Collaborative Research: Understanding Compact Binary Star Formation with the First Gravitational Wave Detections

合作研究：通过首次引力波探测了解致密双星的形成

• 批准号: 1716394
• 负责人: Bangalore Sathyaprakash
• 金额: $ 23.93万
• 依托单位: Pennsylvania State Univ University Park
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2017
• 资助国家: 美国
• 起止时间: 2017-07-01 至 2020-06-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1716394&HistoricalAwards=false
• 关键词: Collaborative; Research; Understanding; Compact; Binary

The first detection of gravitational waves (GW) by the LIGO observatory was from the collision of two black holes (BH), which are considered a type of compact binary stars. This has opened up a new window in astronomy, enabling a deeper understanding of the physics of relativity through the study of merging BHs, the objects that bend space and time the most. Since these interactions are so complicated, powerful computer simulations are needed to interpret the science. A collaboration between research groups at the University of Mississippi and Pennsylvania State University will develop and run computer models to better understand the formation and development of compact binary star systems and to more effectively use the rich information from gravitational waves to probe these systems. A related effort is the development of methods to use GW in the future to study dark matter. The research team will also promote scientific literacy by providing astronomy lectures, demonstrations, and hands-on activities to school children and adult citizenry in economically disadvantaged communities in the state of Mississippi and the commonwealth of Pennsylvania. The investigators will carry out two closely related projects to model the gravitational wave astrophysics of compact binary systems. The first project concerns the astrophysical information that can be extracted from the characteristic signature imposed on a gravitational wave signal due to the spin and the orbital precession of coalescing black hole binaries. The team will introduce spin dynamics into compact binary evolution models and track the evolution of BH binaries from formation through merger, including effects such as an initial supernova kick, mass transfer and spin-orbit coupling. An offshoot of this work is to investigate bounds on ultra-light bosonic dark matter though its possible GW signature. The second project will involve inferring compact binary population models from a catalog of gravitational wave observations. The team will put together a database of evolutionary models and work to distinguish between the predicted observables of the various models. Goals include understanding the distribution of BH masses, spins, and merger rates and the properties of the stochastic GW background. The principal investigators will mentor a graduate student and postdoctoral researcher and plan to organize two workshops on strong gravity and binary dynamics and to lecture at international graduate schools on work related to the proposal.

LIGO天文台首次探测到引力波（GW）来自两个黑洞（BH）的碰撞，这两个黑洞被认为是一种紧凑的双星。这为天文学打开了一扇新的窗口，通过对黑洞合并的研究，使人们能够更深入地理解相对论的物理学，黑洞是弯曲空间和时间最多的物体。 由于这些相互作用如此复杂，因此需要强大的计算机模拟来解释科学。 密西西比大学和宾夕法尼亚州立大学的研究小组之间的合作将开发和运行计算机模型，以更好地了解紧凑的双星星星系统的形成和发展，并更有效地利用引力波的丰富信息来探测这些系统。一个相关的努力是开发未来使用GW研究暗物质的方法。研究小组还将通过为密西西比州和宾夕法尼亚州经济贫困社区的学童和成年公民提供天文学讲座、演示和动手活动，促进科学素养。研究人员将开展两个密切相关的项目，以模拟紧凑双星系统的引力波天体物理学。第一个项目涉及的天体物理信息，可以从施加在引力波信号由于自旋和轨道进动的合并黑洞双星的特征签名提取。该团队将把自旋动力学引入到紧凑的双星演化模型中，并跟踪BH双星从形成到合并的演化，包括初始超新星反冲、质量转移和自旋轨道耦合等效应。这项工作的一个分支是研究超轻玻色子暗物质的界限，尽管它可能有GW签名。第二个项目将涉及从引力波观测目录中推断出紧凑的双星总体模型。该团队将建立一个进化模型数据库，并努力区分各种模型的预测观测值。目标包括了解BH质量，自旋和合并率的分布和随机GW背景的属性。主要研究人员将指导一名研究生和博士后研究员，并计划组织两次关于强引力和二元动力学的讲习班，并在国际研究生院就与该提案有关的工作发表演讲。

项目成果

Implications of Binary Black Hole Detections on the Merger Rates of Double Neutron Stars and Neutron Star–Black Holes

• DOI: 10.3847/2041-8213/aa9271
• 发表时间: 2017-08
• 期刊: The Astrophysical Journal Letters
• 作者: Anuradha Gupta;K. Arun;K. Arun;B. Sathyaprakash;B. Sathyaprakash

Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817

• DOI: 10.3847/1538-4357/ab0f3d
• 发表时间: 2018-10
• 期刊: The Astrophysical Journal
• 作者: The Ligo Scientific Collaboration;T. Abbott;R. Abbott;T. Abbott;F. Acernese;K. Ackley;C. Adams;T. Adams;P. Addesso;R. Adhikari;V. Adya;C. Affeldt;B. Agarwal;M. Agathos;K. Agatsuma;N. Aggarwal;O. Aguiar;L. Aiello;A. Ain;P. Ajith;B. Allen;G. Allen;A. Allocca;M. Aloy;P. Altin;A. Amato;A. Ananyeva;S. Anderson;W. Anderson;S. Angelova;S. Antier;S. Appert;K. Arai;M. Araya;J. Areeda;M. Arène;N. Arnaud;S. Ascenzi;G. Ashton;M. Ast;S. Aston;P. Astone;D. V. Atallah;F. Aubin;P. Aufmuth;C. Aulbert;K. AultONeal;C. Austin;A. Ávila-Álvarez;S. Babak;P. Bacon;F. Badaracco;M. Bader;S. Bae;P. Baker;F. Baldaccini;G. Ballardin;S. Ballmer;S. Banagiri;J. Barayoga;S. Barclay;B. Barish;D. Barker;K. Barkett;S. Barnum;F. Barone;B. Barr;L. Barsotti;M. Barsuglia;D. Barta;J. Bartlett;I. Bartos;R. Bassiri;A. Basti;J. Batch;M. Bawaj;J. Bayley;M. Bazzan;B. B'ecsy;C. Beer;M. Bejger;I. Belahcene;A. Bell;D. Beniwal;M. Bensch;B. Berger;G. Bergmann;S. Bernuzzi;J. Bero;C. Berry;D. Bersanetti;A. Bertolini;J. Betzwieser;R. Bhandare;I. Bilenko;S. Bilgili;G. Billingsley;C. Billman;J. Birch;R. Birney;O. Birnholtz;S. Biscans;S. Biscoveanu;A. Bisht;M. Bitossi;M. Bizouard;J. Blackburn;J. Blackman;C. Blair;D. Blair;R. Blair;S. Bloemen;O. Bock;N. Bode;M. Boer;Y. Boetzel;G. Bogaert;A. Bohé;F. Bondu;E. Bonilla;R. Bonnand;P. Booker;B. A. Boom;C. Booth;R. Bork;V. Boschi;S. Bose;K. Bossie;V. Bossilkov;J. Bosveld;Y. Bouffanais;A. Bozzi;C. Bradaschia;P. Brady;A. Bramley;M. Branchesi;J. Brau;T. Briant;F. Brighenti;A. Brillet;M. Brinkmann;V. Brisson;P. Brockill;A. Brooks;D. Brown;S. Brunett;C. Buchanan;A. Buikema;T. Bulik;H. Bulten;A. Buonanno;D. Buskulic;C. Buy;R. Byer;M. Cabero;L. Cadonati;G. Cagnoli;C. Cahillane;J. C. Bustillo;T. Callister;E. Calloni;J. Camp;M. Canepa;P. Canizares;K. Cannon;H. Cao;J. Cao;C. Capano;E. Capocasa;F. Carbognani;S. Caride;M. Carney;J. C. Diaz;C. Casentini;S. Caudill;M. Cavaglià;F. Cavalier;R. Cavalieri;G. Cella;C. Cepeda;P. Cerd'a-Dur'an;G. Cerretani;E. Cesarini;O. Chaibi;S. 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Hennig;A. Heptonstall;F. Hernandez;M. Heurs;S. Hild;T. Hinderer;D. Hoak;S. Hochheim;D. Hofman;N. Holland;K. Holt;D. Holz;P. Hopkins;C. Horst;J. Hough;E. Houston;E. Howell;A. Hreibi;E. Huerta;D. Huet;B. Hughey;M. Hulko;S. Husa;S. Huttner;T. Huynh--Dinh-T.-Huynh--Dinh-1381195806;A. Iess;N. Indik;C. Ingram;R. Inta;G. Intini;H. N. Isa;J. Isac;M. Isi;B. Iyer;K. Izumi;T. Jacqmin;K. Jani;P. Jaranowski;D. S. Johnson;W. Johnson;D. Jones;R. Jones;R. Jonker;L. Ju;J. Junker;C. Kalaghatgi;V. Kalogera;B. Kamai;S. Kandhasamy;G. Kang;J. Kanner;S. Kapadia;S. Karki;K. Karvinen;M. Kasprzack;W. Kastaun;M. Katolik;S. Katsanevas;E. Katsavounidis;W. Katzman;S. Kaufer;K. Kawabe;N. V. Keerthana;F. K'ef'elian;D. Keitel;A. Kemball;R. Kennedy;J. Key;F. Khalili;B. Khamesra;H. Khan;I. Khan;S. Khan;Z. Khan;E. Khazanov;N. Kijbunchoo;Chunglee Kim;J. Kim;K. Kim;W. Kim;W. Kim;Y. Kim;E. King;P. King;M. Kinley-Hanlon;R. Kirchhoff;J. Kissel;L. Kleybolte;S. Klimenko;T. Knowles;P. Koch;S. Koehlenbeck;S. Koley;V. Kondrashov;A. Kontos;M. Korobko;W. Korth;I. Kowalska;D. Kozak;C. Kramer;V. Kringel;B. Krishnan;A. Kr'olak;G. Kuehn;P. Kumar;R. Kumar;S. Kumar;L. Kuo;A. Kutynia;S. Kwang;B. Lackey;K. Lai;M. Landry;R. Lang;J. Lange;B. Lantz;R. Lanza;A. Lartaux-Vollard;P. Lasky;M. Laxen;A. Lazzarini;C. Lazzaro;P. Leaci;S. Leavey;C. Lee;H. Lee;H. Lee;H. W. Lee;K. Lee;J. Lehmann;A. Lenon;M. Leonardi;N. Leroy;N. Letendre;Y. Levin;J. Li;T. G. F. Li;X. Li;S. Linker;T. Littenberg;J. Liu;X. Liu;R. K. Lo;N. Lockerbie;L. London;A. Longo;M. Lorenzini;V. Loriette;M. Lormand;G. Losurdo;J. Lough;C. Lousto;G. Lovelace;H. Luck;D. Lumaca;A. Lundgren;R. Lynch;Y. Ma;R. Macas;S. Macfoy;B. Machenschalk;M. Macinnis;D. Macleod;I. M. Hernandez;F. Magaña-Sandoval;L. M. Zertuche;R. Magee;E. Majorana;I. Maksimovic;N. Man;V. Mandic;V. Mangano;G. Mansell;M. Manske;M. Mantovani;F. Marchesoni;F. Marion;S. M'arka;Z. M'arka;C. Markakis;A. Markosyan;A. Markowitz;E. Maros;A. Marquina;F. Martelli;L. Martellini;I. Martin;R. Martin;D. 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Wysocki;S. Xiao;W. Yam;H. Yamamoto;C. Yancey;L. Yang;M. Yap;M. Yazback;Hang Yu;Haocun Yu;M. Yvert;A. Zadro.zny;M. Zanolin;T. Zelenova;J. Zendri;M. Zevin;J. Zhang;L. Zhang;M. Zhang;T. Zhang;Y.H. Zhang;C. Zhao;M. Zhou;Z. Zhou;S. Zhu;X. Zhu;A. Zimmerman;M. Zucker;J. Zweizig

Comparison of post-Newtonian mode amplitudes with numerical relativity simulations of binary black holes

后牛顿模式振幅与双黑洞数值相对论模拟的比较

• DOI: 10.1088/1361-6382/ab6a21
• 发表时间: 2020
• 期刊: Classical and Quantum Gravity
• 影响因子: 3.5
• 作者: Borhanian, S;Arun, K G;Pfeiffer, H P;Sathyaprakash, B S
• 通讯作者: Sathyaprakash, B S

A no-hair test for binary black holes

双黑洞的无毛发测试

• DOI: 10.1103/physrevd.99.104056
• 发表时间: 2019
• 期刊: Physical Review D
• 影响因子: 5
• 作者: Dhanpal, Siddharth;Ghosh, Abhirup;Mehta, Ajit Kumar;Ajith, Parameswaran;Sathyaprakash, B. S.
• 通讯作者: Sathyaprakash, B. S.

Calibrating the Cosmic Distance Ladder Using Gravitational-wave Observations

• DOI: 10.3847/1538-4357/ab4c92
• 发表时间: 2019-07
• 期刊: The Astrophysical Journal
• 作者: Anuradha Gupta;D. Fox;B. Sathyaprakash;B. Schutz