varphi_0$ with respect to the $x$-axis. The starting velocities of different pebbles differ depending on the $x$-coordinate as seen in equation \ref{v_y}, therefore their velocity vectors point in different directions. The background gas headwind is denoted with the black arrow on the y-axis.}
    \label{fig:overview}
\end{figure}

We adopt a two-dimensional local shearing sheet box co-moving with the binary center-of-mass (barycenter) at distance $r_0$ from the central star. In this frame the equation of motion of a pebble is given by \citep{Ormel_Klahr_2010}:
\begin{align}
    \frac{\mathrm{d} \mathbf{v}}{\mathrm{d} t} = \begin{pmatrix}
    2 \Omega_0 v_y + 3\Omega_0^2x\\
    -2\Omega_0 v_x
    \end{pmatrix} -\sum_{j=1}^{2} \frac{G M_{j}}{|\mathbf{r} - \mathbf{r}_j(t)|^3}\begin{pmatrix}
    x - x_j(t)\\
    y-y_j(t)
    \end{pmatrix} + \mathbf{a}_\mathrm{drag},
\end{align}
with the first expression in brackets consisting of the Coriolis and tidal accelerations, the second term the two-body gravity of the separate binary components with mass $M_j$ and Cartesian positions ($x_j(t)$, $y_j(t)$).

From here on we use the following terminology for the binary components. We say the binary is equal mass if the mass ratio is unity and no explicit reference to one of the bodies has to be made due to symmetry. If the mass-ratio changes to $f_m \equiv M_1/M_2 > 1$ we say that the more massive one with mass $M_1$ is the \textit{primary}, and the least massive one with mass $M_2$ is the \textit{secondary}.

We consider a binary separation that is narrow and we assume mutual circular motion of the binary system during the accretion. The circular motion of the system with total mass $M = M_1 + M_2$ is then modelled through time $t$ with:
\begin{equation}
    \begin{pmatrix}
    x_{1,2}\\
    y_{1,2}
    \end{pmatrix}= a_{1,2}\begin{pmatrix}  \cos (\varphi_0 + \omega t)\\\sin (\varphi_0 + \omega t) \end{pmatrix}
    \label{eq:phase}
\end{equation}
where $\omega = \sqrt{G M / a_\mathrm{b}^3}$ the angular frequency, $\varphi_0$ the initial phase angle with which the simulation started and the subscripts indicating to which body it applies, respectively. The binary components are assumed massive and unaffected by the gas. They are placed on a circular orbit around the barycenter with orbital separation $a_\mathrm{b} = a_1 + a_2$ with, if $f_m \ne 1$, $a_1$ the distance of the primary with mass $M_1$ and radius $R_1$ and $a_2$ the distance of the secondary with mass $M_2$ and radius $R_2$, to the barycenter. The system rotates in a prograde orientation around its barycenter.

The Cartesian coordinates and velocities of the pebble are given by ($x$, $y$, $v_x$, $v_y$). The last term contains the acceleration due to the drag force on the pebble equal to:
\begin{equation}
    \mathbf{a}_\mathrm{drag} =
    -\frac{\mathbf{v} - \mathbf{v}_\mathrm{g}}{t_\mathrm{s}},
    \label{eq:drag}
\end{equation}
with $\mathbf{v}_\mathrm{g}$ the gas velocity including shear given by:
\begin{equation}
    \mathbf{v}_\mathrm{g} =  \left(v_\mathrm{hw} - \frac{3}{2}\Omega_0 x\right) \mathbf{e}_y.
    \label{eq:vgshear}
\end{equation}
An illustrative sketch of the setup is shown in Figure \ref{fig:overview}.

The total mass $M$ of the system in our model corresponds to the mass of the Pluto-Charon system, with an internal density $\rho_{\bullet} = 1.778\,\mathrm{g \ cm^{-3}}$ taken equal for both bodies. The (shared) Hill radius is then given by:
\begin{equation}
    R_\mathrm{H} = r_0 \left(\frac{M}{3 M_\mathrm{\star}}\right)^{1/3}.
    \label{eq:Rh}
\end{equation}
In varying the mass-ratio of the binary system we then subdivide the total mass accordingly over the components from which their barycentric distance $a_1$ and $a_2$ directly follow as:
\begin{equation}
    a_{1,2} =\frac{M_{2,1}}{M} a_\mathrm{b}.
    \label{eq:barya}
\end{equation}
From the assumed internal density the radius of each body is then calculated from:
\begin{equation}
    R_{1,2} = \left(\frac{3M_{1,2}}{4 \pi \rho_{\bullet}}\right)^{1/3}.\label{eq:radbodies}
\end{equation}

\subsection{Numerical method and initial conditions}
\label{subsec:nummethod}
We are interested in the (relative) growth rate of the binary (components) subject to pebble accretion. To do so we integrate the pebble trajectories with the Runge-Kutta-Fehlberg step variable integration method \citep{Fehlberg69,RKF45} with a relative error tolerance of $\mathrm{tol} = 10^{-6}$. The pebbles are released on a distance far away from the binary in the y-direction:
\begin{align}
        y_0 = C\sqrt{\frac{GMt_\mathrm{s}}{v_\mathrm{hw}}},
        \label{eq:y0}
\end{align}
(as illustrated in figure \ref{fig:overview}) with $C = 200$, a safety factor. This ensures that, initially, gas drag is dominant over the gravity from the binary center-of-mass. The initial velocities of the incoming pebbles are hence given by the unperturbed radial and azimuthal drift velocities \citep{WeidenschillingA},
\begin{align}
        \label{v_x} v_{x,\infty} &=- \frac{2\tau_\mathrm{s}}{\tau_\mathrm{s}^2 + 1} v_\mathrm{hw},\\
        \label{v_y} v_{y,\infty} &= -\frac{1}{\tau_\mathrm{s}^2+1}v_\mathrm{hw} - \frac{3}{2}\Omega_0x_0,
\end{align}
where $-\frac{3}{2}\Omega_0x_0$ is the correction to the Keplerian Shear. The pebbles are released with a shear corrected sampling function, equivalent to the method used in \citet{Visser_2020}. In the co-moving local frame we adopt, the pebble flux released then increases for increasing $x_0$, to account for the increasing relative velocities of the pebbles with respect to the binary barycenter due to shear.

We then use a bisection algorithm to find the range of initial x-coordinates for which the pebbles hit one of the binary components, this range is verified to be equal to the impact parameter of a single planetesimal with mass $M=M_1+M_2$ in the parameter space we investigate. We do note that this only is valid for the close binary separations we consider. A pebble is registered as a hit when it satisfies the condition:
\begin{align}
        \sqrt{(x - x_{1,2})^2 + (y - y_{1,2})^2} \le R_{1,2},
        \label{eq:hit}
\end{align}
with the subscript again referring to the corresponding body. After the cross-section edges have been found we release pebbles between the edges $x_0 \in [x_1,x_2]$ accounting for an error of missing trajectories of $\sim$ 5 percent. The resolution in pebbles released is taken to be $N_{x_0} = 90$ for each initial phase angle linearly spaced between $\varphi_0 \in [0,2 \pi)$ of the binary system with resolution $N_{\varphi_0} = 90$. In total, we then release an amount of $N_{x_0} \times N_{\varphi_0} = 8100$ pebbles per individual simulation. Finally, in each simulation we sum the total number of accreted pebbles on each body $N_{1,2}$ over each initial phase angle and we define the accretion ratio to be:
\begin{equation}
        \varepsilon \equiv \frac{\dot{M_1}}{\dot{M_2}} = \frac{N_1}{N_2},
        \label{eq:accratio}
\end{equation}
with $N_1$ and $N_2$ the total hits on the primary or secondary, respectively if the mass ratio is not unity.

To structure the results from our parameter study we define a fiducial model based on the Pluto-Charon mass(-ratio), radii, orbital distance from the star $r_0 = 39$ au and separation distance $a_\mathrm{b} = 0.0025R_\mathrm{H}$ with a pebble Stokes number of $\tau_\mathrm{s} = 10^{-2}$. An overview of the fiducial model and the rest of our parameter study is provided in Table \ref{Tab:tablepars}.

\begin{figure*}[tp!]
    \centering
    \includegraphics[width=0.9\textwidth]{Figures/Trajectories/hitmap6.pdf}
    \includegraphics[width=1.0\textwidth]{Figures/Trajectories/6trajectories6x1.pdf}

    \caption{Top: Hitmap of pebble impacts on an equal mass binary system such that $M_1=M_2=(M_\mathrm{Pluto}+M_\mathrm{Charon})/2$. Every pixel is a pebble falling into the system. On the $x$-axis the $x_0$ coordinate at moment of release is shown in Hill radii, while on the $y$-axis the initial phase orientation of the binary $\varphi_0$ in radians is depicted as illustrated in figure \ref{fig:overview}. The orange pixels show impacts on $M_1$, the brown pixels on $M_2$ \& the beige pixels indicate ejected pebbles. The final accretion ratio $\varepsilon = 1$, meaning that both bodies accrete an equal flux of pebbles because of symmetry arguments. The dashed red line indicates a starting angle of $\varphi_0=\pi$ rad. From 6 results in this graph the trajectories have been plotted below, those are denoted as A-F in this hitmap. The resolution has been taken $(N_{\varphi_0} \times N_{X_0} = 500 \times 1000)$.\\ Below: Six trajectories from the hitmap above. Shown is a top-down view of the binary system with a pebble "falling" in. In each of the trajectories, an arrow denotes the pebble coming into the frame. Pebble trajectories A through F are sorted with their starting distance $x_0$ going from left to right, corresponding to closer radial distance from the star to further away, respectively. Note that even though the trajectory for F appears to start on the bottom left, it originated on the right outside of the frame only entering the image below.}
    \label{fig:hmf}
\end{figure*}

\begin{figure*}[t]
    \centering
    \includegraphics[width=\textwidth]{Figures/trajectory.pdf}
    \caption{A selection of pebble trajectories for a given initial phase angle for the fiducial model with a mass ratio of 2, to illustrate the accretion advantage for the secondary. Left panel: the pebbles enter the Hill radius (dashed circle) from the top and approach the binary center of mass in the middle of the panel. Gray trajectories miss the entire system, blue ones accrete onto the secondary and red ones onto the primary. Right panel: a zoom in on the trajectories shown in the left panel. The hits on the secondary are indicated with the blue crosses at point of impact. It clearly illustrates the accretion advantage for the smaller body due to close encounters and spirals. Additionally, we show the more massive body in the center (dark red solid circle) with a direct hit of a pebble (dark red trajectory). The trajectories are from different times and are plotted in one panel only for illustration.}
    \label{fig:fidacc}
\end{figure*}

\section{Results}
\label{sec:2}
\subsection{General interpretation}
We have now described the way a single pebble interacts with a binary planetesimal system, but that does not tell us how that system of planetesimals will grow through time. We need every starting $x_0$-position where released pebbles will interact with the system and all starting angles $\varphi_0 \in [0,2 \pi)$ as described in section \ref{subsec:nummethod}. In figure \ref{fig:hmf} we plot a hitmap of 500.000 pebbles using our fiducial system from table \ref{Tab:tablepars}, with the only exception the mass-ratio is set to $f_m=1$. Because of symmetry considerations, the accretion ratio $\varepsilon$ (equation \ref{eq:accratio}) in this run is therefore unity.

Every pixel in the hitmap is a single pebble falling into the binary system, set by the $x$-coordinate when released and the phase of the binary at that moment. When a pebble falls toward the system, there are three possible outcomes; the pebble can fall onto either of the planetesimals, or it can fly by without hitting any of the two bodies and continue on its path around the central star. In the first two cases the pixel is coloured either brown or orange depending on onto which body it accretes.  If the trajectory does not lead to accretion, it is coloured beige.  This specific case describes an equal-mass binary $M_1=M_2$, the planetesimals are moving as a mirror image of each other around the barycenter. Therefore, we expect that the top and the bottom half of the hitmap are identical, with inverted colours. This is indeed the case in figure \ref{fig:hmf}. A horizontal dashed red line is added at $\varphi_0 = \pi$ to emphasise this symmetry. The exact same image can be seen above and below this line, only with the brown and orange colours swapped. In a system of a non-equal mass binary, this symmetry is expected to disappear.

By looking at the different trajectories found in the hitmap shown above, we can identify (at the simplest) three regions for all pebbles falling into a binary system ranging from the most outer left to the most outer right:
\begin{enumerate}
    \item Most pebbles falling in from the left side of the map enter the system circling in a prograde direction around the binary, in the same direction as the planetesimals are moving. This can result in a pebble spiralling into the system slowly, like in trajectory E, but in the example of figure \ref{fig:hmf} it mostly results in chaotic paths as seen in trajectories A and B. In this case we believe these chaotic paths happen because when a pebble gets close to one planetesimal it stays in its vicinity for longer and has a large probability to get slung around resulting in a chaotic path. In other scenario's (different $\tau_\mathrm{s}, a_\mathrm{b}$, etc.) we can see pebbles spiralling in slowly and favouring hitting the outer (less massive) planetesimal, like in figure \ref{fig:fidacc}.
    \item In the middle of the hitmap, for figure \ref{fig:hmf} specifically between $0.28R_\mathrm{H}\lesssim x_0\lesssim0.32R_\mathrm{H}$, the pebbles fall in from straight above the system. Falling in head on, with great velocity, either hitting one of the two bodies or going right past them and missing both. This region is exemplified by trajectories C and D.
    \item On the right side the pebbles come into the system circling around in retrograde fashion, opposing the movement of the binary. In the hitmap, this results in a large region of pebbles spiralling in slowly as seen in E. This happens all the way to $\sim 0.37R_\mathrm{H}$, from which the last trajectories are mostly chaotic paths. We believe this to come from the fact that the pebbles swirl around the binary and come back into the system almost from below. In that case it does not have the same momentum as when it comes in from above since it now is moving opposite to the shearing wind. This lack of momentum makes it easy to get swung around when actually getting near the two bodies and do more chaotic paths as exemplified in F.
\end{enumerate}
Modifying the fundamental parameters $\tau_\mathrm{s}, a_\mathrm{b}$, and mass ratio's will theft the impact parameter ranges leading to the 3 regimes (coming in prograde, head on and retrograde), but the fundamental structure remains similar.

\begin{figure*}[t]
    \centering
    \includegraphics[width=1.\textwidth]{Figures/Gamma.pdf}
    \caption{The growth efficiency $\Gamma$ as described in equation \ref{eq:Gamma}. Left: Mass ratio of $f_m=2$. Right: Mass ratio of $f_m=8$. for a range of Stokes numbers $\tau_\mathrm{s}$, mass-ratios and binary separation $a_\mathrm{b}$ at orbital distance of $r_0=2.5$ au from the central star (top panels) and $r_0 = 39$ au (bottom panels). The most opaque lines denote an orbital separation of $a_\mathrm{b}=0.0075R_\mathrm{H}$ while the most transparent lines shows an orbital separation of $a_\mathrm{b}=0.05R_\mathrm{H}$, other lines indicate orbital separations going logarithmic in between.}
    \label{fig:2-5aures1}
\end{figure*}

\subsection{Spiralling pebbles}
\label{sec:spiralling}
The situation where a pebble is caught by the binary into a spiralling motion is particularly interesting.
For an equal-mass binary, both bodies are then equally likely to accrete the pebble. However, if the binary has one body more massive than the other and if the distance between the 2 bodies is smaller than the initial size of the spiral, the lower-mass body becomes the more likely target. This important effect is illustrated in Figure \ref{fig:fidacc}. In this case, the masses are different, specifically $M_1 = 2M_2$. Integrated over all pebbles in the impact parameter the accretion ratio $\varepsilon$ as described in equation \ref{eq:accratio} of this system is less than one, meaning that the smaller body is accreting more mass per unit time than its more massive counterpart. This may seem counter-intuitive as less massive body has a smaller gravitational pull.  However, it can be understood by the in-spiralling motion of the pebbles that are bound to the binary system long before they actually get accreted. Figure \ref{fig:fidacc} shows a number of pebbles from a horizontal row in a hitmap. These pebbles have different starting positions $x_0$, but are launched with the same starting angle $\varphi_0$ of the binary. Many of the orbits turn into a spiral that slowly closes in on the binary. The small body moves like a vacuum cleaner through its orbit around the massive body (in fact, the barycenter, which will be very close to or even inside the larger body). As long as the settling velocity on the spiral path is low, the smaller body is likely to sweep up the incoming pebble before it can reach the massive body.

\begin{figure*}[t]
    \centering
    \includegraphics[width=1.\textwidth]{Figures/epsilontilde-chi2_5au.pdf}
    \caption{Top: The normalised growth ratios expressed in $\Tilde{\varepsilon}$ like described in equation \ref{eq:epsilontilde} for a range of Stokes numbers $\tau_\mathrm{s}$, mass-ratios and binary separation $a_\mathrm{b}$ at orbital distance of $r_0=2.5$ au from the central star. The most opaque lines denote an orbital separation of $a_\mathrm{b}=0.0075R_\mathrm{H}$ while the most transparent lines shows an orbital separation of $a_\mathrm{b}=0.05R_\mathrm{H}$, other lines indicate orbital separations going logarithmically in between. Bottom: Relative growth timescales of both bodies as a fraction of the growth timescale of a single body with mass $M=M_1+M_2$ as described in equations \ref{eq:tgrowth1} and \ref{eq:tgrowth2}. Black and red lines denote $M_1$, while the blue lines denote $M_2$.}
    \label{fig:2-5aures}
\end{figure*}

\begin{figure*}[t]
    \centering
    \includegraphics[width=1.\textwidth]{Figures/epsilontilde-chi39au.pdf}
    \caption{Same results as described in figure \ref{fig:2-5aures}, only at an orbital distance of $r_0=39$ au from the central star. Note, we use a different range of Stokes numbers $\tau_\mathrm{s}$ and binary separations $a_\mathrm{b}$.}
    \label{fig:39aures}
\end{figure*}

\subsection{Accretion efficiency}
The impact parameter range of pebbles reaching the binary turns out to be the same as in a computation where the total mass of the binary is present as a single, larger body. This is the case when the system has a small binary separation compared to the range of impact parameters in which pebble accretion is relevant. Nevertheless, not all pebbles within the impact parameter range are actually accreted by the binary. The pebbles that are lost escape through scattering by close encounters with the primary and the secondary mass, as illustrated in Figure \ref{fig:hmf}A,D and F. This is different from the single mass case, in which, for the considered parameter space all pebbles in the release range would be accreted. Therefore, we define the fraction of pebbles accreted on the binary, compared to the single-body case:
\begin{equation}
    \Gamma \equiv \frac{N_1 + N_2}{N_\mathrm{all}},
    \label{eq:Gamma}
\end{equation}
where $N_{1,2}$ are the number of pebbles accreted on bodies 1 and 2, respectively. $N_\mathrm{all}$ is the total umber of released pebbles. $\Gamma=1$ applies single body containing the binary mass. The resulting $\Gamma$ values for our parameter study are shown in Figure \ref{fig:2-5aures1}, for 2.5 au and 39 au. The accretion efficiency can drop to as low as $\Gamma \sim 0.4$ for the maximum Stokes numbers considered at 39 au.

Knowing the accretion efficiency $\Gamma$ of the binary system, we can relate the growth time of the binary system to the growth time of a single body with the same mass. That is, in the pebble accretion regime, the growth timescale $t_\mathrm{growth}$ of a single body with radius $R$, internal density $\rho_\bullet$ and mass $M$, is given by \citep{Visser_2016}:
\begin{equation}
        t_\mathrm{growth} = \frac{M}{\dot{M}} = \frac{4\rho_\bullet R}{3v_\mathrm{hw}\rho_\mathrm{p}f_\mathrm{coll}},
        \label{eq:t_growth_single}
\end{equation}
where $\rho_\mathrm{p}$ is the spatial density of solid particles and $f_\mathrm{coll}$ the collision factor/efficiency. In the next section we determine the relative growth timescales of the binary components based on this analysis.

\subsection{Relative growth rates}
To see if the binary mass ratio will shift towards unity durng growth by pebble accretion, we need to look at the normalised growth ratio
\begin{equation}
    \label{eq:epsilontilde} \Tilde{\varepsilon} = \frac{M_2}{M_1}\varepsilon .
\end{equation}
Whenever this ratio $\Tilde{\varepsilon}$ dips below one, the binary will grow towards equal mass. In the top parts of figures \ref{fig:2-5aures} and \ref{fig:39aures} $\Tilde{\varepsilon}$ is shown as a function of the pebble Stokes number $\tau_\mathrm{s}$, for various combinations of our key parameters.
There is a clear regime, an interval of Stokes numbers, where the mass ratio is indeed moving towards equal mass. This is both true in the asteroid belt at 2.5 au, and in the Kuiper belt at 39 au. This effect is seen not only for a moderate mass ratio of $f_m=2$, but also in the more extreme case of $f_m=8$.  It becomes more prevalent when the two objects in the binary are closer together. In Figures \ref{fig:2-5aures} and \ref{fig:39aures} it can be seen that while this is not always the case, it is true for a substantial part of the parameter study, in particular for large Stokes numbers. In this parameter regime, pebble accretion works toward reducing the mass ratio of the binary. The question arises how relevant this effect is. Do bodies spend enough time in this regime to have their mass ratio significantly altered? It comes down to the question of what the growth timescales of these bodies are, the time to $e$-fold the mass of a component.

With the growth timescale derived for a single body and the accretion efficiency $\Gamma$ we can derive the mass accreted by each body over a set amount of time:
\begin{equation}
    \dot{M}_1 + \dot{M_2} = \Gamma\dot{M},
\end{equation}
which can be rewritten to
\begin{align}
    \dot{M}_1 &= \frac{\Gamma\dot{M}}{\left(1+\varepsilon^{-1}\right)},\\
    \dot{M}_2 &= \frac{\Gamma\dot{M}}{\left(1+\varepsilon\right)},
\end{align}
since $\varepsilon = \dot{M}_1/\dot{M}_2$. We now can use the mass ratio $f_m$ such that $M_1 = \frac{f_m}{1+f_m}M$ and $M_2 = \frac{1}{1+f_m}M$. In this way we find the growth timescales of both planetesimals:
\begin{align}
    \label{eq:tgrowth1} t_\mathrm{growth,1} &= \frac{M_1}{\dot{M}_1} = \frac{\left(1 + \varepsilon^{-1}\right)f_m}{\left(1+f_m\right)\Gamma}t_\mathrm{growth} \equiv \chi_1t_\mathrm{growth},\\
    \label{eq:tgrowth2} t_\mathrm{growth,2} &= \frac{M_2}{\dot{M}_2} = \frac{\left(1 + \varepsilon\right)}{\left(1+f_m\right)\Gamma}t_\mathrm{growth} \equiv \chi_2t_\mathrm{growth},
\end{align}
where we have defined $\chi_i$ to be the scalefactor comparing $t_\mathrm{growth}$ of a single body to that of both planetesimals in a binary. The normalised accretion ratio $\Tilde{\varepsilon}$ and the growth timescales of both bodies are shown in the top and in the bottom panels of figures \ref{fig:2-5aures} and \ref{fig:39aures}, respectively. At both 2.5 and 39 au we saw in Figure \ref{fig:2-5aures1} that the efficiency goes down with increasing $\tau_\mathrm{s}$, which can also be seen with the accretion ratio $\varepsilon$. We believe both effects have somewhat the same cause: $\varepsilon$ favours the smaller body since it sweeps up the inspiralling pebbles from the larger mass as described in section \ref{sec:spiralling}, while the efficiency will also go down as the smaller mass throws a significant fraction of these inspiralling pebbles out of the system in close encounters.

\begin{figure*}[t!]
    \centering
    \includegraphics[width=1\textwidth]{Figures/scen.pdf}
    \caption{A sketch of three distinctive cases that characterise the accretion efficiency of the binary components. The red dot indicates the binary barycenter, the small and large black dots the secondary and primary, respectively and circular velocities shown by the black arrows (illustrative, not to scale). Case a): the pebble Stokes number $\tau_\mathrm{s}$ is low, and it is strongly coupled to the gas. It impacts the primary after typically a single encounter and renders the probability low that it will impact the secondary. Case b): the orbital separation $a_\mathrm{b}$ is too wide for the secondary to benefit from accretion on the massive one. Case c): A narrow binary separation combined with the pebble accretion regime in which pebble spirals are ample and dominant. The probability of impact on the secondary is high due to the repeating encounters before the pebble sinks toward the massive body.}
    \label{fig:cases}
\end{figure*}

What can also be clearly seen, is that the relative growth timescale of the larger body is greater than one in almost all of the parameter space, indicating that the growth of a massive body in the pebble accretion regime is slowed down when it has a secondary. In a large part of the parameter space $\chi_2$ of the smaller body drops below 1, indicating that its growth will be accelerated by the presence of the larger partner. Even in the region where the efficiency $\Gamma$ decreases substantially, the growth of the smaller body is faster. That, combined with the fact the larger body grows more slowly, shows that we have a stabilising effect on the mass ratio. Similar-mass binaries are made more common at both 2.5 and 39 au by this process.

For Stokes numbers close to 0.1, which happens to be also the preferred Stokes number regime for triggering the streaming instability \citep{Baietal2010}, the growth timescales of the smaller body can easily be a factor 3-5 shorter than that of the larger body.  So in the time the mass of the large body grows by a factor $e$, the mass of the smaller body may grow by a factor $e^3$ to $e^5$, and the mass ratio would change by a factor $e^2$ to e$^4$ or about 7 to 40.  This clearly demonstrates the strong potential of pebble accretion to create equal-mass binaries, even if the initial binary had a large mass ratio.

\section{Discussion}
\label{sec:3}
\subsection{Pebble trajectory regimes}

We have identified 3 different main regimes that determine the enhancement in accretion rate of the secondary (excluding chaotic paths pebbles can take like in figure \ref{fig:hmf}A, B and F):
\begin{enumerate}
    \item $\tau_\mathrm{s}$ is too low and pebbles are tightly coupled to the gas. The pebbles do not spiral but make a direct impact or typically one loop before impact (Fig. \ref{fig:cases}a). Accretion ratio is in favour of the primary.
    \item Binary separation is too wide, leading to the massive body accreting pebbles in isolation from the smaller one (Fig. \ref{fig:cases}b). Accretion ratio is in favour of the primary.
    \item $\tau_\mathrm{s}$ is in the regime of pebble accretion, and the separation falls within or on the typical radial extent of the spirals. The pebble undergoes tightly wound long-term spiralling inward and inevitably encounters the secondary before reaching the more massive one (Fig. \ref{fig:cases}c). Accretion ratio is in favour of the secondary.
\end{enumerate}
Unsurprisingly, we find the same trend persists for varied orbital distance $r_0$. We show the final accretion efficiency for a distance of $r_0 = 2.5$ au and have verified it shows the same trend for $r_0 = 10$ au in the same manner as Figure \ref{fig:39aures}. While the parameters shift somewhat, the results show the same outcome.

\subsection{Timescale for developing toward equal mass}
It is informative to see non-equal mass binaries growing towards a mass ratio of unity, but it does not give us a definitive timescale of how long it will take to get there. We consider now the timescale to change the mass-ratio $f_m$ by a factor $e$:
\begin{align}
    \nonumber t_\mathrm{em} &= \frac{f_m}{\dot{f_m}} = \left(\frac{1}{1-\Tilde{\varepsilon}^{-1}}\right)\frac{M_1}{\dot{M_1}} = \frac{\Tilde{\varepsilon}}{\Tilde{\varepsilon}-1}t_\mathrm{growth,1}\\
    \label{eq:t_em} &= \frac{\Tilde{\varepsilon}f_m + 1}{\left(\Tilde{\varepsilon}-1\right)\left(1+f_m\right)}\frac{t_\mathrm{growth}}{\Gamma}.
\end{align}
with $\Tilde{\varepsilon} = \varepsilon / f_m < 1$ and both $\dot{f_m}$ and $t_\mathrm{em}$ being negative since we are looking at the time it takes to grow towards equal mass. This equal mass timescale $t_\mathrm{em}$ is plotted in figure \ref{fig:t_em} for our parameter study. We are in an environment where the streaming instability is active or has been active recently, resulting in significant dust settling in the disk. We therefore take for the solid-to-gas ratio a conservative value of 0.1 such that $\rho_p$ from equation \ref{eq:t_growth_single} is given by
\begin{equation}
    \label{eq:solidtogasratio} \rho_p = 0.1\rho_g = 0.1 \frac{\Sigma}{\sqrt{2\pi}H}
\end{equation}
where $\rho_g$ is the density of the gas (see eq.\ \ref{eq:rho}). We have plotted this $t_\mathrm{em}$ in figure \ref{fig:t_em}. For a binary \myrev{with a total mass equal to that of the Pluto-Charon system} at the location of the asteroid belt at 2.5 AU, the timescales to $e$-fold towards unity are well within a Myr. Even at a greater distance of 39 AU, in a substantial part of our parameter space we find timescales shorter than 1 Myr, again implying that pebble accretion has true potential as a formation method of (near to-) equal mass binaries. Even though we have taken the static approach of calculating $t_\mathrm{em}$ by looking at a fixed rather than evolving mass ratio, from the figure we can conclude that $t_\mathrm{em}$ becomes lower with increasing mass ratio $f_m$. Hence, the mass-equality timescale slows down while this process is happening, but initially the masses are rapidly converging.

\myrev{The question arises if the timescales in figure \ref{fig:t_em} hold for smaller binaries than Pluto-Charon. Since $t_\mathrm{growth}$ of a single body at 3 AU is already within a few Myrs once its radius is larger than $\sim$300km \citep{Visser_2016}, we estimate $t_\mathrm{em}$ of binaries with bodies between that and Pluto ($\sim$1200km) to be of the same order as figure \ref{fig:t_em}.}

\begin{figure}
    \centering
    \includegraphics[width=0.5\textwidth]{Figures/massratiotimescale.pdf}
    \caption{The timescale of $e$-folding towards equal mass $t_\mathrm{em}$ as described in equation \ref{eq:t_em} for two tested mass ratios $f_m=[2,8]$ at two different orbital distances $r_0=[2.5,39]$ AU and at different binary separations $a_b$ denoted by the opaqueness of the lines. Note only the values where $\Tilde{\varepsilon} < 1$ are plotted here since we are looking at the times it takes for the mass ratio $f_m$ to grow towards unity, not away from it.}
    \label{fig:t_em}
\end{figure}

\subsection{Limitations of the model}

One important simplification we have made is the assumption of two-dimensional accretion, only looking at particles located in the midplane and ignoring the effects of a vertical distribution of incoming pebbles.  We can speculate that dropping this assumption may reduce the efficiency of the \textit{vacuum cleaning} by the quickly orbiting secondary.  An exploration of this effect would be very useful and should be done. For now, we hypothesise that even though the specific values of growth ratios may differ from the three-dimensional results, the general trends will remain. The parameter space of Stokes numbers, $\tau_\mathrm{s}$ where the growth ratio flips in favour of the smaller body, will also remain largely the same. Therefore, we think the 3 main regimes of determining accretion rates we found in binaries will also remain the same as in our two-dimensional case.

We are ignoring the effect of gas drag on the binary itself. While this assumption is certainly correct during the computation of the trajectory of a single pebble, over long evolutionary times it may affect the orbit of the binary by removing angular momentum from it.

In this work we have only studied considered purely circular orbits in our binary systems. Since truly circular orbits are rarely ever seen, our results might differ if we also simulate elliptical orbits. Most observed binaries that are in close orbits have been tidally circularised \citep{Nolletal2020} and we find the assumption for circular orbits justified. We estimate however the trends will again, stay largely the same for eccentric binaries due to the spiralling nature of pebbles in the "die-hard" pebble accretion regime.

We have only considered prograde orbital orientations for the binary mutual motion. The reason for this is that binaries that form in the context of the streaming instability show a clear preference for prograde orbits and is also the predominant preference in observations of the cold classical Kuiper belt population  \citep{Grundyetal2019,nesvorny2020binary,VisserandBrouwers2022}.

\section{Conclusions}
\label{sec:4}
In this paper, we have studied the growth and evolution of a binary planet (or planetesimal) system subject to pebble accretion. Specifically, we have investigated the accretion efficiency of the individual binary companions and the binary system as a whole for a variety of parameters such as Stokes number, binary separation, and binary mass ratio.
If the binary components are pebble accreting with a mass ratio of unity, they accrete pebbles at an equal rate, as expected from symmetry arguments. If the mass-ratio is not unity, we arrive at the following conclusions:

\begin{enumerate}
    \item A single planetary body that is accreting pebbles will in general accrete more efficiently in a binary system with a more massive companion, if pebbles are slowly spiralling toward the binary center-of-mass and these spirals extend to the length of the binary separation distance $a_\mathrm{b}$ or larger.
    \item In that case, the mass ratio starts off above unity and the growth rate of the smaller body can be accelerated whilst the more massive one grows more slowly, pushing the binary system toward a mass ratio of unity. For Stokes numbers $0.01 \leq \tau_s \sim 0.1$ the growth timescale of the smaller body can be three to five times shorter, changing the mass ratio quickly.
    \item Generally, three regimes can be distinguished: (i) Stokes number are too small and pebbles are tightly coupled to the gas. These pebbles impact the more massive body, typically after a single encounter, with no accretion advantage for the secondary. (ii)  The same hold when Stokes numbers are too large and pebbles meet the binary on ballistic orbits. (iii) Pebbles are captured by the primary in orbits wider than the binary separation. During the in-spiralling, the pebble has a high probability to be swept up by the secondary, resulting in a converging mass ratio.
\end{enumerate}

\begin{acknowledgements}
We would like to thank J. Groot, G. Koning, R. M. van der Linden \& M. Rustenburg for their insightful comments and discussions. We thank everyone at the disk meeting for feedback and improvements to the manuscript. RGV acknowledges funding from the Dutch Research Council, ALWGO/15-01.
\end{acknowledgements}

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


Experience of working with people who have left long-stay hospital would be an advantage.
Richard needs a mixture of people for his team, he has a cracking sense of humour and likes a bit of banter and so he wants some humorous people but he also needs thoughtful people, people who will understand and have empathy for his situation. He wants a committed team, people he can get to know and enjoy spending time with and people who will not shy away from challenges when they arise. He loves to cook but enjoys a takeaway now and again and he is very knowledgeable about lots of different sports, Liverpool FC are his team and he is keeping a keen on the results just now. He also follows cricket and enjoys watching Yeovil and Taunton play.


text:
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"Sales is really establishing one on one and nurturing that to lead to business. I think lawyers do that every day. I don't think they do it in a systematic approach. That's our job — to leverage the successful ones and communicate that to the firm," Rubbo said.
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"Everyone has their different ways of doing things. I've seen lawyers who are great minders of relationships and they have built a huge practice because they are so good at it and they're always thinking about it," said Frantz.
Technology has been one way to aid sales in firms such as McCarthy Tétrault, which has developed Customer Relationship Management software that's based on products such as Salesforce but specific to the firm's needs, said Rubbo.
Moving in that direction makes sense in an age where iPhones and Samsung phones are the conduits for sharing information in the industry, Frantz said.
Rubbo said the process of implementing the software — which included an executive sponsor, a steering committee and a pilot — showed the importance of the existing culture in the firm. He said the lawyers in the pilot showed the CRM team that they were using the sales technology in unexpected ways.
Events can drive business if lawyers are equipped with a list of targets in actually pursuing a lead at an event, as opposed to chit-chat, said Rubbo.
"Marry up each client with one or two people they can talk to. Its awkward to be at an art gallery and say, 'Can we have your labour employment work?'" said Frantz.
Nonetheless, Stojanovic said she keeps the focus on the clients.
"Things are changing. The accounting and consulting firms are eating our lunch. How do we combat that? How I've approached it is focusing on the high-return investments. Every day we can be doing golf sponsorships and buying tables at fundraisers, but the best thing is to focus on your key clients," said Stojanovic.


Dansk Dinnerware, Classic Fjord Nordic Blue, Replacement China, discontinued china pattern made in Portugal.
Modern Scandinavian design with graceful shapes distinguishes Classic Fjord dinnerware. Dansk serves up this beautiful stoneware in unconventional shapes that are part round, part square, and totally fresh. Mix and match with the other Classic Fjord collections. Introduced in 2013. Microwave and dishwasher safe.


In January, our fourth grade students spent time discussing the ACS core ideology and values and linking them to the IB Learner Profiles. These ten attributes are highly valued by our school: inquirer, knowledgeable, thinker, communicator, principled, open-minded, caring, risk-taker, balanced, reflective.
In groups, the students identified activities they had experienced at school and created a visual presentation to represent their ideas.
After the Core Ideology Day students were invited in small groups to discuss how they use technology at school across all subject areas and in particular how it helps them to support the core values of the school. This is a great way to discuss with students how they use technology at school and beyond the school gates. Many students don't see the off-line and on-line worlds as being separate and I find it very useful asking them to discuss the best things they like to do with technology as well as their concerns.
One of the students, Eliza, was very eloquent and we took her words and created the movie opposite and called it Eliza's Journey. She explains how technology allows her to communicate and co-operate with other people, both in school and across the world. How she needs to be responsible when using technology and likes helping other, especially the younger students to make good decisions. We hope you enjoy the rest of her story.
Eliza's Journey from ACS HILLINGDON HS on Vimeo.


We would love the opportunity to serve you as a client.
The full scale cost for services is $135.00/session (individual/couples/family) or $75.00/session (group). At this time, all of our clinicians are private pay only, but can provide the documentation needed for out of network reimbursement.
Forms of payment accepted include cash/check/credit card.
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Click here to locate the necessary forms you will need to complete before your first visit.
With this information, we can match you with the staff members best suited to helping you meet your goals. The intake appointment usually lasts 45-60 minutes and allows you to see the facility and meet the treatment team. Most likely, you will not begin working with the horses until at least your second appointment. We generally see clients weekly, bi-weekly or monthly and schedule appointments six days a week, with the exception of Sunday. Most of the time we are working outside, so we are often weather and sunset dependent.
You may contact us at 704-608-8441 or info@tripleplayfarm.com.


St. Brigid's bell rings on Avenue B.
Holly waves hello from a garden.
"Winter's Dream" by Tchaikovsky plays.
All I can say is CUCKOO!
and pile love around the pilings.
Chocolate covered cherries for Dad.
White lace for Mom's dresser.
and count every pregnant hour.
Calling all angels—stand and deliver.
Jeffrey Cyphers Wright is a publisher, critic, eco-activist, artist, and impresario, who is best known as a poet. He is the author of 16 books of verse, including Blue Lyre from Dos Madres Press, and Fake Lies from Fell Swoop. He received an MFA in Poetry from Brooklyn College where he studied with Allen Ginsberg and also taught. Currently, Wright stages events at KGB Lit Bar, Howl Happening, and La MaMa ETC in NYC, in conjunction with his art and poetry journal, Live Mag! He is a regular contributor to American Book Review and ArtNexus. He is a Kathy Acker Award recipient and Puschcart Prize nominee for 2018.


11:03 does anybody have recommendations for FP specific algorithms/data structurs texts?
11:14 rhickey: how much work would it be to replace all references to a datastructure with a weak reference?
11:15 rhickey: arohner: for me to change vars?
11:16 rhickey: what is the use case?
11:20 arohner: because of things like conj?
11:23 arohner: is there any way to identify what shares structure, or a way to split the two?
14:27 Chouser: The clojure.set operations, by virtue of returning sets, are eager. However, if they returned seqs many could be lazy. I wonder if this would generally be of any benefit.
14:30 rhickey: Chouser: which ones?
14:32 Chouser: I haven't picked trhough all of them, but union, difference, and intersection each only need to access one of their inputs randombly -- the other input and the output could be lazy seqs.
14:36 Chouser: sure. I still don't know if there would often be any use or benefit to the seq forms. It was just an observation.
14:37 rhickey: Chouser: do you like it?
14:37 Chouser: very much -- it's stimulating a lot of thought.
14:38 arohner: what is Tar Pit?
14:38 Chouser: yes. still looking for the link.
14:41 Chouser: I think the ICFP problem would be an easy fit for separating as the paper describes.
14:42 The functional business of deriving useful state from the textual input felt pretty clean to me in Clojure.
14:43 I wasn't thinking too clearly about how to store that state, so that's where my solution starts to get messy.
14:43 And finally the "logic" part for deciding what commands to send is a tiny part of my final code base -- it is also rather dumb and yet still overly complicated.
14:44 I'm fascinated by the thought of replacing the logic part with some set of rules to be given to a rule engine.
14:45 Chouser: This paper is certainly helping me see why you'd choose to work on that next. I was rather surprised when you first mentioned it.
14:52 Chouser: I still feel like I need an efficient mechanism for backing a collection to disk, specifically a collection in a ref.
14:53 STM makes it pretty easy to correctly snapshot an in-memory collection to disk (for example with prn), and of course you can read in such a collection from disk at startup.
14:54 but it seems a shame to write out the whole collection when you, say, add an item to a set. And the whole thing breaks down if your data is too large for RAM.


If there's one thing that Osaka has more of than any other city in Japan (in fact, there are many things), it's underground. First of all, let me remind readers that Japanese cities developed differently than many cities in the West, and there is generally more than one "city center" or "downtown." In Osaka, the two largest are called Umeda and Namba, often called Kita ("north") and Minami ("south") by locals because of their geographical locations.
Even Frommer's claims that "Osaka must rank as one of the world's leading cities in underground shopping arcades." According to Wikipedia numbers, of the top five underground shopping districts in Japan, two are in Osaka (Crysta Nagahori at 81,765 m² in size and Japan's biggest, and Diamor Osaka at 42,977 m²), and the total number of underground shops/restaurants exceeds 1,200. Namba and Umeda have at least as much, if not more, underground as they do above ground and in the sky. Almost any main street has corridors running underneath it with restaurants, arcades, cafes, bars, and shops of all varieties, and layered underneath those are subway lines, rail lines and parking lots. If it's raining outside, or if you are in the midst of a sweltering Kansai summer there's really no need to worry because you can often get from the train station to your destination without ever seeing the sky.
Some of the larger underground complexes include Whity, Diamor, Dojima, Gare, and the Hilton shopping complex in Umeda, Namba Walk and Nan-Nan Town in the Namba area, and Crysta Nagahori running between Shinsaibashi and Nagahoribashi Stations (underneath Nagahori-dori). Other complex such as OCAT, Namba City, and Hankyu Sanbangai have portions above- and below-ground. There are also a number of ground-level, outdoor, covered shopping arcades, the most famous being the Shinsaibashi, Tenjinbashi, and Hankyu Higashi-dori shopping arcades and the Kuromon fresh food market. The outdoor Shinsaibashi arcade is so crowded that it is air-conditioned in the summer.
These trends follow the general theme in Osaka: many of the best things about this city are not readily visible, but if you are willing explore a little, amazing experiences are waiting just below the surface.


As well as our preconfigured packages, you can customise these or create your own. You can add any of our soft play with any of our Bouncy Castles or Slides to create your own package. If you wanted in under a party tent in your back garden you could add this to your party package. Better still why not have a fair theme and add one of our fairground attractions with some of our side stalls. Whatever package you would like with our equipment just contact us with your ideas and requirements for your tailored event needs.