GWAstro.bib

@Book{Wald1984,
  author    = {Wald, Robert M.},
  publisher = {University of Chicago Pr.},
  title     = {General Relativity},
  year      = {1984},
  isbn      = {0-226-87033-2},
  ean       = {9780226870335},
  url       = {https://www.ebook.de/de/product/3238000/robert_m_wald_general_relativity.html},
}

@Book{王2020,
  author    = {王, 运永},
  publisher = {科学出版社},
  title     = {引力波探测},
  year      = {2020},
  isbn      = {978-7-03-064766-5},
}

@Article{Sathyaprakash2009,
  author       = {Sathyaprakash, B. S. and Schutz, Bernard F.},
  journal      = {Living Reviews in Relativity},
  title        = {Physics, Astrophysics and Cosmology with Gravitational Waves},
  year         = {2009},
  issn         = {2367-3613},
  month        = dec,
  number       = {1},
  pages        = {2},
  volume       = {12},
  abstract     = {Gravitational wave detectors are already operating at interesting         sensitivity levels, and they have an upgrade path that should         result in secure detections by 2014. We review the physics of         gravitational waves, how they interact with detectors (bars and         interferometers), and how these detectors operate. We study the         most likely sources of gravitational waves and review the data         analysis methods that are used to extract their signals from         detector noise. Then we consider the consequences of         gravitational wave detections and observations for physics,         astrophysics, and cosmology.},
  doi          = {10.12942/lrr-2009-2},
  eid          = {2},
  eprint       = {0903.0338},
  file         = {:Sathyaprakash2009 - Physics, Astrophysics and Cosmology with Gravitational Waves.pdf:PDF},
  keywords     = {Gravitational waves, Gravitational wave sources, Gravitational wave detectors, Data analysis, General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics},
  primaryclass = {gr-qc},
  publisher    = {Springer Science and Business Media {LLC}},
  url          = {https://ui.adsabs.harvard.edu/abs/2009LRR....12....2S},
}

@Article{Maartens2008,
  author    = {Maartens, Roy},
  journal   = {General Relativity and Gravitation},
  title     = {Nonlinear gravito-electromagnetism},
  year      = {2008},
  month     = jun,
  number    = {6},
  pages     = {1203--1217},
  volume    = {40},
  abstract  = {There is a non-linear and covariant electromagnetic analogy for gravity,         in which the full Bianchi identities are Maxwell-type equations         for the free gravitational field, encoded in the Weyl tensor.         This tensor gravito-electromagnetism is based on a covariant         generalization of spatial vector algebra and calculus to spatial         tensor fields, and includes all non-linear effects from the         gravitational field and matter sources. The non-linear vacuum         Bianchi equations are invariant under spatial duality rotation         of the gravito-electric and gravito-magnetic tensor fields. The         super-energy density and super-Poynting vector of the         gravitational field are natural duality invariants, and satisfy         a super-energy conservation equation.},
  doi       = {10.1007/s10714-007-0600-6},
  file      = {:Maartens2008 - Nonlinear Gravito Electromagnetism.pdf:PDF},
  keywords  = {General relativity, Electromagnetism},
  publisher = {Springer Science and Business Media {LLC}},
  url       = {https://ui.adsabs.harvard.edu/abs/2008GReGr..40.1203M},
}

@Article{Poisson1995,
  author    = {Poisson, Eric and Will, Clifford M.},
  journal   = {Physical Review D},
  title     = {Gravitational waves from inspiraling compact binaries: Parameter estimation using second-post-Newtonian waveforms},
  year      = {1995},
  month     = jul,
  pages     = {848--855},
  volume    = {52},
  doi       = {10.1103/PhysRevD.52.848},
  file      = {:Poisson1995 - Gravitational Waves from Inspiraling Compact Binaries_ Parameter Estimation Using Second Post Newtonian Waveforms.pdf:PDF},
  issue     = {2},
  numpages  = {0},
  publisher = {American Physical Society},
}

@Article{Blanchet1995,
  author    = {Blanchet, Luc and Damour, Thibault and Iyer, Bala R. and Will, Clifford M. and Wiseman, Alan G.},
  journal   = {Physical Review Letters},
  title     = {Gravitational-Radiation Damping of Compact Binary Systems to Second Post-Newtonian Order},
  year      = {1995},
  month     = may,
  number    = {18},
  pages     = {3515--3518},
  volume    = {74},
  doi       = {10.1103/PhysRevLett.74.3515},
  issue     = {18},
  numpages  = {0},
  publisher = {American Physical Society},
}

@Article{Arun2005,
  author    = {Arun, K. G. and Iyer, Bala R. and Sathyaprakash, B. S. and Sundararajan, Pranesh A.},
  journal   = {Physical Review D},
  title     = {Parameter estimation of inspiralling compact binaries using 3.5 post-Newtonian gravitational wave phasing: The nonspinning case},
  year      = {2005},
  month     = apr,
  number    = {8},
  pages     = {084008},
  volume    = {71},
  doi       = {10.1103/PhysRevD.71.084008},
  file      = {:Arun2005 - Parameter Estimation of Inspiralling Compact Binaries Using 3.5 Post Newtonian Gravitational Wave Phasing_ the Nonspinning Case.pdf:PDF},
  issue     = {8},
  numpages  = {16},
  publisher = {American Physical Society},
}

@Article{Abbott2017,
  author        = {Abbott, B. P. and Abbott, R. and Abbott, T. D. and Acernese, F. and Ackley, K. and Adams, C. and Adams, T. and Addesso, P. and Adhikari, R. X. and Adya, V. B. and Affeldt, C. and Afrough, M. and Agarwal, B. and Agathos, M. and Agatsuma, K. and Aggarwal, N. and Aguiar, O. D. and Aiello, L. and Ain, A. and Ajith, P. and Allen, B. and Allen, G. and Allocca, A. and Aloy, M. A. and Altin, P. A. and Amato, A. and Ananyeva, A. and Anderson, S. B. and Anderson, W. G. and Angelova, S. V. and Antier, S. and Appert, S. and Arai, K. and Araya, M. C. and Areeda, J. S. and Arnaud, N. and Arun, K. G. and Ascenzi, S. and Ashton, G. and Ast, M. and Aston, S. M. and Astone, P. and Atallah, D. V. and Aufmuth, P. and Aulbert, C. and AultONeal, K. and Austin, C. and Avila-Alvarez, A. and Babak, S. and Bacon, P. and Bader, M. K. M. and Bae, S. and Baker, P. T. and Baldaccini, F. and Ballardin, G. and Ballmer, S. W. and Banagiri, S. and Barayoga, J. C. and Barclay, S. E. and Barish, B. C. and Barker, D. and Barkett, K. and Barone, F. and Barr, B. and Barsotti, L. and Barsuglia, M. and Barta, D. and Bartlett, J. and Bartos, I. and Bassiri, R. and Basti, A. and Batch, J. C. and Bawaj, M. and Bayley, J. C. and Bazzan, M. and B{\'e}csy, B. and Beer, C. and Bejger, M. and Belahcene, I. and Bell, A. S. and Berger, B. K. and Bergmann, G. and Bero, J. J. and Berry, C. P. L. and Bersanetti, D. and Bertolini, A. and Betzwieser, J. and Bhagwat, S. and Bhandare, R. and Bilenko, I. A. and Billingsley, G. and Billman, C. R. and Birch, J. and Birney, R. and Birnholtz, O. and Biscans, S. and Biscoveanu, S. and Bisht, A. and Bitossi, M. and Biwer, C. and Bizouard, M. A. and Blackburn, J. K. and Blackman, J. and Blair, C. D. and Blair, D. G. and Blair, R. M. and Bloemen, S. and Bock, O. and Bode, N. and Boer, M. and Bogaert, G. and Bohe, A. and Bondu, F. and Bonilla, E. and Bonnand, R. and Boom, B. A. and Bork, R. and Boschi, V. and Bose, S. and Bossie, K. and Bouffanais, Y. and Bozzi, A. and Bradaschia, C. and Brady, P. R. and Branchesi, M. and Brau, J. E. and Briant, T. and Brillet, A. and Brinkmann, M. and Brisson, V. and Brockill, P. and Broida, J. E. and Brooks, A. F. and Brown, D. A. and Brown, D. D. and Brunett, S. and Buchanan, C. C. and Buikema, A. and Bulik, T. and Bulten, H. J. and Buonanno, A. and Buskulic, D. and Buy, C. and Byer, R. L. and Cabero, M. and Cadonati, L. and Cagnoli, G. and Cahillane, C. and Calder{\'o}n Bustillo, J. and Callister, T. A. and Calloni, E. and Camp, J. B. and Canepa, M. and Canizares, P. and Cannon, K. C. and Cao, H. and Cao, J. and Capano, C. D. and Capocasa, E. and Carbognani, F. and Caride, S. and Carney, M. F. and Casanueva Diaz, J. and Casentini, C. and Caudill, S. and Cavagli{\`a}, M. and Cavalier, F. and Cavalieri, R. and Cella, G. and Cepeda, C. B. and Cerd{\'a}-Dur{\'a}n, P. and Cerretani, G. and Cesarini, E. and Chamberlin, S. J. and Chan, M. and Chao, S. and Charlton, P. and Chase, E. and Chassande-Mottin, E. and Chatterjee, D. and Chatziioannou, K. and Cheeseboro, B. D. and Chen, H. Y. and Chen, X. and Chen, Y. and Cheng, H. P. and Chia, H. and Chincarini, A. and Chiummo, A. and Chmiel, T. and Cho, H. S. and Cho, M. and Chow, J. H. and Christensen, N. and Chu, Q. and Chua, A. J. K. and Chua, S. and Chung, A. K. W. and Chung, S. and Ciani, G. and Ciolfi, R. and Cirelli, C. E. and Cirone, A. and Clara, F. and Clark, J. A. and Clearwater, P. and Cleva, F. and Cocchieri, C. and Coccia, E. and Cohadon, P. F. and Cohen, D. and Colla, A. and Collette, C. G. and Cominsky, L. R. and Constancio, M., Jr. and Conti, L. and Cooper, S. J. and Corban, P. and Corbitt, T. R. and Cordero-Carri{\'o}n, I. and Corley, K. R. and Cornish, N. and Corsi, A. and Cortese, S. and Costa, C. A. and Coughlin, M. W. and Coughlin, S. B. and Coulon, J. P. and Countryman, S. T. and Couvares, P. and Covas, P. B. and Cowan, E. E. and Coward, D. M. and Cowart, M. J. and Coyne, D. C. and Coyne, R. and Creighton, J. D. E. and Creighton, T. D. and Cripe, J. and Crowder, S. G. and Cullen, T. J. and Cumming, A. and Cunningham, L. and Cuoco, E. and Dal Canton, T. and D{\'a}lya, G. and Danilishin, S. L. and D'Antonio, S. and Danzmann, K. and Dasgupta, A. and Da Silva Costa, C. F. and Dattilo, V. and Dave, I. and Davier, M. and Davis, D. and Daw, E. J. and Day, B. and De, S. and DeBra, D. and Degallaix, J. and De Laurentis, M. and Del{\'e}glise, S. and Del Pozzo, W. and Demos, N. and Denker, T. and Dent, T. and De Pietri, R. and Dergachev, V. and De Rosa, R. and DeRosa, R. T. and De Rossi, C. and DeSalvo, R. and de Varona, O. and Devenson, J. and Dhurandhar, S. and D{\'\i}az, M. C. and Di Fiore, L. and Di Giovanni, M. and Di Girolamo, T. and Di Lieto, A. and Di Pace, S. and Di Palma, I. and Di Renzo, F. and Doctor, Z. and Dolique, V. and Donovan, F. and Dooley, K. L. and Doravari, S. and Dorrington, I. and Douglas, R. and Dovale {\'A}lvarez, M. and Downes, T. P. and Drago, M. and Dreissigacker, C. and Driggers, J. C. and Du, Z. and Ducrot, M. and Dupej, P. and Dwyer, S. E. and Edo, T. B. and Edwards, M. C. and Effler, A. and Eggenstein, H. B. and Ehrens, P. and Eichholz, J. and Eikenberry, S. S. and Eisenstein, R. A. and Essick, R. C. and Estevez, D. and Etienne, Z. B. and Etzel, T. and Evans, M. and Evans, T. M. and Factourovich, M. and Fafone, V. and Fair, H. and Fairhurst, S. and Fan, X. and Farinon, S. and Farr, B. and Farr, W. M. and Fauchon-Jones, E. J. and Favata, M. and Fays, M. and Fee, C. and Fehrmann, H. and Feicht, J. and Fejer, M. M. and Fernandez-Galiana, A. and Ferrante, I. and Ferreira, E. C. and Ferrini, F. and Fidecaro, F. and Finstad, D. and Fiori, I. and Fiorucci, D. and Fishbach, M. and Fisher, R. P. and Fitz-Axen, M. and Flaminio, R. and Fletcher, M. and Fong, H. and Font, J. A. and Forsyth, P. W. F. and Forsyth, S. S. and Fournier, J. D. and Frasca, S. and Frasconi, F. and Frei, Z. and Freise, A. and Frey, R. and Frey, V. and Fries, E. M. and Fritschel, P. and Frolov, V. V. and Fulda, P. and Fyffe, M. and Gabbard, H. and Gadre, B. U. and Gaebel, S. M. and Gair, J. R. and Gammaitoni, L. and Ganija, M. R. and Gaonkar, S. G. and Garcia-Quiros, C. and Garufi, F. and Gateley, B. and Gaudio, S. and Gaur, G. and Gayathri, V. and Gehrels, N. and Gemme, G. and Genin, E. and Gennai, A. and George, D. and George, J. and Gergely, L. and Germain, V. and Ghonge, S. and Ghosh, Abhirup and Ghosh, Archisman and Ghosh, S. and Giaime, J. A. and Giardina, K. D. and Giazotto, A. and Gill, K. and Glover, L. and Goetz, E. and Goetz, R. and Gomes, S. and Goncharov, B. and Gonz{\'a}lez, G. and Gonzalez Castro, J. M. and Gopakumar, A. and Gorodetsky, M. L. and Gossan, S. E. and Gosselin, M. and Gouaty, R. and Grado, A. and Graef, C. and Granata, M. and Grant, A. and Gras, S. and Gray, C. and Greco, G. and Green, A. C. and Gretarsson, E. M. and Groot, P. and Grote, H. and Grunewald, S. and Gruning, P. and Guidi, G. M. and Guo, X. and Gupta, A. and Gupta, M. K. and Gushwa, K. E. and Gustafson, E. K. and Gustafson, R. and Halim, O. and Hall, B. R. and Hall, E. D. and Hamilton, E. Z. and Hammond, G. and Haney, M. and Hanke, M. M. and Hanks, J. and Hanna, C. and Hannam, M. D. and Hannuksela, O. A. and Hanson, J. and Hardwick, T. and Harms, J. and Harry, G. M. and Harry, I. W. and Hart, M. J. and Haster, C. J. and Haughian, K. and Healy, J. and Heidmann, A. and Heintze, M. C. and Heitmann, H. and Hello, P. and Hemming, G. and Hendry, M. and Heng, I. S. and Hennig, J. and Heptonstall, A. W. and Heurs, M. and Hild, S. and Hinderer, T. and Hoak, D. and Hofman, D. and Holt, K. and Holz, D. E. and Hopkins, P. and Horst, C. and Hough, J. and Houston, E. A. and Howell, E. J. and Hreibi, A. and Hu, Y. M. and Huerta, E. A. and Huet, D. and Hughey, B. and Husa, S. and Huttner, S. 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P. and Zevin, M. and Zhang, L. and Zhang, M. and Zhang, T. and Zhang, Y. H. and Zhao, C. and Zhou, M. and Zhou, Z. and Zhu, S. J. and Zhu, X. J. and Zimmerman, A. B. and Zucker, M. E. and Zweizig, J. and Collaboration, (L. I. G. O. Scientific and Collaboration, Virgo and Burns, E. and Veres, P. and Kocevski, D. and Racusin, J. and Goldstein, A. and Connaughton, V. and Briggs, M. S. and Blackburn, L. and Hamburg, R. and Hui, C. M. and von Kienlin, A. and McEnery, J. and Preece, R. D. and Wilson-Hodge, C. A. and Bissaldi, E. and Cleveland, W. H. and Gibby, M. H. and Giles, M. M. and Kippen, R. M. and McBreen, S. and Meegan, C. A. and Paciesas, W. S. and Poolakkil, S. and Roberts, O. J. and Stanbro, M. and Gamma-ray Burst Monitor, (Fermi and Savchenko, V. and Ferrigno, C. and Kuulkers, E. and Bazzano, A. and Bozzo, E. and Brandt, S. and Chenevez, J. and Courvoisier, T. J. L. and Diehl, R. and Domingo, A. and Hanlon, L. and Jourdain, E. and Laurent, P. and Lebrun, F. and Lutovinov, A. and Mereghetti, S. and Natalucci, L. and Rodi, J. and Roques, J. P. and Sunyaev, R. and Ubertini, P. and (INTEGRAL},
  journal       = {The Astrophysical Journal},
  title         = {Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: {GW}170817 and {GRB} 170817A},
  year          = {2017},
  month         = oct,
  number        = {2},
  pages         = {L13},
  volume        = {848},
  abstract      = {On 2017 August 17, the gravitational-wave event GW170817 was observed by         the Advanced LIGO and Virgo detectors, and the gamma-ray burst         (GRB) GRB 170817A was observed independently by the Fermi Gamma-         ray Burst Monitor, and the Anti-Coincidence Shield for the         Spectrometer for the International Gamma-Ray Astrophysics         Laboratory. The probability of the near-simultaneous temporal         and spatial observation of GRB 170817A and GW170817 occurring by         chance is 5.0{\texttimes} \{10\}$^{-8}$. We therefore confirm         binary neutron star mergers as a progenitor of short GRBs. The         association of GW170817 and GRB 170817A provides new insight         into fundamental physics and the origin of short GRBs. We use         the observed time delay of (+1.74+/- 0.05) \{\{s\}\} between GRB         170817A and GW170817 to: (I) constrain the difference between         the speed of gravity and the speed of light to be between         -3{\texttimes} \{10\}$^{-15}$ and +7{\texttimes} \{10\}$^{-16}$         times the speed of light, (II) place new bounds on the violation         of Lorentz invariance, (III) present a new test of the         equivalence principle by constraining the Shapiro delay between         gravitational and electromagnetic radiation. We also use the         time delay to constrain the size and bulk Lorentz factor of the         region emitting the gamma-rays. GRB 170817A is the closest short         GRB with a known distance, but is between 2 and 6 orders of         magnitude less energetic than other bursts with measured         redshift. A new generation of gamma-ray detectors, and         subthreshold searches in existing detectors, will be essential         to detect similar short bursts at greater distances. Finally, we         predict a joint detection rate for the Fermi Gamma-ray Burst         Monitor and the Advanced LIGO and Virgo detectors of 0.1-1.4 per         year during the 2018-2019 observing run and 0.3-1.7 per year at         design sensitivity.},
  archiveprefix = {arXiv},
  doi           = {10.3847/2041-8213/aa920c},
  eid           = {L13},
  eprint        = {1710.05834},
  file          = {:Abbott2017 - Gravitational Waves and Gamma Rays from a Binary Neutron Star Merger_ GW170817 and GRB 170817A.pdf:PDF},
  keywords      = {binaries: close, gamma-ray burst: general, gravitational waves, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology},
  primaryclass  = {astro-ph.HE},
  publisher     = {American Astronomical Society},
  url           = {https://ui.adsabs.harvard.edu/abs/2017ApJ...848L..13A},
}

@Article{Roy2020,
  author    = {Roy, Soumendra Kishore and Koley, Ratna and Majumdar, Parthasarathi},
  journal   = {Physical Review D},
  title     = {Probing the post-Minkowskian approximation using recursive addition of self-interactions},
  year      = {2020},
  month     = oct,
  pages     = {084045},
  volume    = {102},
  doi       = {10.1103/PhysRevD.102.084045},
  file      = {:Roy2020 - Probing the Post Minkowskian Approximation Using Recursive Addition of Self Interactions.pdf:PDF},
  issue     = {8},
  numpages  = {8},
  publisher = {American Physical Society},
}

@Misc{Blanchet1996,
  author        = {Blanchet, Luc},
  title         = {Gravitational radiation from relativistic sources},
  year          = {1996},
  archiveprefix = {arXiv},
  doi           = {10.48550/arxiv.gr-qc/9607025},
  eprint        = {gr-qc/9607025},
  primaryclass  = {gr-qc},
}

@Book{Maggiore2014,
  author    = {Maggiore, Michele},
  publisher = {Oxford University Press},
  title     = {Gravitational Waves: Volume 1: Theory and Experiments},
  year      = {2014},
  address   = {Oxford},
  edition   = {Repr with corr.},
  isbn      = {978-0-19-857074-5},
  number    = {Theory and experiments},
  volume    = {1},
  pagetotal = {554},
  ppn_gvk   = {1489991220},
  subtitle  = {Michele},
}

@Book{Jaranowski2009,
  author    = {Jaranowski, Piotr},
  editor    = {Andrzej Kr{\'{o}}lak},
  publisher = {Cambridge University Press},
  title     = {Analysis of gravitational-wave data},
  year      = {2009},
  address   = {Cambridge},
  isbn      = {978-0-511-60518-5},
  note      = {Includes bibliographical references (pages 235-248) and index},
  number    = {29},
  series    = {Cambridge monographs on particle physics, nuclear physics and cosmology},
  pagetotal = {1257},
  ppn_gvk   = {1735127396},
}

@Article{Finn1992,
  author    = {Finn, Lee S.},
  journal   = {Physical Review D},
  title     = {Detection, measurement, and gravitational radiation},
  year      = {1992},
  month     = dec,
  number    = {12},
  pages     = {5236--5249},
  volume    = {46},
  abstract  = {The optimum design, construction, and use of the Laser Interferometer Gravitational Wave Observatory (LIGO), the French-Italian Gravitational Wave Observatory (VIRGO), or the Laser Gravitational Wave Observatory (LAGOS) gravitational radiation detectors depends upon accurate calculations of their sensitivity to de'erent sources of radiation. Here I examine how to determine the sensitivity of these instruments to sources of gravitational radiation by considering the process by which data are analyzed in a noisy detector. The problem of detection (is a signal present in the output of the detector?) is separated from that of measurement (what are the parameters that characterize the signal in the detector output?). By constructing the probability that the detector output is consistent with the presence of a signal, I show how to quantify the uncertainty that the output contains a signal and is not simply noise. Proceeding further, I construct the probability distribution that the parametrization p that characterizes the signal has a certain value. From the distribution and its mode I determine volumes V(P) in parameter space such that ts 6 V(P) with probability P [owing to the random nature of the detector noise, the volumes V(P) are always different, even for identical signals in the detector output], thus quantifying the uncertainty in the estimation of the signal parametrization. These techniques are suitable for analyzing the output of a noisy detector. If we are designing a detector, or determining the suitability of an existing detector for observing a new source, then we do not have detector output to analyze but are interested in the "most likely" response of the detector to a signal. I exploit the techniques just described to determine the "most likely" volumes V(P) for detector output that would result in a parameter probability distribution with given mode. Finally, as an example, I apply these techniques to determine the anticipated sensitivity of the LIGO and LAGOS detectors to the gravitational radiation from a perturbed Kerr black hole.},
  date      = {1992},
  doi       = {10.1103/PhysRevD.46.5236},
  file      = {:Finn1992 - Detection, Measurement, and Gravitational Radiation.pdf:PDF},
  issue     = {12},
  keywords  = {number(s): 04.80.+z, 04.30.+x, 06.20.Dk, 97.60.Lf},
  numpages  = {0},
  publisher = {American Physical Society},
}

@Article{Ni1978,
  author    = {Ni, Wei-Tou and Zimmermann, Mark},
  journal   = {Physical Review D},
  title     = {Inertial and gravitational effects in the proper reference frame of an accelerated, rotating observer},
  year      = {1978},
  month     = mar,
  pages     = {1473--1476},
  volume    = {17},
  doi       = {10.1103/PhysRevD.17.1473},
  issue     = {6},
  numpages  = {0},
  publisher = {American Physical Society},
}

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W. and Bals, A. and Balsamo, A. and Baltus, G. and Banagiri, S. and Bankar, D. and Bankar, R. S. and Barayoga, J. C. and Barbieri, C. and Barish, B. C. and Barker, D. and Barneo, P. and Barnum, S. and Barone, F. and Barr, B. and Barsotti, L. and Barsuglia, M. and Barta, D. and Bartlett, J. and Bartos, I. and Bassiri, R. and Basti, A. and Bawaj, M. and Bayley, J. C. and Bazzan, M. and Becher, B. R. and B\'ecsy, B. and Bedakihale, V. M. and Bejger, M. and Belahcene, I. and Beniwal, D. and Benjamin, M. G. and Benkel, R. and Bennett, T. F. and Bentley, J. D. and Bergamin, F. and Berger, B. K. and Bergmann, G. and Bernuzzi, S. and Berry, C. P. L. and Bersanetti, D. and Bertolini, A. and Betzwieser, J. and Bhandare, R. and Bhandari, A. V. and Bhattacharjee, D. and Bidler, J. and Bilenko, I. A. and Billingsley, G. and Birney, R. and Birnholtz, O. and Biscans, S. and Bischi, M. and Biscoveanu, S. and Bisht, A. and Bitossi, M. and Bizouard, M.-A. and Blackburn, J. 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  journal       = {Physical Review D},
  title         = {Tests of general relativity with binary black holes from the second LIGO-Virgo gravitational-wave transient catalog},
  year          = {2021},
  issn          = {2470-0029},
  month         = jun,
  number        = {12},
  pages         = {122002},
  volume        = {103},
  abstract      = {Gravitational waves enable tests of general relativity in the highly dynamical and strong-field regime. Using events detected by LIGO-Virgo up to 1 October 2019, we evaluate the consistency of the data with predictions from the theory. We first establish that residuals from the best-fit waveform are consistent with detector noise, and that the low-and high-frequency parts of the signals are in agreement. We then consider parametrized modifications to the waveform by varying post-Newtonian and phenomenological coefficients, improving past constraints by factors of $\sim$2; we also find consistency with Kerr black holes when we specifically target signatures of the spin-induced quadrupole moment. Looking for gravitational-wave dispersion, we tighten constraints on Lorentz-violating coefficients by a factor of $\sim$2.6 and bound the mass of the graviton to m g $\leq$ 1.76 $\times$ 10-23 eV=c 2 with 90% credibility. We also analyze the properties of the merger remnants by measuring ringdown frequencies and damping times, constraining fractional deviations away from the Kerr frequency to $\delta$ f220 $\sfrac{1}{4}$ 0.03 {\th}0.38-0.35 for the fundamental quadrupolar mode, and $\delta$ f221 $\sfrac{1}{4}$ 0.04 {\th}0.27-0.32 for the first overtone; additionally, we find no evidence for postmerger echoes. Finally, we determine that our data are consistent with tensorial polarizations through a template-independent method. When possible, we assess the validity of general relativity based on collections of events analyzed jointly. We find no evidence for new physics beyond general relativity, for black hole mimickers, or for any unaccounted systematics.},
  collaboration = {LIGO Scientific Collaboration and Virgo Collaboration},
  date          = {2021-06-15},
  day           = {15},
  doi           = {10.1103/PhysRevD.103.122002},
  file          = {:Abbott2021 - Tests of General Relativity with Binary Black Holes from the Second LIGO Virgo Gravitational Wave Transient Catalog.pdf:PDF},
  issue         = {12},
  keywords      = {doi:10.1103/PhysRevD.103.122002 url:https://doi.org/10.1103/PhysRevD.103.122002},
  numpages      = {43},
  publisher     = {American Physical Society},
}

@Misc{Abbott2021a,
  author        = {Abbott, R. and Abe, H. and Acernese, F. and Ackley, K. and Adhikari, N. and Adhikari, R. X. and Adkins, V. K. and Adya, V. B. and Affeldt, C. and Agarwal, D. and Agathos, M. and Agatsuma, K. and Aggarwal, N. and Aguiar, O. D. and Aiello, L. and Ain, A. and Ajith, P. and Akutsu, T. and de Alarc{\'{o}}n, P. F. and Albanesi, S. and Alfaidi, R. A. and Allocca, A. and Altin, P. A. and Amato, A. and Anand, C. and Anand, S. and Ananyeva, A. and Anderson, S. B. and Anderson, W. G. and Ando, M. and Andrade, T. and Andres, N. and Andr{\'{e}}s-Carcasona, M. and Andri{\'{c}}, T. and Angelova, S. V. and Ansoldi, S. and Antelis, J. M. and Antier, S. and Apostolatos, T. and Appavuravther, E. Z. and Appert, S. and Apple, S. K. and Arai, K. and Araya, A. and Araya, M. C. and Areeda, J. S. and Ar{\`{e}}ne, M. and Aritomi, N. and Arnaud, N. and Arogeti, M. and Aronson, S. M. and Arun, K. G. and Asada, H. and Asali, Y. and Ashton, G. and Aso, Y. and Assiduo, M. and de Souza Melo, S. Assis and Aston, S. M. and Astone, P. and Aubin, F. and AultONeal, K. and Austin, C. and Babak, S. and Badaracco, F. and Bader, M. K. M. and Badger, C. and Bae, S. and Bae, Y. and Baer, A. M. and Bagnasco, S. and Bai, Y. and Baird, J. and Bajpai, R. and Baka, T. and Ball, M. and Ballardin, G. and Ballmer, S. W. and Balsamo, A. and Baltus, G. and Banagiri, S. and Banerjee, B. and Bankar, D. and Barayoga, J. C. and Barbieri, C. and Barish, B. C. and Barker, D. and Barneo, P. and Barone, F. and Barr, B. and Barsotti, L. and Barsuglia, M. and Barta, D. and Bartlett, J. and Barton, M. A. and Bartos, I. and Basak, S. and Bassiri, R. and Basti, A. and Bawaj, M. and Bayley, J. C. and Bazzan, M. and Becher, B. R. and B{\'{e}}csy, B. and Bedakihale, V. M. and Beirnaert, F. and Bejger, M. and Belahcene, I. and Benedetto, V. and Beniwal, D. and Benjamin, M. G. and Bennett, T. F. and Bentley, J. D. and BenYaala, M. and Bera, S. and Berbel, M. and Bergamin, F. and Berger, B. K. and Bernuzzi, S. and Berry, C. P. L. and Bersanetti, D. and Bertolini, A. and Betzwieser, J. and Beveridge, D. and Bhandare, R. and Bhandari, A. V. and Bhardwaj, U. and Bhatt, R. and Bhattacharjee, D. and Bhaumik, S. and Bianchi, A. and Bilenko, I. A. and Billingsley, G. and Bini, S. and Birney, R. and Birnholtz, O. and Biscans, S. and Bischi, M. and Biscoveanu, S. and Bisht, A. and Biswas, B. and Bitossi, M. and Bizouard, M. A. and Blackburn, J. K. and Blair, C. D. and Blair, D. G. and Blair, R. M. and Bobba, F. and Bode, N. and Bo{\"{e}}r, M. and Bogaert, G. and Boldrini, M. and Bolingbroke, G. N. and Bonavena, L. D. and Bondu, F. and Bonilla, E. and Bonnand, R. and Booker, P. and Boom, B. A. and Bork, R. and Boschi, V. and Bose, N. and Bose, S. and Bossilkov, V. and Boudart, V. and Bouffanais, Y. and Bozzi, A. and Bradaschia, C. and Brady, P. R. and Bramley, A. and Branch, A. and Branchesi, M. and Brau, J. E. and Breschi, M. and Briant, T. and Briggs, J. 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  title         = {Tests of General Relativity with GWTC-3},
  year          = {2021},
  archiveprefix = {arXiv},
  doi           = {10.48550/arxiv.2112.06861},
  eprint        = {2112.06861},
  file          = {:Abbott2021a - Tests of General Relativity with GWTC 3.pdf:PDF},
  primaryclass  = {gr-qc},
}

@Article{Thrane2019,
  author  = {Thrane, Eric and Talbot, Colm},
  journal = {Publications of the Astronomical Society of Australia},
  title   = {An introduction to Bayesian inference in gravitational-wave astronomy: Parameter estimation, model selection, and hierarchical models},
  year    = {2019},
  pages   = {e010},
  volume  = {36},
  doi     = {10.1017/pasa.2019.2},
  file    = {:Thrane2019 - An Introduction to Bayesian Inference in Gravitational Wave Astronomy_ Parameter Estimation, Model Selection, and Hierarchical Models.pdf:PDF},
}

@Book{Piotr2009,
  author    = {Piotr, Jaranowski and Andrzej, Krolak},
  publisher = {Cambridge University Press},
  title     = {Analysis of Gravitational-Wave Data.},
  year      = {2009},
  isbn      = {9780521864596},
  number    = {Vol. 29},
  series    = {Cambridge Monographs on Particle Physics, Nuclear Physics and Cosmology},
  abstract  = {Research in this field has grown considerably in recent years due to the commissioning of a world-wide network of large-scale detectors. This network collects a very large amount of data that is currently being analyzed and interpreted. This book introduces researchers entering the field, and researchers currently analyzing the data, to the field of gravitational-wave data analysis. An ideal starting point for studying the issues related to current gravitational-wave research, the book contains detailed derivations of the basic formulae related to the detectors'responses and maximum-likelihood detection. These derivations are much more complete and more pedagogical than those found in current research papers, and will enable readers to apply general statistical concepts to the analysis of gravitational-wave signals. It also discusses new ideas on devising the efficient algorithms needed to perform data analysis.},
  url       = {https://search.ebscohost.com/login.aspx?direct=true&db=e000xww&AN=289534&lang=zh-cn&site=ehost-live},
}

@Article{Isaacson1968,
  author    = {Isaacson, Richard A.},
  journal   = {Physical Review},
  title     = {Gravitational Radiation in the Limit of High Frequency. I. The Linear Approximation and Geometrical Optics},
  year      = {1968},
  month     = feb,
  pages     = {1263--1271},
  volume    = {166},
  doi       = {10.1103/PhysRev.166.1263},
  issue     = {5},
  numpages  = {0},
  publisher = {American Physical Society},
}

@Article{Isaacson1968a,
  author    = {Isaacson, Richard A.},
  journal   = {Physical Review},
  title     = {Gravitational Radiation in the Limit of High Frequency. II. Nonlinear Terms and the Effective Stress Tensor},
  year      = {1968},
  month     = feb,
  pages     = {1272--1280},
  volume    = {166},
  doi       = {10.1103/PhysRev.166.1272},
  issue     = {5},
  numpages  = {0},
  publisher = {American Physical Society},
}

@Book{Ellis2012,
  author    = {Ellis, George F. R. and Maartens, Roy and MacCallum, Malcolm A. H.},
  publisher = {Cambridge University Press},
  title     = {Relativistic Cosmology},
  year      = {2012},
  isbn      = {9780521381154},
  abstract  = {Cosmology has been transformed by dramatic progress in high-precision observations and theoretical modelling. This book surveys key developments and open issues for graduate students and researchers. Using a relativistic geometric approach, it focuses on the general concepts and relations that underpin the standard model of the Universe. Part I covers foundations of relativistic cosmology whilst Part II develops the dynamical and observational relations for all models of the Universe based on general relativity. Part III focuses on the standard model of cosmology, including inflation, dark matter, dark energy, perturbation theory, the cosmic microwave background, structure formation and gravitational lensing. It also examines modified gravity and inhomogeneity as possible alternatives to dark energy. Anisotropic and inhomogeneous models are described in Part IV, and Part V reviews deeper issues, such as quantum cosmology, the start of the universe and the multiverse proposal. Colour v},
  url       = {https://search.ebscohost.com/login.aspx?direct=true&db=nlebk&AN=416690&lang=zh-cn&site=ehost-live},
}

@Article{Abbott2020,
  author    = {Abbott, B. P. and Abbott, R. and Abbott, T. D. and Abraham, S. and Acernese, F. and Ackley, K. and Adams, C. and Adya, V. B. and Affeldt, C. and Agathos, M. and Agatsuma, K. and Aggarwal, N. and Aguiar, O. D. and Aiello, L. and Ain, A. and Ajith, P. and Alford, T. and Allen, G. and Allocca, A. and Aloy, M. A. and Altin, P. A. and Amato, A. and Ananyeva, A. and Anderson, S. B. and Anderson, W. G. and Angelova, S. V. and Antier, S. and Appert, S. and Arai, K. and Araya, M. C. and Areeda, J. S. and Ar{\`{e}}ne, M. and Arnaud, N. and Arun, K. G. and Ascenzi, S. and Ashton, G. and Aston, S. M. and Astone, P. and Aubin, F. and Aufmuth, P. and AultONeal, K. and Austin, C. and Avendano, V. and Avila-Alvarez, A. and Babak, S. and Bacon, P. and Badaracco, F. and Bader, M. K. M. and Bae, S. and Baker, P. T. and Baldaccini, F. and Ballardin, G. and Ballmer, S. W. and Banagiri, S. and Barayoga, J. C. and Barclay, S. E. and Barish, B. C. and Barker, D. and Barkett, K. and Barnum, S. and Barone, F. and Barr, B. and Barsotti, L. and Barsuglia, M. and Barta, D. and Bartlett, J. and Bartos, I. and Bassiri, R. and Basti, A. and Bawaj, M. and Bayley, J. C. and Bazzan, M. and B{\'{e}}csy, B. and Bejger, M. and Belahcene, I. and Bell, A. S. and Beniwal, D. and Berger, B. K. and Bergmann, G. and Bernuzzi, S. and Bero, J. J. and Berry, C. P. L. and Bersanetti, D. and Bertolini, A. and Betzwieser, J. and Bhandare, R. and Bidler, J. and Bilenko, I. A. and Bilgili, S. A. and Billingsley, G. and Birch, J. and Birney, R. and Birnholtz, O. and Biscans, S. and Biscoveanu, S. and Bisht, A. and Bitossi, M. and Bizouard, M. A. and Blackburn, J. K. and Blair, C. D. and Blair, D. G. and Blair, R. M. and Bloemen, S. and Bode, N. and Boer, M. and Boetzel, Y. and Bogaert, G. and Bondu, F. and Bonilla, E. and Bonnand, R. and Booker, P. and Boom, B. A. and Booth, C. 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  journal   = {Classical and Quantum Gravity},
  title     = {A guide to {LIGO}-{V}irgo detector noise and extraction of transient gravitational-wave signals},
  year      = {2020},
  issn      = {1361-6382},
  month     = feb,
  number    = {5},
  pages     = {055002},
  volume    = {37},
  abstract  = {The LIGO Scientific Collaboration and the Virgo Collaboration have cataloged eleven confidently detected gravitational-wave events during the first two observing runs of the advanced detector era. All eleven events were consistent with being from well-modeled mergers between compact stellar-mass objects: black holes or neutron stars. The data around the time of each of these events have been made publicly available through the gravitational-wave open science center. The entirety of the gravitational-wave strain data from the first and second observing runs have also now been made publicly available. There is considerable interest among the broad scientific community in understanding the data and methods used in the analyses. In this paper, we provide an overview of the detector noise properties and the data analysis techniques used to detect gravitational-wave signals and infer the source properties. We describe some of the checks that are performed to validate the analyses and results from the observations of gravitational-wave events. We also address concerns that have been raised about various properties of LIGO--Virgo detector noise and the correctness of our analyses as applied to the resulting data.},
  doi       = {10.1088/1361-6382/ab685e},
  file      = {:Abbott2020 - A Guide to LIGO Virgo Detector Noise and Extraction of Transient Gravitational Wave Signals.pdf:PDF},
  publisher = {{IOP} Publishing},
}

@Article{Jaranowski2012,
  author    = {Jaranowski, Piotr and Kr{\'{o}}lak, Andrzej},
  journal   = {Living Reviews in Relativity},
  title     = {Gravitational-Wave Data Analysis. Formalism and Sample Applications: The Gaussian Case},
  year      = {2012},
  month     = mar,
  number    = {1},
  pages     = {4},
  volume    = {15},
  date      = {2012-03-09},
  day       = {9},
  doi       = {10.12942/lrr-2012-4},
  file      = {:Jaranowski2012 - Gravitational Wave Data Analysis. Formalism and Sample Applications_ the Gaussian Case.pdf:PDF},
  publisher = {Springer Science and Business Media LLC},
}

@Article{Hughes2009,
  author    = {Hughes, Scott A.},
  journal   = {Annual Review of Astronomy and Astrophysics},
  title     = {Gravitational Waves from Merging Compact Binaries},
  year      = {2009},
  issn      = {1545-4282},
  month     = sep,
  number    = {1},
  pages     = {107--157},
  volume    = {47},
  doi       = {10.1146/annurev-astro-082708-101711},
  file      = {:Hughes2009 - Gravitational Waves from Merging Compact Binaries.pdf:PDF},
  publisher = {Annual Reviews},
}




@Article{Ni2010,
  author   = {Ni, Wei-Tou},
  journal  = {Modern Physics Letters A},
  title    = {GRAVITATIONAL WAVES, DARK ENERGY AND INFLATION},
  year     = {2010},
  number   = {11n12},
  pages    = {922--935},
  volume   = {25},
  abstract = {In this paper we first present a complete classification of gravitational waves according to their frequencies: (i) Ultra high frequency band (above 1 THz); (ii) Very high frequency band (100 kHz--1 THz); (iii) High frequency band (10 Hz--100 kHz); (iv) Middle frequency band (0.1 Hz--10 Hz); (v) Low frequency band (100 nHz--0.1 Hz); (vi) Very low frequency band (300 pHz--100 nHz); (vii) Ultra low frequency band (10 fHz--300 pHz); (viii) Hubble (extremely low) frequency band (1 aHz--10 fHz); (ix) Infra-Hubble frequency band (below 1 aHz). After briefly discussing the method of detection for different frequency bands, we review the concept and status of space gravitational-wave missions --- LISA, ASTROD, ASTROD-GW, Super-ASTROD, DECIGO and Big Bang Observer. We then address to the determination of dark energy equation, and probing the inflationary physics using space gravitational wave detectors.},
  doi      = {10.1142/S0217732310000071},
  file     = {:ni-2011-gravitational-waves-dark-energy-and-inflation.pdf:PDF},
}

@Article{Schutz1999,
  author   = {Schutz, B. F.},
  journal  = {Classical and Quantum Gravity},
  title    = {Gravitational wave astronomy},
  year     = {1999},
  month    = dec,
  number   = {12A},
  pages    = {A131},
  volume   = {16},
  abstract = {The first decade of the new millennium should see the first direct detections of gravitational waves. This will be a milestone or fundamental physics and it will open the new observational science of gravitational wave astronomy. But gravitational waves already play an important role in the modeling of astrophysical systems. I review here the present state of gravitational radiation theory in relativity and astrophysics, and I then look at the development of detector sensitivity over the next decade, both on the ground (such as LIGO) and in space (LISA). I review the sources of gravitational waves that are likely to play an imp rtant role in observations by first- and second-generation interferometers, including the astrophysical information that will c me from these observations. The review covers some 10 decades of gravitational wave frequency, from the high-frequency normal odes of neutron stars down to the lowest frequencies observable from space. The discussion of sources includes recent developments regarding binary black holes, spinning neutron stars, and the stochastic background.},
  doi      = {10.1088/0264-9381/16/12A/307},
  file     = {:B_F_Schutz_1999_Class._Quantum_Grav._16_A131.pdf:PDF},
}

@Article{Riles2013,
  author   = {Riles, K.},
  journal  = {Progress in Particle and Nuclear Physics},
  title    = {Gravitational waves: Sources, detectors and searches},
  year     = {2013},
  issn     = {0146-6410},
  pages    = {1--54},
  volume   = {68},
  abstract = {Gravitational wave science should transform in this decade from a study of what has not been seen to a full-fledged field of astronomy in which detected signals reveal the nature of cataclysmic events and exotic objects. The LIGO Scientific Collaboration and Virgo Collaboration have recently completed joint data runs of unprecedented sensitivities to gravitational waves. So far, no gravitational radiation has been seen (although data mining continues). It seems likely that the first detection will come from 2\textsuperscript{nd}-generation LIGO and Virgo interferometers now being installed. These new detectors are expected to detect $\sim$40 coalescences of neutron star binary systems per year at full sensitivity. At the same time, research and development continues on 3\textsuperscript{rd}-generation underground interferometers and on space-based interferometers. In parallel there is a vigorous effort in the radio pulsar community to detect $\sim$ several-nHz gravitational waves via the timing residuals from an array of pulsars at different locations in the sky. As the dawn of gravitational wave astronomy nears, this review, intended primarily for interested particle and nuclear physicists, describes what we have learned to date and the prospects for direct discovery of gravitational waves.},
  doi      = {10.1016/j.ppnp.2012.08.001},
  keywords = {Gravity, Astrophysics, Relativity, Interferometry, LIGO, Virgo},
  url      = {https://www.sciencedirect.com/science/article/pii/S0146641012001093},
}

@Misc{Cutler2002,
  author        = {Cutler, Curt and Thorne, Kip S.},
  title         = {An Overview of Gravitational-Wave Sources},
  year          = {2002},
  archiveprefix = {arXiv},
  doi           = {10.48550/arxiv.gr-qc/0204090},
  eprint        = {gr-qc/0204090},
  eprintclass   = {gr-qc},
  eprinttype    = {arxiv},
  primaryclass  = {gr-qc},
}

@Article{Blanchet2024,
  author    = {Blanchet, Luc},
  journal   = {Living Reviews in Relativity},
  title     = {Post-Newtonian theory for gravitational waves},
  year      = {2024},
  issn      = {1433-8351},
  month     = jul,
  number    = {1},
  volume    = {27},
  doi       = {10.1007/s41114-024-00050-z},
  publisher = {Springer Science and Business Media LLC},
}

@Article{Aggarwal2021,
  author    = {Aggarwal, Nancy and Aguiar, Odylio D. and Bauswein, Andreas and Cella, Giancarlo and Clesse, Sebastian and Cruise, Adrian Michael and Domcke, Valerie and Figueroa, Daniel G. and Geraci, Andrew and Goryachev, Maxim and Grote, Hartmut and Hindmarsh, Mark and Muia, Francesco and Mukund, Nikhil and Ottaway, David and Peloso, Marco and Quevedo, Fernando and Ricciardone, Angelo and Steinlechner, Jessica and Steinlechner, Sebastian and Sun, Sichun and Tobar, Michael E. and Torrenti, Francisco and {{\"{U}}}nal, Caner and White, Graham},
  journal   = {Living Reviews in Relativity},
  title     = {Challenges and opportunities of gravitational-wave searches at MHz to GHz frequencies},
  year      = {2021},
  issn      = {1433-8351},
  month     = dec,
  number    = {1},
  volume    = {24},
  doi       = {10.1007/s41114-021-00032-5},
  publisher = {Springer Science and Business Media LLC},
}

@Article{Fryer2011,
  author    = {Fryer, Chris L. and New, Kimberly C. B.},
  journal   = {Living Reviews in Relativity},
  title     = {Gravitational Waves from Gravitational Collapse},
  year      = {2011},
  issn      = {1433-8351},
  month     = jan,
  number    = {1},
  volume    = {14},
  abstract  = {Gravitational wave emission from stellar collapse has been studied for more than three decades. Current state-of-the-art numerical investigations of collapse include those that use How to cite this article Owing to the fact that a Living Reviews article can evolve over time, we recommend to cite the article as follows:},
  date      = {2003-03-10},
  day       = {10},
  doi       = {10.12942/lrr-2011-1},
  publisher = {Springer Science and Business Media LLC},
}

@Article{Romano2017,
  author    = {Romano, Joseph D. and Cornish, Neil. J.},
  journal   = {Living Reviews in Relativity},
  title     = {Detection methods for stochastic gravitational-wave backgrounds: a unified treatment},
  year      = {2017},
  issn      = {1433-8351},
  month     = apr,
  number    = {1},
  volume    = {20},
  abstract  = {Living Reviews in Relativity, doi:10.1007/s41114-017-0004-1},
  doi       = {10.1007/s41114-017-0004-1},
  file      = {:Romano2017 - Detection Methods for Stochastic Gravitational Wave Backgrounds_ a Unified Treatment.pdf:PDF},
  keywords  = {Gravitational waves,Data analysis,Stochastic backgrounds},
  publisher = {Springer Science and Business Media LLC},
}

@Article{Flanagan2005,
  author   = {Flanagan, {{\'{E}}}anna \'{E} and Hughes, Scott A.},
  journal  = {New Journal of Physics},
  title    = {The basics of gravitational wave theory},
  year     = {2005},
  month    = sep,
  number   = {1},
  pages    = {204},
  volume   = {7},
  abstract = {Einstein's special theory of relativity revolutionized physics by teaching us that space and time are not separate entities, but join as {\textquoteleft}spacetime{\textquoteright}. His general theory of relativity further taught us that spacetime is not just a stage on which dynamics takes place, but is a participant: the field equation of general relativity connects matter dynamics to the curvature of spacetime. Curvature is responsible for gravity, carrying us beyond the Newtonian conception of gravity that had been in place for the previous two and a half centuries. Much research in gravitation since then has explored and clarified the consequences of this revolution; the notion of dynamical spacetime is now firmly established in the toolkit of modern physics. Indeed, this notion is so well established that we may now contemplate using spacetime as a tool for other sciences. One aspect of dynamical spacetime---its radiative character, {\textquoteleft}gravitational radiation{\textquoteright}---will inaugurate entirely new techniques for observing violent astrophysical processes. Over the next 100 years, much of this subject's excitement will come from learning how to exploit spacetime as a tool for astronomy. This paper is intended as a tutorial in the basics of gravitational radiation physics.},
  doi      = {10.1088/1367-2630/7/1/204},
  file     = {:Flanagan2005 - The Basics of Gravitational Wave Theory.pdf:PDF},
}

@Article{Favata2010,
  author    = {Favata, Marc},
  journal   = {Classical and Quantum Gravity},
  title     = {The Gravitational-Wave Memory Effect},
  year      = {2010},
  month     = apr,
  number    = {8},
  pages     = {084036},
  volume    = {27},
  abstract  = {The nonlinear memory effect is a slowly growing, non-oscillatory contribution to the gravitational-wave amplitude. It originates from gravitational waves that are sourced by the previously emitted waves. In an ideal gravitationalwave interferometer a gravitational wave with memory causes a permanent displacement of the test masses that persists after the wave has passed. Surprisingly, the nonlinear memory affects the signal amplitude starting at leading (Newtonian-quadrupole) order. Despite this fact, the nonlinear memory is not easily extracted from current numerical relativity simulations. After reviewing the linear and nonlinear memory I summarize some recent work, including (1) computations of the memory contribution to the inspiral waveform amplitude (thus completing the waveform to third post-Newtonian order); (2) the first calculations of the nonlinear memory that include all phases of binary black hole coalescence (inspiral, merger, ringdown); and (3) realistic estimates of the detectability of the memory with LISA.},
  date      = {2010-04-06},
  day       = {6},
  doi       = {10.1088/0264-9381/27/8/084036},
  file      = {:Favata2010 - The Gravitational Wave Memory Effect.pdf:PDF},
  keywords  = {numbers: 04.25.Nx, 04.30.Db, 04.30.Tv, 95.30.Sf},
  publisher = {{IOP} Publishing},
}

@Article{Berry2019,
  author   = {Berry, Christopher and Hughes, Scott and Sopuerta, Carlos and Chua, Alvin and Heffernan, Anna and Holley-Bockelmann, Kelly and Mihaylov, Deyan and Miller, Coleman and Sesana, Alberto},
  journal  = {Bulletin of the American Astronomical Society},
  title    = {Astro2020 Science White Paper: The unique potential of extreme mass-ratio inspirals for gravitational-wave astronomy},
  year     = {2019},
  month    = may,
  note     = {ADS Bibcode: 2019BAAS...51c..42B},
  pages    = {42},
  volume   = {51},
  abstract = {EMRIs are a prime source for LISA. They will tell us about the stellar dynamics in galactic nuclei and massive black hole populations. They will enable percent-level measurements of the multipolar structure of massive black holes and tests of the strong-gravity regime. They may also provide cosmographical data about the expansion of the Universe.},
  doi      = {10.48550/arXiv.1903.03686},
  file     = {:Berry2019 - Astro2020 Science White Paper_ the Unique Potential of Extreme Mass Ratio Inspirals for Gravitational Wave Astronomy.pdf:PDF},
  keywords = {Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology},
  url      = {https://ui.adsabs.harvard.edu/abs/2019BAAS...51c..42B},
  urldate  = {2024-11-23},
}

@Article{AmaroSeoane2018,
  author    = {Amaro-Seoane, Pau},
  journal   = {Living Reviews in Relativity},
  title     = {Relativistic dynamics and extreme mass ratio inspirals},
  year      = {2018},
  issn      = {1433-8351},
  month     = may,
  number    = {1},
  volume    = {21},
  abstract  = {Living Reviews in Relativity, https://doi.org/10.1007/s41114-018-0013-8},
  doi       = {10.1007/s41114-018-0013-8},
  file      = {:AmaroSeoane2018 - Relativistic Dynamics and Extreme Mass Ratio Inspirals.pdf:PDF},
  keywords  = {Black holes,Gravitational waves,Stellar dynamics},
  publisher = {Springer Science and Business Media LLC},
}

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