Observations of AR Sco with $Chandra$ and $AstroSat$ Soft X-ray Telescope

Abstract

We present our $AstroSat$ soft X-ray observations of a compact binary system, AR Sco, and analysis of its X-ray observations with $Chandra$ that were taken only about a week before the $AstroSat$ observations. An analysis of the soft X-ray ($0.3-2.0$ keV) data limits the modulation of the spin, orbital, or beat periods to less than 0.03 counts s${}^{-1}$ or $<$10\% of the average count rate. The X-ray flux obtained from both observatories is found to be almost identical (within a few percent) in flux, and about 30\% lower than reported from the nine months older observations with $XMM-Newton$. A two-temperature thermal plasma model with the same spectral parameters fit $Chandra$ and $AstroSat$ data very well, and requires very little absorption in the line of sight to the source. The low-temperature component has the same temperature ($\sim$1 keV) as reported earlier, but the high-temperature component has a lower temperature of 5.0${}_{-0.7}^{+0.8}$ keV as compared to 8.0 keV measured earlier, however, the difference is not statistically significant.

9 pages, 8 figures, to be published in the Journal of Astrophysics and Astronomy

References in corpus (4)

• A radio pulsing white dwarf binary star
• Polarimetric evidence of a white dwarf pulsar in the binary system AR Scorpii
• An Improved Spin-Down Rate for the Proposed White-Dwarf Pulsar AR Scorpii
• Constraining the Emission Geometry and Mass of the White Dwarf Pulsar AR Sco using the Rotating Vector Model

Cited by in corpus (1)

• Periodic Radio and X-ray Emission from an Accreting White Dwarf Binary