Differential rotation of the solar atmosphere as determined from millimeter data

Abstract

Radiospectroheliograms obtained at millimeter wavelengths were used to determine the rotation of the solar atmosphere. Regions observed in both emission as well as absorption (associated with Hα dark filaments) were followed across the disk. The average sidereal rotation rate deduced from emissive regions is given by ω (deg day-1)=14.152(±0.270)-4.194(±3.017)sin2 B, where B is the heliographic latitude and the quoted errors are the standard deviations of a least squares fit to the data. The rate deduced from absorption regions is given by ω=14.729(±0.286)-1.050(±1.611)sin2 B. This rate is larger than that of emissive regions at all latitudes and shows smaller differential rotation. This apparent difference in the rotation rates is probably due to the difference in the height of formation of the emissive and absorption regions. This difference could be used to estimate the difference in height between an emissive region and an absorption feature in millimeter radiation.