Rotation of the coronal magnetic field

Journal Article · Wed Jul 01 04:00:00 EDT 1987 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/165379· OSTI ID:6120190

Hoeksema, J T; Scherrer, P H

The coronal magnetic field rotates differently than the photosphere. The field configuration of the corona can be calculated from the observed photosphpere field using a potential field model. Correlation of the field patterns at different latitudes with a lag near one solar rotation shows much less differential rotation than observed in the photospheric field; however, the peak is very broad and determines the rotation rate rather poorly. Consideration of longer lags reveals a more complex rotational structure and indicates different rotation rates in the Northern and Southern Hemispheres. Spectral analysis of the equatorial dipole component of the coronal field reveals an organization into just a few discrete rotation frequencies which are apparently present simultaneously. Spectral analysis of the field at different latitudes shows that the frequencies are present simultaneously. Spectra analysis of the field at different latitudes shows that the frequencies are present simultaneously, but in different hemispheres, and that the Southern Hemisphere fields rotate more slowly than those in the north in solar cycle 21. 32 references.

• Research Organization: Stanford Univ., CA
• OSTI ID: 6120190
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 318; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
EARTH PLANET
MAGNETIC FIELD CONFIGURATIONS
MAGNETIC FIELDS
MOTION
NORTHERN HEMISPHERE
PHOTOSPHERE
PLANETS
ROTATION
SOLAR ATMOSPHERE
SOLAR CORONA
SOUTHERN HEMISPHERE
STELLAR ATMOSPHERES
STELLAR CORONAE