Critical Height for the Unstabilization of Prominences

Details Critical Height for the Unstabilization of Prominences Critical Height for the Unstabilization of Prominences

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh51a1660l&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH51A-1660

Astronomy and Astrophysics

Astrophysics

[7531] Solar Physics, Astrophysics, And Astronomy / Prominence Eruptions

Scientific paper

At which altitude will a prominence probably erupt? This question is statistically studied based on the 10072 solar limb prominences recognized by SLIPCAT from 2007 April to the end of 2009. We manually check all the prominences with leading edge greater than 1.2 Rs, and find that there are 256 disrupted prominences (DPs) and 106 stable prominences (SPs). Among the DPs, there are 149 prominences (EPs) showing a clear and successful eruption process in the STEREO/EUVI field of view and 107 prominences (FPs) presenting a failed eruption. The eruption process of EPs can be further classified into 3 types, single eruption (SE), multiple eruptions (ME) and gradual eruption (GE). When the main body of a EP first begins to ascend rapidly with a uniform velocity, we define the height of the prominence’s leading edge at this moment as the unstabilization height. FPs also have unstabilization heights as well. All the unstabilization heights are identified by hands. It is found that 65% DPs are unstabilized between 49 and 90 Mm. The comparison of the number of DPs with all the well-tracked prominences suggests that the ratio between them is a double-peak distribution with the most probable heights for a prominence being unstable at 83 and 125 Mm. The above two results suggest that there are two critical heights for the unstabilization of prominences: the primary height is 83 Mm and the secondary height is 125 Mm. We think two different heights present two kinds of prominences, the primary one corresponding to DPs around or at active region and the secondary one corresponding to DPs at quiet region. We also find eruption velocity of DPs is anti-correlated with the unstabilization height and the total brightness, which means that prominences with less mass and lower unstabilization height would require larger inputting energy and large eruption velocity. The association of EPs with CME in this study is 49%.

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