# Application of the Thermal Wind Model to Absorption Features in the Black Hole X-ray Binary H 1743-322

**Authors:** M. Shidatsu, C. Done  
**arXiv:** [1906.02469](https://arxiv.org/abs/1906.02469)  
**Date:** 2019-06-06  
**Summary page:** https://www.summarizepaper.com/en/paper/1906.02469v3/

## Key points

- Study focuses on high inclination black hole X-ray binaries and their absorption features
- Lines believed to come from disk winds, but launching mechanism debated
- Authors use thermal-radiative wind models to predict wind properties based on RXTE monitoring data
- Detailed photo-ionized absorption features simulated using Chandra spectra
- Thermal wind model reproduces observed lines in high/soft state, predicts disappearance in low/hard state
- Strong features predicted in very high state not seen in data, self-shielding by inner disk atmosphere considered
- Evolution of wind properties during outbursts in H 1743-322 explained by thermal winds without magnetic driving
- Findings contribute to understanding disk winds in black hole X-ray binaries and launching mechanisms debate.

## Summary

This study focuses on the analysis of high inclination black hole X-ray binaries and their absorption features observed in their spectra. These lines are believed to originate from disk winds, but the mechanism behind their launching is still a topic of debate. To investigate this, the authors use analytic thermal-radiative wind models to predict various properties of the wind based on the broadband continuum shape and luminosity obtained from RXTE monitoring. They then simulate detailed photo-ionized absorption features expected during different states (low/hard, high/soft and very high) using Chandra high-resolution spectra. The results show that the thermal wind model successfully reproduces the observed lines in the high/soft state and predicts their disappearance in the low/hard state. However, it also predicts strong features in the very high state that are not seen in the data. To reconcile this discrepancy, self-shielding by the irradiated inner disk atmosphere is taken into account. Overall, this study demonstrates that evolution of observed wind properties during outbursts in H 1743-322 can be explained by thermal winds without requiring magnetic driving. These findings provide valuable insights into understanding disk winds in black hole X-ray binaries and contribute to ongoing debates about their launching mechanisms.