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Estimate of stellar masses from their QPO frequencies

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Abstract

Kilohertz quasiperiodic oscillations (kHz QPOs) are observed in binary stellar systems. For such a system, the stellar radius is very close to the marginally stable orbit R ms as predicted by Einstein’s general relativity. Many models have been proposed to explain the origin of the kHz QPO features in the binaries. Here we start from the work of Li et al (Phys. Rev . Lett. 83, 3776 (1999)) who in 1999, from the unique millisecond X-ray pulsations, suggested SAX J1808.4−3658 to be a strange star, from an accurate determination of its rotation period. It showed kHz QPOs eight years ago and so far it is the only set that has been observed. We suggest that the mass of four compact stars SAX J1808.4−3658, KS 1731−260, SAX J1750.8−2900 and IGR J17191−2821 can be determined from the difference in the observed kHz QPOs of these stars. It is exciting to be able to give an estimate of the mass of the star and three other compact stars in low-mass X-ray binaries using their observed kHz QPOs.

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Authors and Affiliations

  1. Astrophysics and Cosmology Research Unit, School of Mathematical Sciences, University of KwaZulu-Natal, Durban, 4000, South Africa

    SUBHARTHI RAY

  2. Department of Physics, Presidency University, Kolkata, 700 073, India

    TAPARATI GANGOPADHYAY, JISHNU DEY & MIRA DEY

  3. Inter-University Centre for Astronomy and Astrophysics, Ganeshkhind, Pune, 411 007, India

    JISHNU DEY & MIRA DEY

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  1. SUBHARTHI RAY
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  2. TAPARATI GANGOPADHYAY
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Correspondence to SUBHARTHI RAY.

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RAY, S., GANGOPADHYAY, T., DEY, J. et al. Estimate of stellar masses from their QPO frequencies. Pramana - J Phys 77, 571–579 (2011). https://doi.org/10.1007/s12043-011-0176-2

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  • DOI: https://doi.org/10.1007/s12043-011-0176-2

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