Controversy of the GRO J1655-40 black hole mass and spin estimates and its possible solutions

Abstract

Estimates of the black hole mass $M$ and dimensionless spin $a$ in the microquasar GRO J1655-40 implied by strong gravity effects related to the timing and spectral measurements are controversial, if the mass restriction determined by the dynamics related to independent optical measurements, $M_{\mathrm{opt}}=(5.4\pm 0.3)M_{\odot }$, are applied. The timing measurements of twin high-frequency (HF) quasiperiodic oscillations (QPOs) with frequency ratio $3:2$ and the simultaneously observed low-frequency (LF) QPO imply the spin in the range $a\in (0.27-0.29)$ if models based on the frequencies of the geodesic epicyclic motion are used to fit the timing measurements, and correlated creation of the twin HF QPOs and the LF QPO at a common radius is assumed. On the other hand, the spectral continuum method implies $a\in (0.65-0.75)$, and the Fe-line-profile method implies $a\in (0.94-0.98)$. This controversy can be cured, if we abandon the assumption of the occurrence of the twin HF QPOs and the simultaneously observed LF QPO at a common radius. We demonstrate that the epicyclic resonance model of the twin HF QPOs is able to predict the spin in agreement with the Fe-profile method, but no model based on the geodesic epicyclic frequencies can be in agreement with the spectral continuum method. We also show that the non-geodesic string loop oscillation model of twin HF QPOs predicts spin $a>0.3$ under the optical measurement limit on the black hole mass, in agreement with both the spectral continuum and Fe-profile methods.

10 pages, 3 figures, 2 tables

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• Current-carrying string loops in black-hole spacetimes with a repulsive cosmological constant
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• Acceleration of electric current-carrying string loop near a Schwarzschild black hole immersed in an asymptotically uniform magnetic field
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• Super-spinning compact objects and models of high-frequency quasi-periodic oscillations observed in Galactic microquasars. II. Forced resonances
• Measuring Black Hole Spins through X-ray Reflection Spectroscopy and the Relativistic Precession Model: the case of XTE J1859+226
• Accretion Disc Evolution in GRO J1655-40 and LMC X-3 with Relativistic and Non-Relativistic Disc Models
• Testing Ghasemi-Nodehi-Bambi metric parameters with quasi-periodic oscillations
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• A simplified approach for reproducing fully relativistic spectra in X-ray binary systems: Application to Cygnus X-1
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• Lense-Thirring precession of neutron-star accretion flows: Relativistic versus classical precession
• On the origin of core radio emissions from black hole sources in the realm of relativistic shocked accretion flow