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Last orbits of binary strange quark stars
General Relativity and Quantum Cosmology · Submitted 26 Nov 2004
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that the innermost stable circular orbit (ISCO) is given by an orbital instability both for synchronized and irrotational systems.
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The abstract, sentence by sentence
We present the first relativistic calculations of the final phase of inspiral of a binary system consisting of two stars built predominantely of strange quark matter (strange quark stars). We study the precoalescing stage within the Isenberg-Wilson-Mathews approximation of general relativity using a multidomain spectral method. A hydrodynamical treatment is performed under the assumption that the flow is either rigidly rotating or irrotational, taking into account the finite density at the stellar surface -- a distinctive feature with respect to the neutron star case. The gravitational-radiation driven evolution of the binary system is approximated by a sequence of quasi-equilibrium configurations at fixed baryon number and decreasing separation. We find that the innermost stable circular orbit (ISCO) is given by an orbital instability both for synchronized and irrotational systems. This constrasts with neutron stars for which the ISCO is given by the mass-shedding limit in the irrotational case. The gravitational wave frequency at the ISCO, which marks the end of the inspiral phase, is found to be 1400 Hz for two irrotational 1.35 Msol strange stars and for the MIT bag model of strange matter with massless quarks and a bag constant B=60 MeV/fm^3. Detailed comparisons with binary neutrons star models, as well as with third order Post-Newtonian point-mass binaries are given.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present the first relativistic calculations of the final phase of inspiral of a binary system consisting of two stars built predominantely of strange quark matter (strange quark stars). | contribution 1.00 | 0.96 | 0.07 | asserted 0.99 |
| s1 | We study the precoalescing stage within the Isenberg-Wilson-Mathews approximation of general relativity using a multidomain spectral method. | method 0.99 | 0.88 | 0.02 | asserted 0.98 |
| s2 | A hydrodynamical treatment is performed under the assumption that the flow is either rigidly rotating or irrotational, taking into account the finite density at the stellar surface -- a distinctive feature with respect to the neutron star case. | method 1.00 | 0.88 | 0.03 | asserted 0.97 |
| s3 | The gravitational-radiation driven evolution of the binary system is approximated by a sequence of quasi-equilibrium configurations at fixed baryon number and decreasing separation. | method 1.00 | 0.77 | 0.05 | asserted 0.96 |
| s4 | We find that the innermost stable circular orbit (ISCO) is given by an orbital instability both for synchronized and irrotational systems. | result 1.00 | 0.97 | 0.49 | asserted 1.00 |
| s5 | This constrasts with neutron stars for which the ISCO is given by the mass-shedding limit in the irrotational case. | interpretation 0.64 | 0.32 | 0.20 | asserted 1.00 |
| s6 | The gravitational wave frequency at the ISCO, which marks the end of the inspiral phase, is found to be 1400 Hz for two irrotational 1.35 Msol strange stars and for the MIT bag model of strange matter with massless quarks and a bag constant B=60 MeV/fm^3. | result 1.00 | 0.96 | 0.38 | asserted 1.00 |
| s7 | Detailed comparisons with binary neutrons star models, as well as with third order Post-Newtonian point-mass binaries are given. | contribution 0.72 | 0.79 | 0.03 | asserted 0.96 |
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Original abstract
We present the first relativistic calculations of the final phase of inspiral of a binary system consisting of two stars built predominantely of strange quark matter (strange quark stars). We study the precoalescing stage within the Isenberg-Wilson-Mathews approximation of general relativity using a multidomain spectral method. A hydrodynamical treatment is performed under the assumption that the flow is either rigidly rotating or irrotational, taking into account the finite density at the stellar surface -- a distinctive feature with respect to the neutron star case. The gravitational-radiation driven evolution of the binary system is approximated by a sequence of quasi-equilibrium configurations at fixed baryon number and decreasing separation. We find that the innermost stable circular orbit (ISCO) is given by an orbital instability both for synchronized and irrotational systems. This constrasts with neutron stars for which the ISCO is given by the mass-shedding limit in the irrotational case. The gravitational wave frequency at the ISCO, which marks the end of the inspiral phase, is found to be 1400 Hz for two irrotational 1.35 Msol strange stars and for the MIT bag model of strange matter with massless quarks and a bag constant B=60 MeV/fm^3. Detailed comparisons with binary neutrons star models, as well as with third order Post-Newtonian point-mass binaries are given.
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7 arXiv papers cite this in 7 sentences
Papers citing it · 6 sentences without a confident label
Cites it as background 1 paper
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Previously, various efforts have been made in the calculation of the quasi-/equilibrium structures of uniformly and differentially rotating QSs in general relativity (GR) [ref] as well as the configuration of BQSs in the last orbits [ref] .
Evolution of bare quark stars in full general relativity: Single star case · Introduction · 0.98
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