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Inferring the chromospheric magnetic topology through waves

Published online by Cambridge University Press:  01 September 2007

S. S. Hasan ,
O. Steiner  and
A. van Ballegooijen
S. S. Hasan
Affiliation:
Indian Institute of Astrophysics, Bangalore, India, email: hasan@iiap.res.in
O. Steiner
Affiliation:
Kiepenheuer Institut für Sonnenphysik, Freiburg, Germany
A. van Ballegooijen
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, U.S.A.
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Abstract

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The aim of this work is to examine the hypothesis that the wave propagation time in the solar atmosphere can be used to infer the magnetic topography in the chromosphere as suggested by Finsterle et al. (2004). We do this by using an extension of our earlier 2-D MHD work on the interaction of acoustic waves with a flux sheet. It is well known that these waves undergo mode transformation due to the presence of a magnetic field which is particularly effective at the surface of equipartition between the magnetic and thermal energy density, the β = 1 surface. This transformation depends sensitively on the angle between the wave vector and the local field direction. At the β = 1 interface, the wave that enters the flux sheet, (essentially the fast mode) has a higher phase speed than the incident acoustic wave. A time correlation between wave motions in the non-magnetic and magnetic regions could therefore provide a powerful diagnostic for mapping the magnetic field in the chromospheric network.

Keywords

wavesMHDSun: atmosphereSun: photosphereSun: chromosphereSun: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S247: Waves & Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology , September 2007 , pp. 78 - 81
Copyright
Copyright © International Astronomical Union 2008

References

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