Analysis of Solar Transition Region Bright Points and Application to Existing Heating Models

Details Analysis of Solar Transition Region Bright Points and Application to Existing Heating Models Analysis of Solar Transition Region Bright Points and Application to Existing Heating Models

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21715510o&link_type=abstract

American Astronomical Society, AAS Meeting #217, #155.10; Bulletin of the American Astronomical Society, Vol. 43, 2011

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I have conducted an analysis on the spatial, spectral, and magnetic field data of bright point phenomena that occur in the Sun's upper transition region atmosphere. There are two main aspects to this study: an empirical study of the statistical distribution and properties of upper transition region bright points (UBPs) and a comparison of the measured quantities with theoretical models of their generation and characteristics. I also conducted a comparison of UBPs to other well-studied transition region (TR) phenomena such as blinkers, explosive events, and spicules. Our empirical study of UBPs is made possible through archived SOHO and Hinode data that contain full-disk images of the solar TR and corona with effective temperatures ranging from 0.10 MK to 2.0 MK. We measured surface densities, sizes, radiative outputs, Dopplergrams and magnetic structures of UBPs at 0.25 MK and 0.63 MK in the quiet Sun. The UBPs were modeled as hydrostatic loops to determine of volumetric heating rates. Comparison of the measured and modeled parameters suggest that magnetic reconnection is likely the dominate generation mechanism of UBPs, although MHD waves (or a combination of both) can not be ruled out.

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