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Inner disc obscuration in GRS 1915+105 based on relativistic slim disc model
Vierdayanti K.a, Sadowski A.b, Mineshige S.c, Bursa M.
a Department of Astronomy, FMIPA, Institut Teknologi Bandung, Indonesia
b Harvard-Smithsonian Center for Astrophysics, United States
c Department of Astronomy, Kyoto University, Japan
d Astronomical Institute, Academy of Sciences of the Czech Republic, Czech Republic
[vc_row][vc_column][vc_row_inner][vc_column_inner][vc_separator css=”.vc_custom_1624529070653{padding-top: 30px !important;padding-bottom: 30px !important;}”][/vc_column_inner][/vc_row_inner][vc_row_inner layout=”boxed”][vc_column_inner width=”3/4″ css=”.vc_custom_1624695412187{border-right-width: 1px !important;border-right-color: #dddddd !important;border-right-style: solid !important;border-radius: 1px !important;}”][vc_empty_space][megatron_heading title=”Abstract” size=”size-sm” text_align=”text-left”][vc_column_text]We study the observational signatures of the relativistic slim disc of 10M black hole, in a wide range of mass accretion rate, m, dimensionless spin parameter, a*, and viewing angle, i. In general, the innermost temperature, Tin, increases with the increase of i for a fixed value of m and a*, due to the Doppler effect. However, for i > 50° and m > mturn, Tin starts to decrease with the increase of m. This is a result of self-obscuration – the radiation from the innermost hot part of the disc is blocked by the surrounding cooler part. The value of mturn and the corresponding luminosities depend on a* and i. Such obscuration effects cause an interesting behaviour on the disc luminosity (Ldisc)αTin4 plane for high inclinations. In addition to the standard disc branch which appears below mturn and which obeys Ldisc T 4 in relation, another branch above mturn, which is nearly horizontal, may be observed at luminosities close to the Eddington luminosity. We show that these features are likely observed in a Galactic X-ray source, GRS 1915+105. We support a high spin parameter (a* > 0.9) for GRS 1915+105 since otherwise the high value of Tin and small size of the emitting region (rin 1rS) cannot be explained. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Author keywords” size=”size-sm” text_align=”text-left”][vc_column_text][/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Indexed keywords” size=”size-sm” text_align=”text-left”][vc_column_text]Accretion,Accretion discs – black hole physics – stars,Binaries,GRS 1915+105 -X-rays,Individual[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Funding details” size=”size-sm” text_align=”text-left”][vc_column_text][/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”DOI” size=”size-sm” text_align=”text-left”][vc_column_text]https://doi.org/10.1093/mnras/stt1467[/vc_column_text][/vc_column_inner][vc_column_inner width=”1/4″][vc_column_text]Widget Plumx[/vc_column_text][/vc_column_inner][/vc_row_inner][/vc_column][/vc_row][vc_row][vc_column][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][/vc_column][/vc_row]