Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-22T23:32:42.160Z Has data issue: false hasContentIssue false
  • English
  • Français

Metal-poor Wolf-Rayet star enriching the ISM by nitrogen in the galaxy NGC 4068

Published online by Cambridge University Press:  29 August 2024

Anastasiya Yarovova Open the ORCID record for Anastasiya Yarovova [Opens in a new window] ,
Oleg Egorov ,
Alexei Moiseev  and
Olga Maryeva
Anastasiya Yarovova*
Affiliation:
Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetsky pr. 13, Moscow 119234, Russia
Oleg Egorov
Affiliation:
Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetsky pr. 13, Moscow 119234, Russia Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstraß e 12-14, D-69120 Heidelberg, Germany
Alexei Moiseev
Affiliation:
Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetsky pr. 13, Moscow 119234, Russia Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz 369167, Russia
Olga Maryeva
Affiliation:
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz 369167, Russia Astronomical Institute of the Czech Academy of Sciences, Fričova 298, 25165 Ondřejov, Czech Republic
*
email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We discovered a nebula in the low-metallicity (Z=0.1 ) nearby ( Mpc) dwarf galaxy NGC 4068, which reveals broad Hα line profile and unusual emission line fluxes in its spectrum. The object also shows significant nitrogen overabundance, not typical for metal-poor environment. We assumed that the nebula could be ionized by an evolved massive star with , Wolf-Rayet or Blue Supergiant, and built models of the nebula using Cloudy and CMFGEN codes. Our models successfully reproduce the optical emission spectrum of the object, including the peculiar [SII]/[NII] ratio and the presence of the HeII λ4686 line.

Keywords

stars: Wolf-Rayetstars: mass lossISM: abundances
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 513 - 514
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Afanasiev, V. L., & Moiseev, A. V. 2011, Baltic Astronomy, 20, 363 Google Scholar
Ferland, G. J., et al. 2017, RMxAA, 53, 385 Google Scholar
Georgy, C., et al. 2013, A&A, 558, A103 Google Scholar
Grasha, K., Roy, A., Sutherland, R. S., & Kewley, L. J. 2021, arXiv e-prints, arXiv:2101.01197Google Scholar
Hillier, D. J., & Miller, D. L. 1998, ApJ, 496, 407 Google Scholar