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  Keplerian frequencies and innermost stable circular orbits of rapidly rotating strange stars

Stergioulas, N., Kluzniak, W., & Bulik, T. (1999). Keplerian frequencies and innermost stable circular orbits of rapidly rotating strange stars. Astronomy and Astrophysics, 352, L116-L120.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-5858-8 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-5859-6
Genre: Journal Article

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2785.pdf (Publisher version), 119KB
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Stergioulas, Nikolaos1, Author
Kluzniak, W., Author
Bulik, T., Author
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013              

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 Abstract: It has been suggested that the frequency in the co-rotating innermost stable circular orbit (ISCO) about a compact stellar remnant can be determined through X-ray observations of low-mass X-ray binaries, and that its value can be used to constrain the equation of state of ultradense matter. Upon constructing numerical models of rapidly rotating strange (quark) stars in general relativity, we find that for stars rotating at the equatorial mass-shedding limit, the ISCO is indeed above the stellar surface, for a wide range of central energy densities at a height equal to 11% of the circumferential stellar radius, which scales inversely with the square root of the energy density, of self-bound quark matter at zero presure. In contrast to static stars, the ISCO frequencies of rapidly rotating strange stars can be as low as 0.9 kHz for a 1.3 solar mass strange star. Hence, the presence of strange stars in low-mass X-ray binaries cannot be excluded on the basis of the currently observed frequencies of kHz QPOs, such as the cut-off frequency of 1066 Hz in 4U 1820-30.

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Language(s): eng - English
 Dates: 1999
 Publication Status: Published in print
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 Identifiers: eDoc: 2785
Other: 27966
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Title: Astronomy and Astrophysics
Source Genre: Journal
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Pages: - Volume / Issue: 352 Sequence Number: - Start / End Page: L116 - L120 Identifier: -