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Resonance Line Formation in Moving Gas Flows with High Porosity

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Astrophysics Aims and scope

The formation of resonance lines in gas flows generated by interactions of circumstellar gas with a star’s magnetosphere is examined. An effective method is proposed for calculating these lines when the magnetospheric wind is highly porous. The resonance sodium lines observed in the spectrum of UX Ori type star RZ Psc are modelled as an example. It is shown that the narrow absorptions observed in the short wavelength wings of these lines can be formed by scattering of the star’s radiation in two gas jets that are semitransparent at the line frequencies when they cross the line of sight.

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Authors and Affiliations

  1. St. Petersburg State University, St. Petersburg, Russia

    S. G. Shulman

  2. Main (Pulkovo) Astronomical Observatory, Russian Academy of Sciences, St. Petersburg, Russia

    S. G. Shulman

Authors
  1. S. G. Shulman
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Correspondence to S. G. Shulman.

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Translated from Astrofizika, Vol. 60, No. 2, pp. 205-218 (May 2017).

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Shulman, S.G. Resonance Line Formation in Moving Gas Flows with High Porosity. Astrophysics 60, 188–199 (2017). https://doi.org/10.1007/s10511-017-9474-9

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  • DOI: https://doi.org/10.1007/s10511-017-9474-9

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