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On the Formation of Line Profiles of Solar P Modes

Published online by Cambridge University Press:  08 February 2017

I.W. Roxburgh  and
S.V. Vorontsov
I.W. Roxburgh
Affiliation:
Astronomy Unit, Queen Mary and Westfield College Mile End Road, London E1 4NS, UK
S.V. Vorontsov
Affiliation:
Astronomy Unit, Queen Mary and Westfield College Mile End Road, London E1 4NS, UK Institute of Physics of the Earth, B. Gruzinskaya 10, Moscow 123810, Russia

Abstract

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We address the problem of the opposite asymmetry of low-frequency p-mode line profiles observed in intensity and velocity measurements (Duvall et al. 1993). We use a simple model to illustrate that this feature can be explained by including a contribution from the stochastic excitation velocity field to the non-resonant background in the doppler measurements.

Type
IV. Solar Small-Scale Structure
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 229 - 230
Copyright
Copyright © Kluwer 1998 

References

Duvall, T. L. Jr., Jefferies, S. M., Harvey, J. W., Osaki, Y. and Pomerantz, M. A. (1993), ApJ 410, p.829 Google Scholar
Roxburgh, I. W. and Vorontsov, S. V. (1995), Mon. Not. R. astr. Soc. 272, p.850 Google Scholar
Roxburgh, I. W. and Vorontsov, S. V. (1997), Mon. Not. R. astr. Soc., in press Google Scholar