# Spectral Analysis of $\chi$ Class Data of GRS 1915+105 Using TCAF Solution

## TL;DR

This study applies spectral analysis using the TCAF model to understand flow dynamics and variability classes of GRS 1915+105, revealing differences in accretion flow parameters and outflow contributions across classes.

## Contribution

It provides a detailed physical interpretation of the $ extit{ extbf{chi}}$ class variability in GRS 1915+105 using TCAF spectral fitting, highlighting flow geometry and outflow effects.

## Key findings

- TCAF model fits well for $ ext{chi}_2,4$ classes without outflows.
- Additional cutoff power-law needed for $ ext{chi}_1,3$ classes with outflows.
- Flow parameters and Compton cloud properties are derived from spectral fits.

## Abstract

The class variable source GRS 1915+105 exhibits a wide range of time variabilities in time scales 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, which were later sequenced in ascending order of Comptonization Efficiency (CE). The CE is the ratio of the phenomenological power-law and disk blackbody model fitted spectral photon fluxes. For a better understanding of the flow dynamics in one of the variability classes, namely $\chi$, we fitted spectra with the physical two-component advective flow (TCAF) model. In $\chi$ class, X-ray flux is steady with no significant variation, however, various $\chi$ subclasses are observed at different X-ray flux and variations of count rates across different $\chi$ subclasses must be linked to the variation of flow parameters such as the accretion rates, be it the Keplerian disc rate and/or the low angular momentum halo rate. We find that in the $\chi_{2,4}$ classes, which are reportedly devoid of significant outflows, the spectra could be fitted well using TCAF solution alone. In the $\chi_{1,3}$ class, which are always linked with outflows, a cutoff power-law model is needed in addition to the TCAF solution. At the same time, the normalization required by this model along with the variation of photon index and exponential roll-off factor provides us with the information on the relative dominance of the outflow in the latter two classes. TCAF fit also provides us with the size and location of the Compton cloud along with its optical depth. Thus by fitting with TCAF, a physical understanding of the flow geometry in different $\chi$ classes of GRS 1915+105 has been obtained.