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Velocity Dispersion and H\(\boldsymbol{\alpha}\)-emission of Ionized Gas in Star-forming Regions

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Abstract

To understand the nature of gas flows in star-forming regions of nearby galaxies, the relationship between the surface brightness values in the H\(\alpha\) line and the velocity dispersion of ionized gas, known as the ‘‘surface brightness–velocity dispersion’’ diagram, is often used. Based on three-dimensional gas-dynamic calculations, we examined the evolution of synthetic diagrams for supershells formed as a result of multiple supernova explosions in a star cluster located in the galactic disk. Based on the results of a study of changes in the shape and structure of the diagram depending on the gas density, its metallicity, and the disk scale height, it is possible to identify ranges of values in the diagram that are characteristic of young bubbles developing in dense or rarefied gas at large heights above the plane of the disk. We found that the structure of the diagram depends on the age of the supershells and the physical properties of the gas in the disk. For nearby dwarf galaxies, the structure of the observed ‘‘surface brightness–velocity dispersion’’ diagrams can only be explained by describing the dynamics of bubbles formed by multiple SN explosions in small star clusters of different ages.

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Fig. 1
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Notes

  1. The intensity from the unperturbed part of the disk presents a uniform background with rather low intensity values, as shown by the white part of the color scale in panel (a). Vertical velocities in the undisturbed disk are practically absent, their dispersion is close to zero (see panel (b)).

  2. The cross-shaped structures in the central part are a manifestation of the well-known numerical instability from recent SN explosions (Quirk, 1994); at the considered moment in time, their relative contribution to the total surface is several percent, and in the future it will rapidly decrease.

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ACKNOWLEDGEMENTS

The authors are grateful to O.V. Egorov and A.V. Moiseev for numerous discussions and valuable clarifications.

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This work was supported by ongoing institutional funding.

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Authors and Affiliations

  1. Lebedev Physical Institute, Russian Academy of Sciences, 117997, Moscow, Russia

    E. O. Vasiliev

  2. Raman Research Institute, 560080, Sadashiva Nagar, Bangalore, India

    Yu. A. Shchekinov

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Correspondence to E. O. Vasiliev.

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Vasiliev, E.O., Shchekinov, Y.A. Velocity Dispersion and H\(\boldsymbol{\alpha}\)-emission of Ionized Gas in Star-forming Regions. Astrophys. Bull. 79, 60–70 (2024). https://doi.org/10.1134/S1990341323600242

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