Hostname: page-component-78c5997874-mlc7c Total loading time: 0 Render date: 2024-11-16T19:24:46.211Z Has data issue: false hasContentIssue false
  • English
  • Français

Three dimensional simulations of Hall magnetohydrodynamics

Published online by Cambridge University Press:  08 June 2011

Daniel O. Gómez
Daniel O. Gómez*
Affiliation:
Instituto de Astronomía y Física del Espacio, C.C. 67 - Suc. 28, (1428) Buenos Aires, Argentina email: [email protected] Departamento de Física, Facultad de Ciencias Exactas y Naturales (UBA), Ciudad Universitaria, (1428) Buenos Aires, Argentina
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.

Turbulent flows take place in a large variety of astrophysical objects, and often times are the source of dynamo generated magnetic fields. Much of the progress in our understanding of dynamo mechanisms, has been made within the theoretical framework of magnetohydrodynamics (MHD). However, for sufficiently diffuse media, the Hall effect eventually becomes non-negligible.

We present results from simulations of the Hall-MHD equations. The simulations are performed with a pseudospectral code to achieve exponentially fast convergence. We study the role of the Hall effect in the dynamo efficiency for different values of the Hall parameter.

Keywords

ISM: magnetic fieldsMHDturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 433 - 436
Copyright
Copyright © International Astronomical Union 2011

References

Balbus, S. A. & Terquem, C. 2001, ApJ, 552, 235.CrossRefGoogle Scholar
Gómez, D. O., Mininni, P. D., & Dmitruk, P. 2010, Phys. Rev. E, 82, 036406.Google Scholar
Gómez, D. O., Dmitruk, P., & Mahajan, S. M. 2008, Phys. Plasmas, 15, 102303.Google Scholar
Gómez, D. O. & Mininni, P. D. 2004, Nonlin. Proc. Geophys., 11, 619.Google Scholar
Haugen, N. E. L., Brandenburg, A., & Dobler, W. 2004, Phys. Rev. E 70, 016308.CrossRefGoogle Scholar
Kazantsev, A. P. 1968, Sov. Phys. JETP 26, 1031.Google Scholar
Ma, Z. & Bhattacharjee, A. 2001, J. Geophys. Res., 106, 3773.CrossRefGoogle Scholar
Martín, L., Dmitruk, P., & Gómez, D. O. 2010, Phys. Plasmas, 17, 112304.Google Scholar
Mininni, P. D., Gómez, D. O., & Mahajan, S. M. 2005, ApJ, 619, 1019.Google Scholar
Mininni, P. D., Gómez, D. O., & Mahajan, S. M. 2003, ApJ, 587, 472.CrossRefGoogle Scholar
Mininni, P. D., Gómez, D. O., & Mahajan, S. M. 2002, ApJ, 567, L81.CrossRefGoogle Scholar
Morales, L., Gómez, D. O., Dasso, S., & Mininni, P. D. 2006, Adv. Space Res., 37, 1287.Google Scholar
Morales, L., Dasso, S., Gómez, D. O., & Mininni, P. D. 2005, J. Atm. Sci. & Sol. Terr. Phys., 67, 1865.Google Scholar
Mozer, F., Bale, S., & Phan, T. D. 2002, Phys. Rev. Lett., 89, 015002.CrossRefGoogle Scholar
Sano, T. & Stone, J. M. 2002, ApJ, 570, 314.CrossRefGoogle Scholar
Wardle, M. & Ng, C. 1999, Mon. Not. R. A. S., 303, 239.CrossRefGoogle Scholar
Yakovlev, D. G. & Urpin, V. A. 1980, Astr. Zh., 57, 526.Google Scholar