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Article: Gravitational waves from phase-transition-induced collapse of neutron stars

TitleGravitational waves from phase-transition-induced collapse of neutron stars
Authors
KeywordsDense Matter
Gravitational Waves
Stars: Neutron
Stars: Oscillations
Issue Date2006
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2006, v. 639 n. 1 I, p. 382-396 How to Cite?
AbstractWe study the gravitational radiation from gravitational collapses of rapidly rotating neutron stars induced by a phase transition from normal nuclear matter to a mixed phase of quark and nuclear matter in the core of the stars. The study is based on self-consistent three-dimensional hydrodynamic simulations with Newtonian gravity and a high-resolution shock-capturing scheme and the quadrupole formula of gravitational radiation. The quark matter of the mixed phase is described by the MIT bag model and the normal nuclear matter is described by an ideal fluid EOS. While there is a broad range of interesting astrophysics problems associated with the phase-transition-induced gravitational collapse, we focus on the following: First, we determine the magnitudes of the emitted gravitational waves for several collapse scenarios, with gravitational wave amplitudes ranging from 0.3 × 10 -22 to 1.5 × 10 -22 for a source distance of 10 Mpc and the energy being carried away by the gravitational waves ranging between 0.3 × 10 51 and 2.8 × 10 51 ergs. Second, we determine the types and frequencies of the fluid oscillation modes excited by the process. In particular, we find that the gravitational wave signals produced by the collapses are dominated by the fundamental quadrupole and quasi-radial modes of the final equilibrium configurations. The two types of modes have comparable amplitude, with the latter mode representing the coupling between the rotation and radial oscillations induced by the collapse. In some collapse scenarios, we find that the oscillations are damped out within a few dynamical timescales due to the growth of differential rotations and the formation of strong shock waves. Third, we show that the spectrum of the gravitational wave signals is sensitive to the EOS, implying that the detection of such gravitational waves could provide useful constraints on the EOS of newly born quark stars. Finally, for the range of rotation periods studied, we find no sign of the development of nonaxisymmetric dynamical instabilities in the collapse process. © 2006. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175006
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorLin, LMen_US
dc.contributor.authorCheng, KSen_US
dc.contributor.authorChu, MCen_US
dc.contributor.authorSuen, WMen_US
dc.date.accessioned2012-11-26T08:48:44Z-
dc.date.available2012-11-26T08:48:44Z-
dc.date.issued2006en_US
dc.identifier.citationAstrophysical Journal Letters, 2006, v. 639 n. 1 I, p. 382-396en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175006-
dc.description.abstractWe study the gravitational radiation from gravitational collapses of rapidly rotating neutron stars induced by a phase transition from normal nuclear matter to a mixed phase of quark and nuclear matter in the core of the stars. The study is based on self-consistent three-dimensional hydrodynamic simulations with Newtonian gravity and a high-resolution shock-capturing scheme and the quadrupole formula of gravitational radiation. The quark matter of the mixed phase is described by the MIT bag model and the normal nuclear matter is described by an ideal fluid EOS. While there is a broad range of interesting astrophysics problems associated with the phase-transition-induced gravitational collapse, we focus on the following: First, we determine the magnitudes of the emitted gravitational waves for several collapse scenarios, with gravitational wave amplitudes ranging from 0.3 × 10 -22 to 1.5 × 10 -22 for a source distance of 10 Mpc and the energy being carried away by the gravitational waves ranging between 0.3 × 10 51 and 2.8 × 10 51 ergs. Second, we determine the types and frequencies of the fluid oscillation modes excited by the process. In particular, we find that the gravitational wave signals produced by the collapses are dominated by the fundamental quadrupole and quasi-radial modes of the final equilibrium configurations. The two types of modes have comparable amplitude, with the latter mode representing the coupling between the rotation and radial oscillations induced by the collapse. In some collapse scenarios, we find that the oscillations are damped out within a few dynamical timescales due to the growth of differential rotations and the formation of strong shock waves. Third, we show that the spectrum of the gravitational wave signals is sensitive to the EOS, implying that the detection of such gravitational waves could provide useful constraints on the EOS of newly born quark stars. Finally, for the range of rotation periods studied, we find no sign of the development of nonaxisymmetric dynamical instabilities in the collapse process. © 2006. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectDense Matteren_US
dc.subjectGravitational Wavesen_US
dc.subjectStars: Neutronen_US
dc.subjectStars: Oscillationsen_US
dc.titleGravitational waves from phase-transition-induced collapse of neutron starsen_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/499202en_US
dc.identifier.scopuseid_2-s2.0-33645008729en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33645008729&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume639en_US
dc.identifier.issue1 Ien_US
dc.identifier.spage382en_US
dc.identifier.epage396en_US
dc.identifier.isiWOS:000235836900034-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridLin, LM=8388053000en_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridChu, MC=7402457207en_US
dc.identifier.scopusauthoridSuen, WM=7006977947en_US

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