Hostname: page-component-78c5997874-m6dg7 Total loading time: 0 Render date: 2024-11-07T23:06:34.789Z Has data issue: false hasContentIssue false
  • English
  • Français

Cosmic-ray driven dynamo in the medium of irregular galaxy

Published online by Cambridge University Press:  01 November 2008

Hubert Siejkowski ,
Marian Soida ,
Katarzyna Otmianowska-Mazur ,
Michał Hanasz  and
Dominik Bomans
Hubert Siejkowski
Affiliation:
Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Kraków, Poland email: [email protected]
Marian Soida
Affiliation:
Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Kraków, Poland email: [email protected]
Katarzyna Otmianowska-Mazur
Affiliation:
Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Kraków, Poland email: [email protected]
Michał Hanasz
Affiliation:
Toruń Centre for Astronomy, Nicolaus Copernicus University, 87-148 Toruń/Piwnice, Poland
Dominik Bomans
Affiliation:
Astronomical Institute of Ruhr-University Bochum, Univeristätsstr. 150/NA7, D-44780 Bochum, Germany
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 investigate the cosmic ray driven dynamo in the interstellar medium of irregular galaxy. The observations (Chyży et al. 2000, 2003) show that the magnetic field in irregular galaxies is present and its value reaches the same level as in spiral galaxies. However the conditions in the medium of irregular galaxy are very unfavorable for amplification the magnetic field due to slow rotation and low shearing rate.

In this work we present numerical model of the interstellar medium in irregular galaxies. The model includes magnetohydrodynamical dynamo driven by cosmic rays in the interstellar medium provided by random supernova explosions. We describe models characterized by different shear and rotation. We find that even slow galactic rotation with low shearing rate gives amplification of the magnetic field. Simulations have shown that high amount of the magnetic energy flow out off the simulation region becoming an efficient source of intergalactic magnetic fields.

Keywords

MHD – methods: numerical – galaxies: magnetic fields – galaxies: irregular
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 557 - 558
Copyright
Copyright © International Astronomical Union 2009

References

Chyży, K. T., Beck, R., Kohle, S., Klein, U., & Urbanik, M. 2000, A&A 355, 128Google Scholar
Chyży, K. T., Knapik, J., Bomans, D. J., Klein, U., Beck, R., Soida, M., & Urbanik, M. 2003, A&A 405, 513Google Scholar
Ferrière, K. 1998, ApJ 497, 759CrossRefGoogle Scholar
Hanasz, M., Kowal, G., Otmianowska-Mazur, K., & Lesch, H. 2004, ApJ 605, L33CrossRefGoogle Scholar
Hanasz, M., Kowal, G., Otmianowska-Mazur, K., & Lesch, H. 2006, AN 327, 469Google Scholar
Hawley, J. F., Gammie, C. F., & Balbus, S. A. 1995, ApJ 440, 742CrossRefGoogle Scholar
Kronberg, P. P., Lesch, H., & Hopp, U. 1999, ApJ 551, 56CrossRefGoogle Scholar