Studies of solar magnetic fields
โ Scribed by Robert Howard
- Publisher
- Springer
- Year
- 1977
- Tongue
- English
- Weight
- 299 KB
- Volume
- 52
- Category
- Article
- ISSN
- 0038-0938
No coin nor oath required. For personal study only.
โฆ Synopsis
An estimate of the average magnetic field strength at the poles of the Sun from Mount Wilson measurements is made by comparing low latitude magnetic measurements in the same regions made near the center of the disk and near the limb. There is still some uncertainty because the orientation angle of the field lines in the meridional plane is unknown, but the most likely possibility is that the true average field strengths are about twice the measured values (0-2 G), with an absolute upper limit on the underestimation of the field strengths of about a factor 5. The measurements refer to latitudes below about 80 ~ .
๐ SIMILAR VOLUMES
Solar magnetic flux data accumulated from the magnetograph of the Mount Wilson Observatory are used to infer average east-west field inclination angles for the interval 196%1973. In all latitude zones the total flux (IF +] ยง measurements indicate that the field is inclined so as to trail the rotatio
In order to provide a smooth transition to a smaller aperture for the Mount Wilson daily magnetograms, a 2-step change was made, with two daily observations made using two different apertures covering an interval of several months. A comparison of these observations has made possible a check on the
The evolution of azimuthal modulation of the solar wind is examined by numerical integration of the basic equations governing supersonic, super-Alfv6nic, polytropic one fluid flow in the equatorial plane of the Sun with radial as well as azumuthal magnetic fields. The computations are started by int
In the task of studying stellar magnetic fields, polarimetric methods have been intensively used in Ap stars. But the observational material classically used to reconstruct stellar magnetic structures (average longitudinal magnetic field as a function of rotational phase) is not rich enough in spati