High-speed coronal rain

Free access article

Issue		A&A Volume 436, Number 3, June IV 2005


Page(s)		1067 - 1074
Section		The Sun
DOI		http://dx.doi.org/10.1051/0004-6361:20042141

A&A 436, 1067-1074 (2005)
DOI: 10.1051/0004-6361:20042141

High-speed coronal rain

D. A. N. Müller^{1, 2, 3}, A. De Groof⁴, V. H. Hansteen^{1, 2} and H. Peter³

¹ Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway
    e-mail: [Daniel.Mueller;Viggo.Hansteen]@astro.uio.no
² Center of Mathematics for Applications, University of Oslo, PO Box 1053 Blindern, 0316 Oslo, Norway
³ Kiepenheuer-Institut für Sonnenphysik, Schöneckstr. 6, 79104 Freiburg, Germany
    e-mail: peter@kis.uni-freiburg.de
⁴ Centrum voor Plasma-Astrofysica, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
    e-mail: Anik.DeGroof@wis.kuleuven.ac.be

(Received 8 October 2004 / Accepted 24 January 2005)

Abstract
At high spatial and temporal resolution, coronal loops are observed to have a highly dynamic nature. Recent observations with SOHO and TRACE frequently show localized brightenings "raining" down towards the solar surface. What is the origin of these features? Here we present for the first time a comparison of observed intensity enhancements from an EIT shutterless campaign with non-equilibrium ionization simulations of coronal loops in order to reveal the physical processes governing fast flows and localized brightenings. We show that catastrophic cooling around the loop apex as a consequence of footpoint-concentrated heating offers a simple explanation for these observations. An advantage of this model is that no external driving mechanism is necessary as the dynamics result entirely from the non-linear character of the problem.

Key words: Sun: corona -- Sun: transition region -- Sun: UV radiation -- Sun: magnetic fields -- Sun: atmosphere

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