Coronal Rotation Between 1.5 and 3.5 Solar Radii at Solar Minimum

Details Coronal Rotation Between 1.5 and 3.5 Solar Radii at Solar Minimum Coronal Rotation Between 1.5 and 3.5 Solar Radii at Solar Minimum

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh41b1655j&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH41B-1655

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7599] Solar Physics, Astrophysics, And Astronomy / General Or Miscellaneous

Scientific paper

Here we report on coronal rotation measurements using STEREO COR1. Multiple studies have confirmed that rotation rates in the outer corona differ markedly from those of the photosphere, where a steady decline in rotation rate with latitude is observed. Emission line observations of low-lying coronal magnetic features typically correspond well with photospheric rotation rates, while white-light measurements in the upper corona indicate very rigid rotation. Some studies have reported a sudden jump in the rotation rate in the 2.3-2.5 R_sun range, indicating a transition from differentially rotating features to rigidly rotating ones. It has been suggested that the rotation rates measured in a given study may be related to the lifetimes of features observed, which should make the simultaneous observation of features rotating at different rates difficult. Using autocorrelation measurements of COR1 data we have studied rotation rates between 1.5 and 3.5 solar radii for features with lifetimes longer than one full rotation. We observe latitudinally and radially rigid rotation during 2007 and 2008, and no transition from differentially rotating to rigidly rotating features. This is consistent with the idea that longer-lived features rotate more rigidly, or with a transition from differential to rigid rotation below 1.5 R_sun.

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