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MHD simulations of ram pressure stripping of disk galaxies

Published online by Cambridge University Press:  17 August 2016

Mariana Ramos-Martínez  and
Gilberto C. Gómez
Mariana Ramos-Martínez
Affiliation:
Instituto de Radioastronomía y Astrofísica, UNAM, Apartado Postal 3-72, 58089 Morelia, México email: [email protected]
Gilberto C. Gómez
Affiliation:
Instituto de Radioastronomía y Astrofísica, UNAM, Apartado Postal 3-72, 58089 Morelia, México email: [email protected]
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Abstract

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The removal of ISM of disk galaxies through ram pressure stripping (RPS) has been extensively studied in numerous simulations (see Roediger 2009 and references therein). The models show that RPS has a significant impact on galaxy evolution (truncation of the ISM will lead to a decrease in star formation and a change in galaxy color). Nevertheless, the role of magnetic fields (MFs) on the dynamics of the gas in this process has not been sufficiently studied, although the influence of the MFs on the large scale structure is well established. This motivated us to perform a 3D MHD simulation of a disk galaxy with an isothermal, non-self gravitating and magnetized gaseous disk in equilibrium with a galaxy potential (Allen & Santillán, 1991). We model RPS on the galactic disk under the wind-tunnel approximation with the use of the RAMSES code (Teyssier, 2002) in order to understand the effects of MFs in RPS.

Keywords

galaxies: evolutionintergalactic mediumgalaxies: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S319: Galaxies at High Redshift and Their Evolution Over Cosmic Time , August 2015 , pp. 143
Copyright
Copyright © International Astronomical Union 2016 

References

Allen, C. & Santillán, A. 1991, Rev. Mexicana AyA, 22, 255 Google Scholar
Gómez, G. C. & Cox, D. 2002, ApJ, 580, 235 CrossRefGoogle Scholar
Roediger, E. 2009, AN, 330, 888 Google Scholar
Teyssier, R., 2002, A&A, 385, 337 Google Scholar