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Open Astronomy

formerly Baltic Astronomy

Editor-in-Chief: Barbuy, Beatriz


IMPACT FACTOR 2018: 0.350

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2543-6376
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Volume 24, Issue 2

Issues

Velocity Dispersion of Ionized Gas and Multiple Supernova Explosions

E. O. Vasiliev
  • Institute of Physics, Southern Federal University, Stachki Ave. 194, Rostov-on-Don, 344090 Russian Federation
  • Department of Physics, Southern Federal University, Sorge Str. 5, Rostov-on-Don, 344090 Russian Federation
  • Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, Karachaevo-Cherkesskaya Republic, 369167 Russian Federation
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  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ A. V. Moiseev
  • Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, Karachaevo-Cherkesskaya Republic, 369167 Russian Federation
  • Sternberg Astronomical Institute, Moscow M. V. Lomonosov State University, Universitetskij pr. 13, 119992 Moscow, Russian Federation
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ Yu. A. Shchekinov
  • Department of Physics, Southern Federal University, Sorge Str. 5, Rostov-on-Don, 344090 Russian Federation
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
Published Online: 2017-02-18 | DOI: https://doi.org/10.1515/astro-2017-0222

Abstract

We use 3D numerical simulations to study the evolution of the Hα intensity and velocity dispersion for single and multiple supernova (SN) explosions. We find that the IHα– σ diagram obtained for simulated gas flows is similar in shape to that observed in dwarf galaxies. We conclude that colliding SN shells with significant difference in age are responsible for high velocity dispersion that reaches up to ≳ 100 km s−1. Such a high velocity dispersion could be hardly obtained for a single SN remnant. Peaks of velocity dispersion in the IHα– σ diagram may correspond to several isolated or merged SN remnants with moderately different ages. Degrading the spatial resolution in the Hα intensity and velocity dispersion maps makes the simulated IHα– σ diagrams close to those observed in dwarf galaxies not only in shape, but also quantitatively.

Keywords: galaxies: ISM; ISM: bubbles; ISM: supernova remnants; ISM: kinematics and dynamics; shock waves; methods: numerical

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About the article

Received: 2015-03-25

Accepted: 2015-04-20

Published Online: 2017-02-18

Published in Print: 2015-06-01


Citation Information: Open Astronomy, Volume 24, Issue 2, Pages 213–220, ISSN (Online) 2543-6376, DOI: https://doi.org/10.1515/astro-2017-0222.

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© 2015 E. O. Vasiliev et al., published by De Gruyter Open. This work is licensed under the Creative Commons Attribution-NonCommercial-NoDerivatives 3.0 License. BY-NC-ND 3.0

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