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.

在接下来的6年内，新一代更敏感的引力波检测器有望开始寻找引力波的天体物理来源。人们普遍期望这些工具将在运营后的几周内检测到引力波，从而开始一个新的天文学时代。我提出的研究旨在提高这些“第二代”探测器的敏感性，并且对于计划的“第三代”探测器的成功至关重要，该检测器可能在低温温度下运行。引力波是时空的曲率波动，是由质量不对称加速产生的，并预测由天体物理物体（例如灵感的二进制中子星星），相互作用的黑洞和超新星相互作用。当前的长降压重力波检测器使用激光干涉仪监测测试量的相对位移，这些测试量的相对位移被覆盖以形成在1064 nm处高度反射的镜子。这些被悬挂在相距不高几公里的摆时。预计重力波在臂长度内诱导小于10^-19m的位移。这种位移是如此之小，以至于镜子的热诱导振动及其悬浮液构成了检测器灵敏度的重要限制。特别是，与离子光束溅射镜涂层相关的机械耗散已被确定为重要的噪声源，它将限制未来检测器的灵敏度。我建议开发减少机械损失的方法，从而减少对这些检测器运行至关重要的反射涂层的热噪声贡献。这将增加未来探测器的灵敏度，从而使他们能够搜索大量的宇宙以获取引力波的来源。特别是，预测在涂层热噪声限制未来探测器的灵敏度的频带中，预计来自聚合紧凑型二元系统的重力波信号，例如两个轨道中子星。当前探测器中使用的涂层包括坦塔尔五氧化坦原（Tantala）和二氧化硅的交替层。实验表明，机械耗散主要来自Tantala层，并且可以通过将材料与二氧化钛（Titania）掺杂材料来减少Tantala的机械损失。我最近的研究表明，在掺杂二氧化钛的tantala涂层中存在低温耗散峰，这是一种特定的耗散机制的特征，可能与两个稳定能量状态之间的坦塔alum氧键振荡有关。我将进行一系列实验，以了解与涂料材料机械损失相关的基本物理学。如上所述，低温损失测量可能是了解材料中损失机制的有力方法。特别是，我计划研究是否可以通过改变掺杂浓度或对涂层的热处理来改变低温耗散峰的形状，高度和温度，以开发最初在Tantala中开发详细的耗散模型。我建议参与Ligo Scientific Shocient的研究研究，以了解可能的新涂料材料，并开发模型以理解和减少其机械耗散。这些研究的结果应该使我能够开发具有较低机械损耗的涂层设计，因此，与当前可能的热噪声相对应，并增强了对晚期重力波检测器的灵敏度的相应增强。这项提出的对于未来低温冷却引力检测器（例如“爱因斯坦望远镜”）的成功也至关重要，这是当前EC FP7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 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

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 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.

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