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Intermediate degree solar oscillations

Published online by Cambridge University Press:  03 August 2017

T. L. Duvall Jr. ,
J. W. Harvey  and
M. A. Pomerantz
T. L. Duvall Jr.
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771 U.S.A.
J. W. Harvey
Affiliation:
National Solar Observatory, National Optical Astronomy Observatories†, P.O. Box 26732 Tucson, AZ 85726 U.S.A.
M. A. Pomerantz
Affiliation:
Bartol Research Foundation, University of Delaware, Newark, DE 19711 U.S.A.

Abstract

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Spectra of solar intensity oscillations in the degree range ℓ = 20–98 were obtained with a 92% duty cycle over a 50 hour period from the geographic South Pole. After correction for solar rotation, the spectra have been averaged over azimuthal order m and fit with Lorentzian functions to provide values of background noise, amplitude, frequency and line width for 636 oscillation modes. The background noise is nearly independent of frequency in the range containing strong p-modes. The amplitude envelope shows little dependence on ℓ value and a frequency dependence similar to that of Doppler oscillations but shifted to higher frequency. Line widths increase at higher frequency and at higher ℓ values.

Type
Chapter 1: Observations of Solar Oscillations
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 37 - 40
Copyright
Copyright © Reidel 1988 

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