Enabling Astronomy with Gravitational Waves

利用引力波实现天文学

• 批准号: ST/F01032X/1
• 负责人: Iain Martin
• 金额: $ 27.77万
• 依托单位: University of Glasgow
• 依托单位国家: 英国
• 项目类别: Fellowship
• 财政年份: 2008
• 资助国家: 英国
• 起止时间: 2008 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FF01032X%2F1
• 关键词: Enabling; Astronomy; Gravitational; Waves

Within the next 6 years, a new generation of more sensitive gravitational wave detectors is expected to start searching for astrophysical sources of gravitational waves. It is widely expected that these instruments will detect gravitational waves within weeks of becoming operational, beginning a new era of astronomy. The research I propose aims to increase the sensitivity these 'second generation' detectors and is critical for the success of planned 'third generation' detectors, which may operate at cryogenic temperatures. Gravitational waves are fluctuations in the curvature of space-time, produced by the asymmetric acceleration of mass and predicted to be emitted by astrophysical objects such as inspiralling binary neutron stars, interacting black holes and supernovae. Current long-baseline gravitational wave detectors use laser interferometry to monitor the relative displacements of test-masses, which are coated to form mirrors that are highly reflective at 1064 nm. These are suspended as pendulums up to several kilometres apart. Gravitational waves are predicted to induce displacements of less than ~10^-19m in the length of the arms. This displacement is so small that that thermally induced vibrations of the mirrors and their suspensions form an important limit to detector sensitivity. In particular, the mechanical dissipation associated with the ion-beam sputtered mirror coatings has been identified as an important noise source which will limit the sensitivity of future detectors. I propose to develop methods of reducing the mechanical loss, and thus the thermal noise contribution, of the reflective coatings which are crucial to the operation of these detectors. This will increase the sensitivity of future detectors, enabling them to search a larger volume of the Universe for sources of gravitational waves. In particular, gravity wave signals from coalescing compact binary systems, such as two orbiting neutron stars, are predicted to be emitted in the frequency band at which coating thermal noise is expected to limit the sensitivity of future detectors. The coatings used in current detectors consist of alternating layers of tantalum pentoxide (tantala) and silica. Experiments have shown that the mechanical dissipation arises primarily from the tantala layers and that the mechanical loss of tantala can be reduced by doping the material with titanium dioxide (titania). My recent research has shown the presence of a low-temperature dissipation peak in a tantala coating doped with titania, which is characteristic of a particular dissipation mechanism, possibly associated with the tantalum-oxygen bond oscillating between two stable energy states. I would undertake a series of experiments to gain an understanding of the fundamental physics associated with mechanical loss in the coating materials. As noted above, cryogenic loss measurements can be a powerful method of understanding the loss mechanisms in a material. In particular, I plan to investigate whether the shape, height and temperature of the low temperature dissipation peak can be altered by varying the doping concentration, or by heat treatment of the coating, with the aim of developing a detailed model of dissipation initially in tantala. I propose to participate in research planned by the LIGO Scientific Collaboration into possible new coating materials and develop models to understand and reduce their mechanical dissipation. The results of these studies should enable me to develop coating designs with lower mechanical loss, and hence thermal noise, than currently possible, with corresponding enhancement to the sensitivity of advanced gravitational wave detectors. This proposed is also critical for the success of future cryogenically cooled gravitational wave detectors such as the 'Einstein Telescope' which is the subject of a current EC FP7 design study.

在未来6年内，新一代更灵敏的引力波探测器有望开始寻找引力波的天体物理来源。人们普遍预计，这些仪器将在投入使用后的几周内探测到引力波，开启天文学的新时代。我提出的研究旨在提高这些“第二代”探测器的灵敏度，这对计划中的“第三代”探测器的成功至关重要，这些探测器可能在低温下工作。引力波是时空曲率中的波动，由质量的不对称加速产生，预计由天体物理物体发射，如螺旋双星、相互作用的黑洞和超新星。目前的长基线引力波探测器使用激光干涉测量法来监测测试质量的相对位移，这些测试质量被涂覆以形成在1064 nm处具有高反射率的镜子。这些卫星被悬挂在相距几公里的空中。引力波预计会在臂的长度上引起小于~10^-19 m的位移。这种位移是如此之小，以至于反射镜及其悬架的热致振动对检测器灵敏度形成重要限制。特别是，与离子束溅射反射镜涂层的机械耗散已被确定为一个重要的噪声源，这将限制未来的探测器的灵敏度。我建议开发的方法，减少机械损失，从而热噪声的贡献，反射涂层，这是至关重要的这些探测器的操作。这将提高未来探测器的灵敏度，使它们能够在更大的宇宙空间中搜索引力波源。特别是，重力波信号从合并紧凑的双星系统，如两个轨道中子星，预计将在频带中发射涂层热噪声预计将限制未来探测器的灵敏度。电流检测器中使用的涂层由五氧化二钽（tantaloa）和二氧化硅交替层组成。实验表明，机械耗散主要来自氧化钽层，并且可以通过用二氧化钛（二氧化钛）掺杂材料来减少氧化钽的机械损耗。我最近的研究表明，在掺杂二氧化钛的钽涂层中存在低温耗散峰，这是一种特殊耗散机制的特征，可能与钽-氧键在两个稳定能态之间振荡有关。我将进行一系列实验，以了解与涂层材料中的机械损耗相关的基本物理学。如上所述，低温损失测量可以是理解材料中损失机制的有力方法。特别是，我计划调查的形状，高度和温度的低温耗散峰是否可以改变通过改变掺杂浓度，或通过热处理的涂层，开发一个详细的模型耗散最初在钽的目的。我建议参加LIGO科学合作组织计划的研究，研究可能的新涂层材料，并开发模型来理解和减少它们的机械耗散。这些研究的结果应该使我能够开发出比目前可能的机械损失更低的涂层设计，从而降低热噪声，并相应提高先进引力波探测器的灵敏度。这一提议对于未来低温冷却引力波探测器的成功也至关重要，例如“爱因斯坦望远镜”，这是目前EC FP 7设计研究的主题。

项目成果

FIRST SEARCH FOR GRAVITATIONAL WAVES FROM THE YOUNGEST KNOWN NEUTRON STAR

首次搜索来自已知最年轻中子星的引力波

• DOI: 10.1088/0004-637x/722/2/1504
• 发表时间: 2010
• 期刊: The Astrophysical Journal
• 作者: Abadie J

Search for gravitational waves associated with the August 2006 timing glitch of the Vela pulsar

搜索与 2006 年 8 月船帆脉冲星计时故障相关的引力波

• DOI: 10.1103/physrevd.83.042001
• 发表时间: 2011
• 期刊: Physical Review D
• 影响因子: 5
• 作者: Abadie J

Search for Gravitational Waves from Compact Binary Coalescence in LIGO and Virgo Data from S5 and VSR1

• DOI: 10.1103/physrevd.82.102001
• 发表时间: 2010-05
• 作者: J. Abadie;B. Abbott;R. Abbott;M. Abernathy;T. Accadia;F. Acernese;C. Adams;R. Adhikari;P. Ajith;B. Allen;G. Allen;E. Ceron;R. Amin;S. Anderson;W. Anderson;F. Antonucci;M. Arain;M. Araya;M. Aronsson;K. Arun;Y. Aso;S. Aston;P. Astone;D. Atkinson;P. Aufmuth;C. Aulbert;S. Babak;P. Baker;G. Ballardin;T. Ballinger;S. Ballmer;D. Barker;S. Barnum;F. Barone;B. Barr;P. Barriga;L. Barsotti;M. Barsuglia;M. Barton;I. Bartos;R. Bassiri;M. Bastarrika;J. Bauchrowitz;T. Bauer;B. Behnke;M. Beker;A. Bellétoile;M. Benacquista;A. Bertolini;J. Betzwieser;N. Beveridge;P. Beyersdorf;S. Bigotta;I. Bilenko;G. Billingsley;J. Birch;S. Birindelli;R. Biswas;M. Bitossi;M. Bizouard;E. Black;J. Blackburn;L. Blackburn;D. Blair;B. Bland;M. Blom;C. Boccara;O. Bock;T. Bodiya;R. Bondarescu;F. Bondu;L. Bonelli;R. Bonnand;R. Bork;M. Born;S. Bose;L. Bosi;B. Bouhou;M. Boyle;S. Braccini;C. Bradaschia;P. Brady;V. Braginsky;J. Brau;J. Breyer;D. Bridges;A. Brillet;M. Brinkmann;V. Brisson;M. Britzger;A. Brooks;Daniel D. Brown;R. Budzyński;T. Bulik;H. Bulten;A. Buonanno;J. Burguet-Castell;O. Burmeister;D. Buskulic;Christelle Lesvigne-Buy;R. Byer;L. Cadonati;G. Cagnoli;J. Cain;E. Calloni;J. Camp;E. Campagna;P. Campsie;J. Cannizzo;K. Cannon;B. Canuel;Junwei Cao;C. Capano;F. Carbognani;S. Caudill;M. Cavaglià;F. Cavalier;R. Cavalieri;G. Cella;C. Cepeda;E. Cesarini;T. Chalermsongsak;E. Chalkley;P. Charlton;É. Chassande-Mottin;S. Chelkowski;Yan Chen;A. Chincarini;N. Christensen;S. Chua;C. Y. Chung;D. Clark;J. Clark;Jh. Clayton;F. Cleva;E. Coccia;C. Colacino;J. Colas;A. Colla;M. Colombini;R. Conte;D. Cook;T. Corbitt;N. Cornish;A. Corsi;C. Costa;J. Coulon;D. Coward;D. Coyne;J. Creighton;T. Creighton;A. Cruise;R. Culter;A. Cumming;L. Cunningham;E. Cuoco;K. Dahl;S. Danilishin;R. Dannenberg;S. D’Antonio;K. Danzmann;K. Das;V. Dattilo;B. Daudert;M. Davier;G. Davies;A. Davis;E. Daw;R. Day;T. Dayanga;R. De;D. DeBra;J. Degallaix;M. Del;V. Dergachev;R. Derosa;R. DeSalvo;P. Devanka;S. Dhurandhar;L. Di;A. Di;I. Di;M. Emilio;A. Di;M. Díaz;A. Dietz;F. Donovan;K. Dooley;E. Doomes;S. Dorsher;E. Douglas;M. Drago;R. Drever;J. Driggers;J. Dueck;J. Dumas;T. Eberle;M. Edgar;M. Edwards;A. Effler;P. Ehrens;G. Ely;R. Engel;T. Etzel;M. Evans;T. Evans;V. Fafone;S. Fairhurst;Yaohui Fan;B. Farr;D. Fazi;H. Fehrmann;D. Feldbaum;I. Ferrante;F. Fidecaro;L. Finn;I. Fiori;R. Flaminio;M. Flanigan;K. Flasch;S. Foley;C. Forrest;E. Forsi;N. Fotopoulos;J. Fournier;J. Franc;S. Frasca;F. Frasconi;M. Frede;M. Frei;Z. Frei;A. Freise;R. Frey;T. Fricke;D. Friedrich;P. Fritschel;V. Frolov;P. Fulda;M. Fyffe;M. Galimberti;L. Gammaitoni;J. Garofoli;F. Garufi;G. Gemme;E. Génin;A. Gennai;Shaon Ghosh;J. Giaime;S. Giampanis;K. Giardina;A. Giazotto;C. Gill;E. Goetz;L. Goggin;G. González;S. Goler;R. Gouaty;C. Graef;M. Granata;A. Grant;S. Gras;C. Gray;R. Greenhalgh;A. Gretarsson;C. Greverie;R. Grosso;H. Grote;S. Grunewald;G. Guidi;E. Gustafson;R. Gustafson;B. Hage;P. Hall;J. Hallam;D. Hammer;G. Hammond;J. Hanks;C. Hanna;J. Hanson;J. Harms;G. Harry;I. Harry;E. Harstad;K. Haughian;K. Hayama;J. Hayau;T. Hayler;J. Heefner;H. Heitmann;P. Hello;Is. Heng;A. Heptonstall;M. Hewitson;S. Hild;E. Hirose;D. Hoak;K. Hodge;K. Holt;D. Hosken;J. Hough;E. Howell;D. Hoyland;D. Huet;B. Hughey;S. Husa;S. Huttner;T. Huynh--Dinh-T.-Huynh--Dinh-1381195806;Ingram;R. Inta;T. Isogai;A. Ivanov;P. Jaranowski;W. Johnson;Dilwyn P. Jones;G. Jones;Russell Jones;L. Ju;P. Kalmus;V. Kalogera;S. Kandhasamy;J. Kanner;E. Katsavounidis;K. Kawabe;S. Kawamura;F. Kawazoe;W. Kells;D. Keppel;A. Khalaidovski;F. Khalili;E. Khazanov;H. Kim;P. King;D. Kinzel;J. Kissel;S. Klimenko;V. Kondrashov;R. Kopparapu;S. Koranda;I. Kowalska;D. Kozak;T. Krause;V. Kringel;S. Krishnamurthy;B. Krishnan;A. Królak;G. Kuehn;J. Kullman;Rakesh Kumar;P. Kwee;M. Landry;M. Lang;B. Lantz;N. Lastzka;A. Lazzarini;P. Leaci;J. Leong;I. Leonor;N. Leroy;N. Letendre;J. Li;Tgf. Li;H. Lin;P. Lindquist;N. Lockerbie;D. Lodhia;M. Lorenzini;V. Loriette;M. Lormand;G. Losurdo;P. Lu;J. Luan;M. Lubinski;A. Lucianetti;H. Lück;A. Lundgren;B. Machenschalk;M. Macinnis;M. Mageswaran;K. Mailand;E. Majorana;C. Mak;I. Maksimovic;N. Man;I. Mandel;V. Mandic;M. Mantovani;F. Marchesoni;F. Marion;S. Márka;Z. Márka;E. Maros;J. Marque;F. Martelli;I. Martin;R. Martin;J. Marx;K. Mason;A. Masserot;F. Matichard;L. Matone;R. Matzner;N. Mavalvala;Robert McCarthy-;D. McClelland;S. Mcguire;G. Mcintyre;G. McIvor;D. McKechan;G. Meadors;M. Mehmet;T. Meier;A. Melatos;A. Melissinos;G. Mendell;D. Menendez;R. Mercer;L. Merill;S. Meshkov;C. Messenger;Meyer;H. Miao;C. Michel;L. Milano;J. Miller;Y. Minenkov;Y. Mino;S. Mitra;V. Mitrofanov;G. Mitselmakher;R. Mittleman;B. Moe;M. Mohan;S. Mohanty;S. Mohapatra;D. Moraru;J. Moreau;G. Moreno;N. Morgado;A. Morgia;K. Mors;S. Mosca;V. Moscatelli;K. Mossavi;B. Mours;C. Mow-Lowry;G. Mueller;S. Mukherjee;A. Mullavey;Hm. Ller-Ebhardt;J. Munch;P. Murray;T. Nash;R. Nawrodt;J. Nelson;I. Neri;G. Newton;E. Nishida;A. Nishizawa;F. Nocera;D. Nolting;E. Ochsner;J. O'Dell;G. Ogin;R. Oldenburg;B. O'reilly;R. O’Shaughnessy;C. Osthelder;D. Ottaway;R. Ottens;H. Overmier;B. Owen;A. Page;G. Pagliaroli;L. Palladino;C. Palomba;Yi Pan;C. Pankow;F. Paoletti;M. Papa;S. Pardi;M. Pareja;M. Parisi;A. Pasqualetti;R. Passaquieti;D. Passuello;P. Patel;D. Pathak;M. Pedraza;L. Pekowsky;S. Penn;C. Peralta;A. Perreca;G. Persichetti;M. Pichot;M. Pickenpack;F. Piergiovanni;M. Pietka;L. Pinard;I. Pinto;M. Pitkin;H. Pletsch;M. Plissi;R. Poggiani;F. Postiglione;M. Prato;V. Predoi;L. Price;M. Prijatelj;M. Principe;R. Prix;G. Prodi;L. Prokhorov;O. Puncken;M. Punturo;P. Puppo;V. Quetschke;F. Raab;D. Rabeling;T. Radke;H. Radkins;P. Raffai;M. Rakhmanov;B. Rankins;P. Rapagnani;V. Raymond;V. Re;C. Reed;T. Reed;T. Regimbau;S. Reid;D. Reitze;F. Ricci;R. Riesen;K. Riles;P. Roberts;N. Robertson;F. Robinet;C. Robinson;E. Robinson;A. Rocchi;S. Roddy;C. Röver;L. Rolland;J. Rollins;J. Romano;R. Romano;J. Romie;D. Rosińska;S. Rowan;A. Rüdiger;P. Ruggi;K. Ryan;S. Sakata;M. Sakosky;F. Salemi;L. Sammut;Ls. La Jordana De;V. Sandberg;V. Sannibale;L. Santamaría;G. Santostasi;S. Saraf;B. Sassolas;B. Sathyaprakash;S. Sato;M. Satterthwaite;P. Saulson;R. Savage;R. Schilling;R. Schnabel;R. Schofield;B. Schulz;B. Schutz;P. Schwinberg;J. Scott;S. Scott;A. Searle;F. Seifert;D. Sellers;A. Sengupta;D. Sentenac;A. Sergeev;D. Shaddock;B. Shapiro;P. Shawhan;D. Shoemaker;A. Sibley;X. Siemens;D. Sigg;A. Singer;A. Sintes;G. Skelton;B. Slagmolen;J. Slutsky;Jr. Smith;Smith;N. Smith;K. Somiya;B. Sorazu;F. Speirits;L. Sperandio;A. Stein;L. Stein;S. Steinlechner;S. Steplewski;A. Stochino;R. Stone;K. Strain;S. Strigin;A. Stroeer;R. Sturani;A. Stuver;T. Summerscales;M. Sung;S. Susmithan;P. Sutton;B. Swinkels;D. Talukder;D. Tanner;S. Tarabrin;Jr. Taylor;Robert J. Taylor;P. Thomas;K. Thorne;K. Thorne;E. Thrane;A. Ring;C. Titsler;K. Tokmakov;A. Toncelli;M. Tonelli;O. Torre;C. Torres;C. Torrie;E. Tournefier;F. Travasso;G. Traylor;M. Trias;J. Trummer;K. Tseng;L. Turner;D. Ugolini;K. Urbanek;H. Vahlbruch;B. Vaishnav;G. Vajente;M. Vallisneri;Jfj. Den Brand Van;Den Broeck C. Van;S. Van;A. Van;V. Van;S. Vass;R. Vaulin;M. Vavoulidis;A. Vecchio;G. Vedovato;J. Veitch;P. Veitch;C. Veltkamp;D. Verkindt;F. Vetrano;A. Viceré;A. Villar;Y. Vinetj;H. Vocca;C. Vorvick;S. Vyachanin;S. Waldman;L. Wallace;A. Wanner;R. Ward;M. Was;P. Wei;M. Weinert;A. Weinstein;R. Weiss;L. Wen;S. Wen;P. Wessels;M. West;T. Westphal;K. Wette;J. Whelan;S. Whitcomb;D. White;B. Whiting;C. Wilkinson;P. Willems;L. Williams;B. Willke;L. Winkelmann;W. Winkler;C. Wipf;A. Wiseman;G. Woan;R. Wooley;J. Worden;I. Yakushin;H. Yamamoto;Kazuhiro Yamamoto;D. Yeaton-Massey;S. Yoshida;P. Yu;M. Yvert;M. Zanolin;L. Zhang;Zhen Zhang;Chunnong Zhao;N. Zotov;M. Zucker;J. Zweizig

Calibration of the LIGO gravitational wave detectors in the fifth science run

第五次科学运行中 LIGO 引力波探测器的校准

• DOI: 10.1016/j.nima.2010.07.089
• 发表时间: 2010
• 期刊: Accelerators, Spectrometers, Detectors and Associated Equipment
• 作者: Abadie J

SEARCH FOR GRAVITATIONAL WAVE BURSTS FROM SIX MAGNETARS

• DOI: 10.1088/2041-8205/734/2/l35
• 发表时间: 2011-06-20
• 期刊: ASTROPHYSICAL JOURNAL LETTERS
• 影响因子: 7.9
• 作者: Abadie, J.;Abbott, B. P.;Yamaoka, K.
• 通讯作者: Yamaoka, K.