Cookies

We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.


Durham Research Online
You are in:

The thermal-radiative wind in low-mass X-ray binary H1743−322 – II : iron line predictions from Monte Carlo radiation transfer.

Takahashi, Tadayuki and Odaka, Hirokazu and Ohsuga, Ken and Done, Chris and Tomaru, Ryota (2020) 'The thermal-radiative wind in low-mass X-ray binary H1743−322 – II : iron line predictions from Monte Carlo radiation transfer.', Monthly notices of the Royal Astronomical Society., 494 (3). pp. 3413-3421.

Abstract

We show the best current simulations of the absorption and emission features predicted from thermal-radiative winds produced from X-ray illumination of the outer accretion disc in binary systems. We use the density and velocity structure derived from a radiation hydrodynamic code as input to a Monte Carlo radiation transport calculation. The initial conditions are matched to those of the black hole binary system H1743−322 in its soft, disc dominated state, where wind features are seen in Chandra grating data. Our simulation fits well to the observed line profile, showing that these physical wind models can be the origin of the absorption features seen, rather than requiring a magnetically driven wind. We show how the velocity structure is the key observable discriminator between magnetic and thermal winds. Magnetic winds are faster at smaller radii, whereas thermal winds transition to a static atmosphere at smaller radii. New data from XRISM (due for launch 2022 January) will give an unprecedented view of the physics of the wind launch and acceleration processes, but the existence of static atmospheres in small disc systems already rules out magnetic winds which assume self-similar magnetic fields from the entire disc as the origin of the absorption features seen.

Item Type:Article
Full text:(VoR) Version of Record
Download PDF
(2332Kb)
Status:Peer-reviewed
Publisher Web site:https://doi.org/10.1093/mnras/staa961
Publisher statement:This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. ©: 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:29 March 2020
Date deposited:17 June 2020
Date of first online publication:10 April 2020
Date first made open access:17 June 2020

Save or Share this output

Export:
Export
Look up in GoogleScholar