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Optical Characteristics of a Magnetocentrifugal Disk Wind in the Visual, Ultraviolet, and X-ray Spectral Ranges

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Abstract

The optical characteristics of a magnetocentrifugal disk wind from T Tauri stars that we calculated based on the MHD models of Safier (1993a, 1993b) are presented. For an outflow rate in the range \(10^{-10}{-}10^{-7} M_{\odot}\) yr\({}^{-1}\) we calculated the critical angles at which the wind becomes opaque in the optical, ultraviolet, and X-ray parts of the spectrum. The illumination of the outer regions of protoplanetary disks involved in creating a photoevaporating wind by the star and the conditions for observing young stars in different wavelength ranges depend on these angles. We show that at the early evolutionary stages of T Tauri stars the disk wind is capable of completely shielding the star and preventing the direct illumination of the peripheral disk regions in both optical and X-ray ranges. By absorbing the bulk of the stellar radiation, the disk wind itself becomes a radiation source capable of heating the disk. We show that at an outflow rate \({\geq}10^{-9} M_{\odot}\) yr\({}^{-1}\) the fraction of the radiation absorbed by the wind can reach \(60\%\). Hot accretion spots can contribute significantly to the absorbed radiation. This allows the disk wind to be considered as an important infrared radiation source of T Tauri stars.

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Notes

  1. Comparison with the results of MHD calculations by Romanova et al. (2009) shows that the wind in Safier’s models turns out to be flatter at the initial acceleration phases than the canonical wind in the models of the above authors.

  2. In the models of Safier (1993a, 1993b) this temperature range corresponds to the densest disk wind region in which the gas acceleration occurs.

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ACKNOWLEDGMENTS

We thank the anonymous referee for the useful remarks.

Funding

This work was supported by ongoing institutional funding. No additional grants to carry out or direct this particular research were obtained.

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Authors and Affiliations

  1. St. Petersburg State University, 199034, St. Petersburg, Russia

    M. A. Albrant & V. P. Grinin

  2. Pulkovo Astronomical Observatory, Russian Academy of Sciences, 196140, St. Petersburg, Russia

    V. P. Grinin & T. A. Ermolaeva

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  1. M. A. Albrant
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  2. V. P. Grinin
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  3. T. A. Ermolaeva
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Correspondence to V. P. Grinin.

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Translated by V. Astakhov

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Albrant, M.A., Grinin, V.P. & Ermolaeva, T.A. Optical Characteristics of a Magnetocentrifugal Disk Wind in the Visual, Ultraviolet, and X-ray Spectral Ranges. Astron. Lett. 50, 269–278 (2024). https://doi.org/10.1134/S1063773724700099

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