dc.contributor.author |
Mondal, Santanu |
|
dc.contributor.author |
Adhikari, Tek P |
|
dc.contributor.author |
Singh, Chandra B |
|
dc.date.accessioned |
2021-07-16T06:05:06Z |
|
dc.date.available |
2021-07-16T06:05:06Z |
|
dc.date.issued |
2021-07 |
|
dc.identifier.citation |
Monthly Notices of the Royal Astronomical Society, Vol. 505, No. 1, pp. 1071–1082 |
en_US |
dc.identifier.issn |
1365-2966 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/7789 |
|
dc.description |
Restricted Access |
en_US |
dc.description.abstract |
X-ray flux from the inner hot region around central compact object in a binary system illuminates the upper surface of an accretion disc and it behaves like a corona. This region can be photoionized by the illuminating radiation, and thus can emit different emission lines. We study those line spectra in black hole X-ray binaries for different accretion flow parameters including its geometry. The varying range of model parameters captures maximum possible observational features. We also put light on the routinely observed Fe-line emission properties based on different model parameters, ionization rate, and Fe abundances. We find that the Fe-line equivalent width WE decreases with increasing disc accretion rate and increases with the column density of the illuminated gas. Our estimated line properties are in agreement with observational signatures. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
Oxford University Press on behalf of the Royal Astronomical Society |
en_US |
dc.relation.uri |
https://doi.org/10.1093/mnras/stab1194 |
|
dc.rights |
© The Royal Astronomical Society |
|
dc.subject |
Accretion |
en_US |
dc.subject |
Accretion disc |
en_US |
dc.subject |
Atomic processes |
en_US |
dc.subject |
Line: formation |
en_US |
dc.subject |
Radiative transfer |
en_US |
dc.title |
Emission lines from X-ray illuminated accretion disc in black hole binaries |
en_US |
dc.type |
Article |
en_US |