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Title: Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum

Abstract

We present model fits to the X-ray line spectrum of the well-known high-mass X-ray binary Cyg X-3. The primary observational data set is a spectrum taken with the Chandra X-ray Observatory High Energy Transmission Grating in 2006, though we compare it to all the other observations of this source taken so far by this instrument. We show that the density must be ≥10 12 cm –3 in the region responsible for most of the emission. We discuss the influence of the dust scattering halo on the broadband spectrum, and we argue that dust scattering and extinction is not the most likely origin for the narrow feature seen near the Si K edge. We identify the features of a wind in the profiles of the strong resonance lines and show that the wind is more apparent in the lines from the lighter elements. We argue that this wind is most likely associated with the companion star. We show that the intensities of most lines can be fitted, crudely, by a single-component photoionized model. Yet, the iron K lines do not fit with this model. We show that the iron K line variability as a function of orbital phase is different frommore » the lower-energy lines, which indicates that the lines arise in physically distinct regions. We discuss the interpretation of these results in the context of what is known about the system and similar systems.« less

Authors:
ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [3];  [4];  [5];  [6];  [7];  [8];  [9];  [10];  [5]
  1. NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States)
  2. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
  3. Univ. of Turku (Finland)
  4. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
  5. Univ. of Michigan, Ann Arbor, MI (United States)
  6. Columbia Univ., New York, NY (United States)
  7. Mullard Radio Astronomy Observatory, Cambridge (United Kingdom)
  8. Univ. of Pennsylvania, Philadelphia, PA (United States)
  9. Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States)
  10. Special Astrophysical Observatory RAS (Russia); Kazan Federal Univ., Kazan (Russia)
Publication Date:
Research Org.:
Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC); USDOE National Nuclear Security Administration (NNSA); National Aeronautic and Space Administration (NASA)
OSTI Identifier:
1545280
Grant/Contract Number:  
AC52-07NA27344; 14-ATP14-0022
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 874; Journal Issue: 1; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
stars: black holes; stars: winds, outflows; X-rays: binaries

Citation Formats

Kallman, T., McCollough, M., Koljonen, K., Liedahl, D., Miller, J., Paerels, F., Pooley, G., Sako, M., Schulz, N., Trushkin, S., and Corrales, L. Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum. United States: N. p., 2019. Web. doi:10.3847/1538-4357/ab09f8.
Kallman, T., McCollough, M., Koljonen, K., Liedahl, D., Miller, J., Paerels, F., Pooley, G., Sako, M., Schulz, N., Trushkin, S., & Corrales, L. Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum. United States. doi:10.3847/1538-4357/ab09f8.
Kallman, T., McCollough, M., Koljonen, K., Liedahl, D., Miller, J., Paerels, F., Pooley, G., Sako, M., Schulz, N., Trushkin, S., and Corrales, L. Thu . "Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum". United States. doi:10.3847/1538-4357/ab09f8. https://www.osti.gov/servlets/purl/1545280.
@article{osti_1545280,
title = {Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum},
author = {Kallman, T. and McCollough, M. and Koljonen, K. and Liedahl, D. and Miller, J. and Paerels, F. and Pooley, G. and Sako, M. and Schulz, N. and Trushkin, S. and Corrales, L.},
abstractNote = {We present model fits to the X-ray line spectrum of the well-known high-mass X-ray binary Cyg X-3. The primary observational data set is a spectrum taken with the Chandra X-ray Observatory High Energy Transmission Grating in 2006, though we compare it to all the other observations of this source taken so far by this instrument. We show that the density must be ≥1012 cm–3 in the region responsible for most of the emission. We discuss the influence of the dust scattering halo on the broadband spectrum, and we argue that dust scattering and extinction is not the most likely origin for the narrow feature seen near the Si K edge. We identify the features of a wind in the profiles of the strong resonance lines and show that the wind is more apparent in the lines from the lighter elements. We argue that this wind is most likely associated with the companion star. We show that the intensities of most lines can be fitted, crudely, by a single-component photoionized model. Yet, the iron K lines do not fit with this model. We show that the iron K line variability as a function of orbital phase is different from the lower-energy lines, which indicates that the lines arise in physically distinct regions. We discuss the interpretation of these results in the context of what is known about the system and similar systems.},
doi = {10.3847/1538-4357/ab09f8},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 874,
place = {United States},
year = {2019},
month = {3}
}

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