Accretion flow dynamics during 1999 outburst of XTE J1859+226—modeling of broadband spectra and constraining the source mass - INSPIRE

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Accretion flow dynamics during 1999 outburst of XTE J1859+226—modeling of broadband spectra and constraining the source mass

Mar 22, 2018

12 pages

Published in:

Astrophys.Space Sci. 363 (2018) 5, 90

Published: Apr 9, 2018

e-Print:

1803.08638 [astro-ph.HE]

DOI:

10.1007/s10509-018-3314-1

View in:

ADS Abstract Service

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Abstract: (Springer)

We examine the dynamical behavior of accretion flow around XTE J1859+226 during the 1999 outburst by analyzing the entire outburst data (∼166 days) from RXTE Satellite. Towards this, we study the hysteresis behavior in the hardness intensity diagram (HID) based on the broadband (3–150 keV) spectral modeling, spectral signature of jet ejection and the evolution of Quasi-periodic Oscillation (QPO) frequencies using the two-component advective flow model around a black hole. We compute the flow parameters, namely Keplerian accretion rate (

{\dot{m}}_{d}

), sub-Keplerian accretion rate (

{\dot{m}}_{h}

), shock location (

r_{s}

) and black hole mass (

M_{\mathit{bh}}

) from the spectral modeling and study their evolution along the q-diagram. Subsequently, the kinetic jet power is computed as L^{\mathrm{obs}}_{\mathrm{jet}} \sim3\mbox{--}6 \times10^{37}~\mbox{erg}\,\mbox{s}^{-1} during one of the observed radio flares which indicates that jet power corresponds to 8–16% mass outflow rate from the disc. This estimate of mass outflow rate is in close agreement with the change in total accretion rate (∼14%) required for spectral modeling before and during the flare. Finally, we provide a mass estimate of the source XTE J1859+226 based on the spectral modeling that lies in the range of 5.2–7.9

M_{\odot}

with 90% confidence.

Note:

12 pages, 8 figures, 3 tables, Accepted for publication in Astrophysics and Space Science

Accretion
Accretion discs
Black hole physics
Radiation mechanisms: non thermal
X rays: binaries
ISM: jets and outflows
Stars: black holes

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