Possible signatures for strange stars in stellar X-ray binaries

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dc.creatorDatta, Bhaskar
dc.creatorThampan, Arun V.
dc.creatorBombaci, Ignazio
dc.date1999-12-08
dc.date.accessioned2026-07-07T02:34:52Z
dc.date.available2026-07-07T02:34:52Z
dc.descriptionKilohertz quasi-periodic brightness oscillations (kHz QPOs) observed in certain X-ray burst sources may represent Keplerian frequencies in the inner regions of the accretion disk in such systems. If this assumption is strictly adhered to, we show here that if the central accretor in stellar X-ray burst sources is a strange star (made up of u, d and s quarks in beta equilibrium, referred to as strange matter) then the calculated QPO frequencies are reconcilable with the observed QPO frequencies (corresponding to the highest frequency of 1.22 kHz, observed so far from the source 4U 1636-53) only for particular values of the QCD-related parameters which describe the equation of state of strange matter. We demonstrate that QPO frequencies in the very high range (1.9-3.1) kHz can be understood in terms of a (non- magnetized) strange star X-ray binary (SSXB) rather than a neutron star X-ray binary (NSXB). Future discovery of such high frequency QPOs from X-ray burst sources will constitute a new astrophysical di- agnostic for identifying solar mass range stable strange stars in our galaxy.
dc.description4 pages, 2 figs., uses psbox.tex, submitted to A&A
dc.identifierhttps://arxiv.org/abs/astro-ph/9912173
dc.identifierhttp://arxiv.org/abs/astro-ph/9912173
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/15412
dc.subjectAstrophysics
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectNuclear Theory
dc.titlePossible signatures for strange stars in stellar X-ray binaries
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