eprintid: 10204848
rev_number: 7
eprint_status: archive
userid: 699
dir: disk0/10/20/48/48
datestamp: 2025-02-18 16:04:44
lastmod: 2025-02-18 16:04:44
status_changed: 2025-02-18 16:04:44
type: article
metadata_visibility: show
sword_depositor: 699
creators_name: Dihingia, Indu K
creators_name: Mizuno, Yosuke
creators_name: Fromm, Christian M
creators_name: Younsi, Ziri
title: Impact of radiative cooling on the magnetised geometrically thin  accretion disc around Kerr black hole
ispublished: pub
divisions: UCL
divisions: B04
divisions: C06
divisions: F63
keywords: Accretion, Magnetohydrodynamics, X-ray binaries, Radiation processes
note: This version is the author accepted manuscript. For information on re-use, please refer to the publisher’s terms and conditions.
abstract: It is believed that the spectral state transitions of the outbursts in X-ray binaries (XRBs) are triggered by the rise of the mass accretion rate due to underlying disc instabilities. Recent observations found that characteristics of disc winds are probably connected with the different spectral states, but the theoretical underpinnings of it are highly ambiguous. To understand the correlation between disc winds and the dynamics of the accretion flow, we have performed General Relativistic Magneto-hydrodynamic (GRMHD) simulations of an axisymmetric thin accretion disc with different accretion rates and magnetic field strengths.
Our simulations have shown that the dynamics and the temperature properties depend on both accretion rates and magnetic field strengths. We later found that these properties greatly influence spectral properties. We calculated the average coronal temperature for different simulation models, which is correlated with high-energy Compton emission. Our simulation models reveal that the average coronal temperature is anti-correlated with the accretion rates, which are correlated with the magnetic field strengths. We also found that the structured component of the disc winds (Blandford-Payne disc wind) predominates as the accretion rates and magnetic field strengths increase. In contrast, the turbulent component of the disc winds (B
                  tor disc wind) predominates as the accretion rates and magnetic field strengths decrease. Our results suggest that the disc winds during an outburst in XRBs can only be understood if the magnetic field contribution varies over time (e.g., MAXI J1820+070).
date: 2025-01
date_type: published
publisher: IOP Publishing
official_url: https://doi.org/10.1088/1475-7516/2025/01/152
full_text_type: other
language: eng
verified: verified_manual
elements_id: 2357890
doi: 10.1088/1475-7516/2025/01/152
lyricists_name: Younsi, Ziri
lyricists_id: ZYOUN45
actors_name: Younsi, Ziri
actors_id: ZYOUN45
actors_role: owner
full_text_status: restricted
publication: Journal of Cosmology and Astroparticle Physics
volume: 2025
number: 1
pagerange: 152-152
issn: 1475-7516
citation:        Dihingia, Indu K;    Mizuno, Yosuke;    Fromm, Christian M;    Younsi, Ziri;      (2025)    Impact of radiative cooling on the magnetised geometrically thin accretion disc around Kerr black hole.                   Journal of Cosmology and Astroparticle Physics , 2025  (1)   p. 152.    10.1088/1475-7516/2025/01/152 <https://doi.org/10.1088/1475-7516%2F2025%2F01%2F152>.      
 
document_url: https://discovery.ucl.ac.uk/id/eprint/10204848/1/Thin_disk_with_cooling.pdf