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The Nature of the Emission Spectrum of NGC 7793 P13: Testing the Supercritical Accretion Disk Wind Model

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Abstract

The optical spectra of ultraluminous X-ray sources (ULXs) show signs of powerful outflows of matter. These outflows are responsible for the formation of a significant portion of optical and ultraviolet emission in ULXs and can either be stellar winds of the donor stars or optically thick outflows (winds) from the surface of supercritical accretion disks. In the latter scenario the outflows are still expected to be similar to stellar winds of massive stars, which allows one to use the same methods for their study based on a comparison of the observed spectra with those simulated within the framework of non-LTE extended atmosphere models. In this paper, we simulate the optical spectrum of the ultraluminous X-ray pulsar NGC 7793 P13, assuming that its emission part is produced in the wind of the supercritical accretion disk. The estimated mass loss rate is about \(1.4\times 10^{-5}M_{\odot}\) yr\({}^{-1}\). We consider the positive and negative aspects of the model and also discuss the applicability of the concept of supercritical disk winds to NGC 7793 P13 and to another well-known ultraluminous X-ray pulsar, NGC 300 ULX-1.

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Notes

  1. Note that the red spectra of NGC 7793 P13 have not been published before.

  2. By photosphere we mean the surface corresponding to the Rosseland optical depth \(\tau_{\textrm{Ross}}=2/3\).

  3. The photospheric radius and luminosity of the supercritical disk wind were already determined at the first step, and considered fixed at this stage.

  4. Hereinafter by turbulent velocity we understand the microturbulent velocity.

  5. The name of the approximation is abbreviated by the first letters of the names of its authors.

  6. The photometric period measured from the data of long term Swift/UVOT monitoring of the object is somewhat shorter than the orbital period, \(P_{\textrm{orb}}=64.86\pm 0.19\) days (Fürst et al., 2021), and probably arises due to the superorbital modulation of the orbital period.

  7. The optical depth values for the wind depend on the parameters of the wind velocity variation law in the vicinity of the supercritical disk. For example, for a virial wind, according to relation (30) in Poutanen et al. (2007), for the wind matter outflow rates equal to about \(300\,\dot{M}_{\textrm{Edd}}\), the disk-plane optical depth of the wind would be about 100.

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ACKNOWLEDGMENTS

The authors are grateful to the anonymous referees for their valuable comments which allowed us to significantly improve the text of the paper. This work is based on observations collected by the European Organization for Astronomical Research in the Southern Hemisphere within the framework of the 084.D-0881(A) program.

Funding

This work was supported by the Russian science foundation (project no. 21-72-10167 ‘‘Ultraluminous X-ray sources: wind and donors’’).

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Authors and Affiliations

  1. Special Astrophysical Observatory, Russian Academy of Sciences, 369167, Nizhnii Arkhyz, Russia

    A. Kostenkov, A. Vinokurov, K. Atapin & Y. Solovyeva

  2. Sternberg Astronomical Institute, Moscow State University, 119234, Moscow, Russia

    K. Atapin

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  1. A. Kostenkov
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  2. A. Vinokurov
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Kostenkov, A., Vinokurov, A., Atapin, K. et al. The Nature of the Emission Spectrum of NGC 7793 P13: Testing the Supercritical Accretion Disk Wind Model. Astrophys. Bull. 78, 395–411 (2023). https://doi.org/10.1134/S1990341323700086

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