Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-30T16:08:22.089Z Has data issue: false hasContentIssue false
  • English
  • Français

Electron-Cyclotron Maser Emission and Propagation in Solar Microwave Spike Bursts

Published online by Cambridge University Press:  25 April 2016

P. A. Robinson  and
Z. Kuncic
P. A. Robinson
Affiliation:
School of Physics and Research Center for Theoretical Astrophysics, University of Sydney, NSW 2006
Z. Kuncic
Affiliation:
School of Physics and Research Center for Theoretical Astrophysics, University of Sydney, NSW 2006
Get access Rights & Permissions [Opens in a new window]

Abstract

An improved model of the generation and propagation of cyclotron-maser radiation in flaring loops is discussed, which incorporates competition between driving of the maser instability and maser-induced relaxation of the unstable plasma. This model enables previous large discrepancies between the build-up, relaxation, and observed timescales to be resolved for solar microwave spike bursts. Also, it implies that emission via fundamental o-mode and second-harmonic x-mode instabilities can compete more effectively against fundamental x-mode emission than has previously been thought. Propagation of the radiation to the observer is discussed both theoretically and with reference to ray tracing calculations and it is shown that the observed levels of MHD waves in the corona make it significantly easier for the radiation to escape than in the unperturbed case. In the absence of nonlinear processes or mode conversion we argue that the escaping radiation is generated by either fundamental o-mode or second-harmonic x-mode instabilities.

Type
Solar and Solar System
Information
Publications of the Astronomical Society of Australia , Volume 10 , Issue 1 , 1992 , pp. 61 - 63
Copyright
Copyright © Astronomical Society of Australia 1992

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Aschwanden, M. J., 1987, Solar Phys., 111, 113.Google Scholar
Aschwanden, M. J., 1990, Astron. Astrophys., 237, 512.Google Scholar
Benz, A. O., 1986, Solar Phys., 104, 99.Google Scholar
Crannell, C. J., Duik, G. A., Kosugi, T. and Magun, A., 1988, Solar Phys., 118, 155.Google Scholar
Droge, F, 1977, Astron. Astrophys., 57, 285.Google Scholar
Gudel, M. and Zlobec, P., 1991, Astron. Astrophys., 245, 299.Google Scholar
Hewitt, R. G., Melrose, D. B. and Ronnmark, K. G., 1982, Ausi. J. Phys., 35, 447.Google Scholar
Holman, G. D., Eichler, D. and Kundu, M. R., 1980, in IAUSymp. 86, Radio Physics of the Sun, Kundu, M. R. and Gergely, T. E. (eds), Reidel, Dordrecht, p. 57.Google Scholar
McKean, M. E., Winglee, R. M. and Dulk, G. A., 1989, Solar Phys., 122, 53.Google Scholar
Melrose, D. B. and Dulk, G. A., 1982a, Astrophys. J., 259, L41.CrossRefGoogle Scholar
Melrose, D. B. and Dulk, G. A., 1982b, Astrophys. J., 259, 844.Google Scholar
Melrose, D. B. and Dulk, G. A., 1984, Astrophys. J., 282, 308.Google Scholar
Melrose, D. B., Hewitt, R. G. and Ronnmark, K. G., 1982, J. Geophys. Res., 87, 5140.Google Scholar
Robinson, P. A., 1989, Astrophys. J., 341, L99.Google Scholar
Robinson, P. A., 1991a, Solar Phys., 134, 299.Google Scholar
Robinson, P. A., 1991b, Solar Phys., 136, 343.Google Scholar
Slottje, C, 1978, Nature, 275, 520.Google Scholar
Winglee, R. M., Dulk, G. A. and Pritchett, P. L., 1988, Astrophys. J., 328, 809.Google Scholar
Wu, C. S. and Lee, L. C, 1979, Astrophys. J., 230, 691.Google Scholar