Asymmetry and Frequencies of Low-Degree p-Modes and the Structure of the Sun's Core

Details Asymmetry and Frequencies of Low-Degree p-Modes and the Structure of the Sun's Core Asymmetry and Frequencies of Low-Degree p-Modes and the Structure of the Sun's Core

Oct 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...506l.147t&link_type=abstract

The Astrophysical Journal, Volume 506, Issue 2, pp. L147-L150.

Astronomy and Astrophysics

Astronomy

57

Methods: Data Analysis, Sun: Interior, Sun: Oscillations

Scientific paper

An accurate determination of the frequencies of low-degree solar p-modes is an important task of helioseismology. Using 679 days of solar oscillation data observed in Doppler velocity and continuum intensity from two Solar and Heliospheric Observatory instruments (the Michelson Doppler Imager and the SunPhotoMeter), we show that fitting the spectra with Lorentzian profiles leads to systematic differences between intensity and velocity frequencies as large as 0.1 muHz for angular degrees l=0, 1, and 2 because of the opposite asymmetry between intensity and velocity. We use a physics-based asymmetrical line shape to fit p-mode lines, and we demonstrate that their asymmetry is statistically significant and that frequency differences are considerably reduced. These measurements provide more accurate estimates of the solar eigenfrequencies. We discuss inferences of the structure of the solar core.

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