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Spectral analysis of χ class data of GRS 1915+105 using TCAF solution

Research in Astronomy and Astrophysics 2020年第12期20卷 347-356页

作者： anuvab banerjee Ayan Bhattacharjee Dipak Debnath Sandip K.Chakrabarti S.N.Bose National Centre for Basic Sciences Block-JDSector-3Salt LakeKolkata700106India Indian Centre for Space Physics 43 ChalantikaGaria St.Rd.Kolkata700084India

The class variable source GRS 1915+105 exhibits a wide range of time variabilities on timescales of a few seconds to a few days. Depending on the count rates in different energy bands and the nature of the conventional color-color diagram, the variabilities were classified into sixteen classes that were later sequenced in ascending order of Comptonization Efficiency(CE), which is the ratio of power-law and blackbody photons. However, CE estimation is based on an empirical model which does not provide us with a comprehensive picture regarding accretion flow dynamics around the central source. In reality, the accretion flow is comprised of two components: the high angular momentum Keplerian flow in the form of a radiatively efficient disk and a low angular momentum radiatively inefficient sub-Keplerian halo enveloping the disk. These two components contribute differently to the overall flux due to the differences in their radiative efficiencies. Therefore, it is necessary to analyze the spectral behaviors and time variabilities in terms of accretion rates. In χ class, X-ray flux is steady with no significant variation, however various χsubclasses are observed at different X-ray fluxes and variations of count rates across different χ subclasses must be linked to the variation of flow parameters such as the accretion rates, be it the Keplerian disk rate and/or the low angular momentum halo rate. This motivated us to analyze the spectra of the χ class data implementing the physical Two Component Advective Flow(TCAF) solution which directly extracts these two rates from spectral fits. We find that in the χ2,4 classes, which are reportedly devoid of significant outflows, the spectra could be fitted well applying the TCAF solution alone. In the χ1,3 classes, which are always linked with outflows, a cutoff power-law model is needed in addition to the TCAF *** the same time, the normalization required by this model along with the variation of photon index and exponent

关键词： X-Rays:binaries stars:individual(GRS 1915+105) stars:black holes accretion,accretion disks ISM:jets and outflows radiation:dynamics

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