Mass Evaluation of The Microquasar XTE J1807-294 by Means of the Relativistic Precession Model. (arXiv:1811.05223v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tasheva_R/0/1/0/all/0/1">Radostina P. Tasheva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stefanov_I/0/1/0/all/0/1">Ivan Zh. Stefanov</a>
The high frequency quasiperiodic oscillations (QPOs) in the X-ray spectra of
the millisecond pulsar XTE J1807-294 are under consideration. By application of
the relativistic precession (RP) model an attempt is made to approximate the
observed frequencies as well as to assess the mass and the angular momentum of
the object. The obtained mass is too high for a neutron star.
The high frequency quasiperiodic oscillations (QPOs) in the X-ray spectra of
the millisecond pulsar XTE J1807-294 are under consideration. By application of
the relativistic precession (RP) model an attempt is made to approximate the
observed frequencies as well as to assess the mass and the angular momentum of
the object. The obtained mass is too high for a neutron star.
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