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IRIS
The recent discovery by Advanced LIGO and Advanced Virgo of a gravitational wave signal from a binary neutron star inspiral has enabled tests of general relativity (GR) with this new type of source. This source, for the first time, permits tests of strong-field dynamics of compact binaries in the presence of matter. In this Letter, we place constraints on the dipole radiation and possible deviations from GR in the post-Newtonian coefficients that govern the inspiral regime. Bounds on modified dispersion of gravitational waves are obtained; in combination with information from the observed electromagnetic counterpart we can also constrain effects due to large extra dimensions. Finally, the polarization content of the gravitational wave signal is studied. The results of all tests performed here show good agreement with GR.
Tests of General Relativity with GW170817 / Abbott, B P; Abbott, R; Abbott, T D; Acernese, F; Ackley, K; Adams, C; Adams, T; Addesso, P; Adhikari, R X; Adya, V B; Affeldt, C; Agarwal, B; Agathos, M; Agatsuma, K; Aggarwal, N; Aguiar, O D; Aiello, L; Ain, A; Ajith, P; Allen, B; Allen, G; Allocca, A; Aloy, M A; Altin, P A; Amato, A; Ananyeva, A; Anderson, S B; Anderson, W G; Angelova, S V; Antier, S; Appert, S; Arai, K; Araya, M C; Areeda, J S; Arène, M; Arnaud, N; Arun, K G; Ascenzi, S; Ashton, G; Ast, M; Aston, S M; Astone, P; Atallah, D V; Aubin, F; Aufmuth, P; Aulbert, C; Aultoneal, K; Austin, C; Avila-Alvarez, A; Babak, S; Bacon, P; Badaracco, F; Bader, M K M; Bae, S; Baker, P T; Baldaccini, F; Ballardin, G; Ballmer, S W; Banagiri, S; Barayoga, J C; Barclay, S E; Barish, B C; Barker, D; Barkett, K; Barnum, S; Barone, F; Barr, B; Barsotti, L; Barsuglia, M; Barta, D; Bartlett, J; Bartos, I; Bassiri, R; Basti, A; Batch, J C; Bawaj, M; Bayley, J C; Bazzan, M; Bécsy, B; Beer, C; Bejger, M; Belahcene, I; Bell, A S; Beniwal, D; Bensch, M; Berger, B K; Bergmann, G; Bernuzzi, S; Bero, J J; Berry, C P L; Bersanetti, D; Bertolini, A; Betzwieser, J; Bhandare, R; Bilenko, I A; Bilgili, S A; Billingsley, G; Billman, C R; Birch, J; Birney, R; Birnholtz, O; Biscans, S; Biscoveanu, S; Bisht, A; Bitossi, M; Bizouard, M A; Blackburn, J K; Blackman, J; Blair, C D; Blair, D G; Blair, R M; Bloemen, S; Bock, O; Bode, N; Boer, M; Boetzel, Y; Bogaert, G; Bohe, A; Bondu, F; Bonilla, E; Bonnand, R; Booker, P; Boom, B A; Booth, C D; Bork, R; Boschi, V; Bose, S; Bossie, K; Bossilkov, V; Bosveld, J; Bouffanais, Y; Bozzi, A; Bradaschia, C; Brady, P R; Bramley, A; Branchesi, M; Brau, J E; Briant, T; Brighenti, F; Brillet, A; Brinkmann, M; Brisson, V; Brockill, P; Brooks, A F; Brown, D D; Brunett, S; Buchanan, C C; Buikema, A; Bulik, T; Bulten, H J; Buonanno, A; Buskulic, D; Buy, C; Byer, R L; Cabero, M; Cadonati, L; Cagnoli, G; Cahillane, C; Bustillo, J Calderón; Callister, T A; Calloni, E; Camp, J B; Canepa, M; Canizares, P; Cannon, K C; Cao, H; Cao, J; Capano, C D; Capocasa, E; Carbognani, F; Caride, S; Carney, M F; Carullo, G; Diaz, J Casanueva; Casentini, C; Caudill, S; Cavaglià, M; Cavalier, F; Cavalieri, R; Cella, G; Cepeda, C B; Cerdá-Durán, P; Cerretani, G; Cesarini, E; Chaibi, O; Chamberlin, S J; Chan, M; Chao, S; Charlton, P; Chase, E; Chassande-Mottin, E; Chatterjee, D; Chatziioannou, K; Cheeseboro, B D; Chen, H Y; Chen, X; Chen, Y; Cheng, H-P; Chia, H Y; Chincarini, A; Chiummo, A; Chmiel, T; Cho, H S; Cho, M; Chow, J H; Christensen, N; Chu, Q; Chua, A J K; Chua, S; Chung, K W; Chung, S; Ciani, G; Ciobanu, A A; Ciolfi, R; Cipriano, F; Cirelli, C E; Cirone, A; Clara, F; Clark, J A; Clearwater, P; Cleva, F; Cocchieri, C; Coccia, E; Cohadon, P-F; Cohen, D; Colla, A; Collette, C G; Collins, C; Cominsky, L R; Constancio, M; Conti, L; Cooper, S J; Corban, P; Corbitt, T R; Cordero-Carrión, I; Corley, K R; Cornish, N; Corsi, A; Cortese, S; Costa, C A; Cotesta, R; Coughlin, M W; Coughlin, S B; 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[10.1103/PhysRevLett.123.011102]
Tests of General Relativity with GW170817
Abbott, B P;Abbott, R;Abbott, T D;Acernese, F;Ackley, K;Adams, C;Adams, T;Addesso, P;Adhikari, R X;Adya, V B;Affeldt, C;Agarwal, B;Agathos, M;Agatsuma, K;Aggarwal, N;Aguiar, O D;Aiello, L;Ain, A;Ajith, P;Allen, B;Allen, G;Allocca, A;Aloy, M A;Altin, P A;Amato, A;Ananyeva, A;Anderson, S B;Anderson, W G;Angelova, S V;Antier, S;Appert, S;Arai, K;Araya, M C;Areeda, J S;Arène, M;Arnaud, N;Arun, K G;Ascenzi, S;Ashton, G;Ast, M;Aston, S M;Astone, P;Atallah, D V;Aubin, F;Aufmuth, P;Aulbert, C;AultONeal, K;Austin, C;Avila-Alvarez, A;Babak, S;Bacon, P;Badaracco, F;Bader, M K M;Bae, S;Baker, P T;Baldaccini, F;Ballardin, G;Ballmer, S W;Banagiri, S;Barayoga, J C;Barclay, S E;Barish, B C;Barker, D;Barkett, K;Barnum, S;Barone, F;Barr, B;Barsotti, L;Barsuglia, M;Barta, D;Bartlett, J;Bartos, I;Bassiri, R;Basti, A;Batch, J C;Bawaj, M;Bayley, J C;Bazzan, M;Bécsy, B;Beer, C;Bejger, M;Belahcene, I;Bell, A S;Beniwal, D;Bensch, M;Berger, B K;Bergmann, G;Bernuzzi, S;Bero, J J;Berry, C P L;Bersanetti, D;Bertolini, A;Betzwieser, J;Bhandare, R;Bilenko, I A;Bilgili, S A;Billingsley, G;Billman, C R;Birch, J;Birney, R;Birnholtz, O;Biscans, S;Biscoveanu, S;Bisht, A;Bitossi, M;Bizouard, M A;Blackburn, J K;Blackman, J;Blair, C D;Blair, D G;Blair, R M;Bloemen, S;Bock, O;Bode, N;Boer, M;Boetzel, Y;Bogaert, G;Bohe, A;Bondu, F;Bonilla, E;Bonnand, R;Booker, P;Boom, B A;Booth, C D;Bork, R;Boschi, V;Bose, S;Bossie, K;Bossilkov, V;Bosveld, J;Bouffanais, Y;Bozzi, A;Bradaschia, C;Brady, P R;Bramley, A;Branchesi, M;Brau, J E;Briant, T;Brighenti, F;Brillet, A;Brinkmann, M;Brisson, V;Brockill, P;Brooks, A F;Brown, D D;Brunett, S;Buchanan, C C;Buikema, A;Bulik, T;Bulten, H J;Buonanno, A;Buskulic, D;Buy, C;Byer, R L;Cabero, M;Cadonati, L;Cagnoli, G;Cahillane, C;Bustillo, J Calderón;Callister, T A;Calloni, E;Camp, J B;Canepa, M;Canizares, P;Cannon, K C;Cao, H;Cao, J;Capano, C D;Capocasa, E;Carbognani, F;Caride, S;Carney, M F;Carullo, G;Diaz, J Casanueva;Casentini, C;Caudill, S;Cavaglià, M;Cavalier, 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S J;Zhu, X J;Zimmerman, A B;Zucker, M E;Zweizig, J
2019-01-01
Abstract
The recent discovery by Advanced LIGO and Advanced Virgo of a gravitational wave signal from a binary neutron star inspiral has enabled tests of general relativity (GR) with this new type of source. This source, for the first time, permits tests of strong-field dynamics of compact binaries in the presence of matter. In this Letter, we place constraints on the dipole radiation and possible deviations from GR in the post-Newtonian coefficients that govern the inspiral regime. Bounds on modified dispersion of gravitational waves are obtained; in combination with information from the observed electromagnetic counterpart we can also constrain effects due to large extra dimensions. Finally, the polarization content of the gravitational wave signal is studied. The results of all tests performed here show good agreement with GR.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11572/370430
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 589/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.
