Physics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp61a02k&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SP61A-02
Physics
7507 Chromosphere, 7509 Corona, 7843 Numerical Simulation Studies
Scientific paper
The existence of cool plasma high in the solar corona was first established a century ago. In addition to the well-studied phenomenon of prominences, persistent knots and episodic downflows of cool plasma commonly denoted `coronal rain' have been observed in Hα , EUV, and UV spectral lines. Our recent 1D hydrodynamic simulations of localized, steady heating near the footpoints of long coronal loops produce dynamic condensations which form, flow, and fall onto the nearest chromosphere over the course of tens of hours (Antiochos et al. 2000, Karpen et al. 2001). In low-lying loops, this process yields condensed knots with dimensions and velocities consistent with high-resolution observations of counterstreaming flows along prominence spines (Zirker et al. 1998). Similar condensations develop even in high ( ~100,000 km) model loops, although they are small, short-lived, and form at irregular intervals. In order to explain the broader phenomenon of coronal condensations beyond prominences, however, we must investigate the effects of temporally varying, localized footpoint heating on the plasma dynamics in a range of active-region and quiet-Sun loops. We will discuss the results of a series of 1D numerical simulations with spatially and temporally variable heating, their observable signatures, and how well they reproduce observations by SOHO and TRACE of `coronal rain' and coronal condensations (e.g., Brekke 1999; Schrijver 2001).
Antiochos Spiro K.
Karpen Judith T.
MacNeice Peter J.
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