ERRATUM: “BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE CRAB PULSAR” (2008, ApJ, 683, L45)

Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Ajith, P.; Allen, B.; Allen, G.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.; Araya, M. C.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S. M.; Aufmuth, P.; Aulbert, C.; Babak, S.; Ballmer, S. W.; Bantilan, H.; Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bastarrika, M.; Bayer, K.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.; Blackburn, L.; Blair, David; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Brinkmann, M.; Brooks, A. F.; Brown, D. A.; Brunet, G.; Bullington, A.; Buonanno, A.; Burmeister, O.; Byer, Robert L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J. K.; Cannon, K. C.; Cao, J.; Cardenas, L.; Casebolt, T.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Clark, D.; Clark, J. A.; Cokelaer, Thomas; Conte, R.; Cook, D.; Corbitt, T. R.; Coyne, D. C.; Creighton, J. D. E.; Cumming, A.; Cunningham, L.; Cutler, R. M.; Dalrymple, James; Danzmann, K.; Davies, G.; DeBra, D.; Degallaix, J.; Degree, M.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.; Díaz, M. C.; Dickson, J.; Dietz, A.; Donovan, Frederick J; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Duke, I.; Dumas, J. C.; Dupuis, R. J.; Dwyer, J. G.; Echols, C.; Effler, A.; Ehrens, P.; Espinoza, Eduardo; Etzel, T.; Evans, T. M.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fehrmann, H.; Fejer, M. M.; Finn, L. S.; Flasch, Kurt; Fotopoulos, N.; Freise, A.; Frey, R.; Fricke, T. T.; Fritschel, P.; Фролов, В. В.; Fyffe, M.; Garofoli, J.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, Keisuke; Goetz, E.; Goggin, L. M.; González, G.; Goßler, S.; Gouaty, R.; Grant, A.; Gras, S.; Gray, C.; Gray, Malcolm B.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grünewald, S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer, D. A.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harstad, E. D.; Hayama, K.; Hayler, T.; Heefner, J.; Heng, I. S.; Hennessy, M.; Heptonstall, A. W.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D. J.; Hough, J.; Huttner, S. H.; Ingram, D. R.; Ito, Masahiro; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.; Jones, Gareth; Jones, R.; Li, Ju; Kalmus, P.; Kalogera, V.; Kamat, S.; Kanner, J. B.; Kasprzyk, Dimitri; Katsavounidis, E.; Kawabe, K.; Kawamura, Seiji; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili, F. Y.; Khan, R.; Хазанов, Е. А.; Kim, C.; King, Peter; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Kozak, D. B.; Kozhevatov, I. E.; Krishnan, B.; Kwee, P.; Lam, Ping Koy; Landry, M.; Lang, M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leindecker, N.; Leonhardt, V.; Leonor, I.; Libbrecht, K. G.; Lin, H. L.; Lindquist, P.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.; Łubiński, M.; Lucianetti, Antonio; Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A. S.; Markowitz, J.; Maros, E.; Martin, Ian; Martin, R. M.; Marx, J. N.; Mason, K.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.; McKenzie, Kirk; Meier, T.; Melissinos, A. C.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyers, D.; Miller, J.; Minelli, J.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, Soumya D.; Moreno, G.; Mossavi, K.; Mow–Lowry, C. M.; Mueller, G.; Mukherjee, Suvodip; Mukhopadhyay, H.; Müller‐Ebhardt, H.; Münch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash, T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, Kenji; O’Dell, J.; Ogin, G. H.; O’Reilly, B.; O’Shaughnessy, R.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Perreca, A.; Pétrie, T.W.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Postiglione, F.; Principe, M.; Prix, R.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins, H.; Rainer, N.; Rakhmanov, M.; Ramsunder, M.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen, Rolf; Riles, K.; Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodríguez, A.; Rogan, A. M.; Rollins, J. G.; Romano, Joseph D.; Romie, J. H.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, Laurent; Russell, P.; Ryan, K.; Sakata, S.; Samidi, M.; Jordana, L. Sancho De La; Sandberg, V.; Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.; Savov, P.; Schediwy, Sascha; Schilling, R.; Schnabel, R.; Schofield, R. M. S.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein, L. C.; Stochino, A.; Stone, R.; Strain, K. A.; Strom, D.; Stuver, A. L.; Summerscales, T. Z.; Sun, K. X.; Sung, M.; Sutton, P. J.; Takahashi, Hideya; Tanner, D. B.; Taylor, Robert W.; Thacker, John G.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov, K. V.; Torres, C. V.; Torrie, C. I.; Traylor, G.; Trias, M.; Tyler, W.; Ugolini, D.; Ulmen, J.; Urbánek, Karel; Vahlbruch, H.; Broeck, C. Van Den; Sluys, M. van der; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P. J.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R. L.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut, Ian; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, Shijun; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.; Santostasi, G.

doi:10.1088/0004-637x/706/1/l203

Cited by 14 publications

(12 citation statements)

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“…This is well below the predicted sensitivity of even the proposed Einstein Telescope (see, e.g., Fig. 3 in Pitkin [22]), and around the minimum ellipticity quoted in [19] as being produced by an internal field of the same magnitude as the Crab's external field. (The Frieben and Rezzolla [13] fits predict an ellipticity of $10 À9 for an internal field of that strength.)…”

Section: Appendix: Corrections Due To Stresses and The Magnetic Fieldmentioning

confidence: 63%

“…The first of these errors is also present in an inline equation in the first paragraph of Sec. 1 of [19] and Eq. (14) of [21] [though Eq.…”

Section: Resultsmentioning

confidence: 99%

“…The second is also present in the first paragraph of Sec. 3 of [19], though the analogous Eqs. (6.1) in [17] and (15) in [21] are correct.…”

Section: Resultsmentioning

confidence: 99%

“…But the cleanest bounds come from gravitational wave observations, and a prominent accomplishment of the first generation of large-scale laser interferometer gravitational wave detectors has been setting direct upper bounds on the m ¼ 2 quadrupole moment of certain known neutron stars, below the bounds that are given by electromagnetic observations of the spin-down, or indirect limits given by the star's age [15,[19][20][21]. See [16,22,23] for recent reviews.…”

Section: Introductionmentioning

confidence: 99%

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Gravitational wave constraints on the shape of neutron stars

Johnson-McDaniel

2013

Phys. Rev. D

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We show that there is a direct relation between upper limits on (or potential future measurements of) the m = 2 quadrupole moments of slowly rotating neutron stars and the l = m = 2 deformation of the star's surface, in full general relativity, to first order in the perturbation. This relation only depends on the star's structure through its mass and radius. All one has to assume about the star's constituents is that the stress-energy tensor at its surface is that of a perfect fluid, which will be true with good accuracy in almost all the situations of interest, and that the magnetic field configuration there is force-free, which is likely to be a good approximation. We then apply this relation to the stars which have direct LIGO/Virgo bounds on their m = 2 quadrupole moment, below the spin-down limit, and compare with the expected surface deformations due to rotation. In particular, we find that LIGO observations have constrained the Crab pulsar's l = m = 2 surface deformation to be smaller than its l = 2, m = 0 deformation due to rotation, for all the causal equations of state we consider, a statement that would not have been able to be made just using the upper bounds on the l = m = 2 deformation from electromagnetic observations.Comment: 13 pages, 3 figures, version accepted by PRD, including expanded discussion of the calculation and a few correction

show abstract

Section: Appendix: Corrections Due To Stresses and The Magnetic Fieldmentioning

confidence: 63%

“…The first of these errors is also present in an inline equation in the first paragraph of Sec. 1 of [19] and Eq. (14) of [21] [though Eq.…”

Section: Resultsmentioning

confidence: 99%

“…The second is also present in the first paragraph of Sec. 3 of [19], though the analogous Eqs. (6.1) in [17] and (15) in [21] are correct.…”

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Gravitational wave constraints on the shape of neutron stars

Johnson-McDaniel

2013

Phys. Rev. D

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“…Among others, searches for continuous gravitational waves (CGWs) from known objects have been performed [1], including, for example, searches for CGWs from the low-mass x-ray binary Scorpius X-1 [2,3], the Cas A central compact object [4] and the Crab and Vela pulsars [5][6][7]. Extensive all-sky studies searching for as yet unknown neutron stars have been performed in recent years [8][9][10][11][12][13][14].…”

Section: Introductionmentioning

confidence: 99%

Directed search for continuous gravitational waves from the Galactic center

Aasi¹,

Abadie²,

Abbott³

et al. 2013

Phys. Rev. D

Self Cite

138

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We present the results of a directed search for continuous gravitational waves from unknown, isolated neutron stars in the Galactic center region, performed on two years of data from LIGO's fifth science run from two LIGO detectors. The search uses a semicoherent approach, analyzing coherently 630 segments, each spanning 11.5 hours, and then incoherently combining the results of the single segments. It covers gravitational wave frequencies in a range from 78 to 496 Hz and a frequency-dependent range of first-order spindown values down to -7.86 x 10(-8) Hz/s at the highest frequency. No gravitational waves were detected. The 90% confidence upper limits on the gravitational wave amplitude of sources at the Galactic center are similar to 3.35 x 10(-25) for frequencies near 150 Hz. These upper limits are the most constraining to date for a large-parameter-space search for continuous gravitational wave signals

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Searches for continuous gravitational waves from neutron stars: A twenty-year retrospective

Wette

2023

Astroparticle Physics

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ERRATUM: “BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE CRAB PULSAR” (2008, ApJ, 683, L45)

Cited by 14 publications

References 0 publications

Gravitational wave constraints on the shape of neutron stars

Gravitational wave constraints on the shape of neutron stars

Directed search for continuous gravitational waves from the Galactic center

Searches for continuous gravitational waves from neutron stars: A twenty-year retrospective

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