Latitudinal and Radial Variation of Solar Corona Rotation at Solar Minimum

Details Latitudinal and Radial Variation of Solar Corona Rotation at Solar Minimum Latitudinal and Radial Variation of Solar Corona Rotation at Solar Minimum

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..934..119g&link_type=abstract

FLOWS, BOUNDARIES, INTERACTIONS: Flows, Boundaries, and Interaction Workshop. AIP Conference Proceedings, Volume 934, pp. 119-1

Physics

Corona, Diameter, Rotation, And Mass, Time Series Analysis, Time Variability, Solar Wind Plasma, Sources Of Solar Wind

Scientific paper

The rotation of the solar corona at different heliolatitudes from 1.5 to 3.0 Rsolar from Sun center has been studied at solar minimum from the reconstructed intensity time series of the O VI 1032 Å and H I Lyα l216 Å spectral lines and visible light polarized brightness obtained by the observations of UVCS/SOHO instrument. The time period analyzed range from mid May 1996 to mid May 1997, when, at solar minimum, some features persist for several rotations, thus allowing to analyze the UV and visible emission as time series modulated at the period of the solar rotation. The coronal differential rotation rate significantly differs from that of the photospheric plasma. The estimated equatorial synodic rotation period of the corona at 1.5 Rsolar is 27.48+/-0.15 days. The study of the latitudinal variation shows that the UV corona decelerates towards the photospheric rates from the equator up to the poleward boundary of the mid-latitude streamers, reaching a peak of 28.16+/-0.20 days around +/-30° from the equator at 1.5 Rsolar, while a less evident peak is observed in the northern hemisphere, suggesting a real north-south rotational asymmetry, the northern hemisphere the rotation looks more solid-body-like and slower than in the southern hemisphere. The mid-latitude results are also confirmed by the visible light data available at 1.75 and 2.0 Rsolar. The study of the radial rotation profiles shows that the corona is rotating almost rigidly with height, but we find an abrupt increase by about half a days between 2.3 and 2.5 Rsolar. The larger radial and latitudinal gradients of the rotation rates are localized at the boundary between the open and closed field lines, suggesting that in these regions the differential rotation might be a source of magnetic stress and, consequently, of energy release.

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