Emission lines from X-ray illuminated accretion disc in black hole binaries

被引:3
作者
Mondal, Santanu [1 ,2 ]
Adhikari, Tek P. [3 ]
Singh, Chandra B. [4 ]
机构
[1] Indian Inst Astrophys, 2 Block, Koramangala 560034, Bengaluru, India
[2] Ben Gurion Univ Negev, Phys Dept, IL-84105 Beer Sheva, Israel
[3] Interuniv Ctr Astron & Astrophys IUCAA, Pune 411007, Maharashtra, India
[4] Yunnan Univ, South Western Inst Astron Res, Kunming 650500, Yunnan, Peoples R China
基金
中国国家自然科学基金;
关键词
accretion; accretion disc; atomic processes; line: formation; radiative transfer; ABSORPTION MEASURE DISTRIBUTION; RADIATION PRESSURE CONFINEMENT; 2-COMPONENT ADVECTIVE FLOWS; ACTIVE GALACTIC NUCLEI; SPECTRAL PROPERTIES; REFLECTION SPECTRA; COMPTON REFLECTION; STANDING SHOCKS; MASS OUTFLOW; COLD MATTER;
D O I
10.1093/mnras/stab1194
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 W-E 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.
引用
收藏
页码:1071 / 1082
页数:12
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