MULTI-STRAND CORONAL LOOP MODEL AND FILTER-RATIO ANALYSIS
- Max-Planck-Institut fuer Sonnensystemforschung, 37191 Katlenburg-Lindau (Germany)
We model a coronal loop as a bundle of seven separate strands or filaments. Each of the loop strands used in this model can independently be heated (near their left footpoints) by Alfven/ion-cyclotron waves via wave-particle interactions. The Alfven waves are assumed to penetrate the strands from their footpoints, at which we consider different wave energy inputs. As a result, the loop strands can have different heating profiles, and the differential heating can lead to a varying cross-field temperature in the total coronal loop. The simulation of Transition Region and Coronal Explorer (TRACE) observations by means of this loop model implies two uniform temperatures along the loop length, one inferred from the 171:195 filter ratio and the other from the 171:284 ratio. The reproduced flat temperature profiles are consistent with those inferred from the observed extreme-ultraviolet coronal loops. According to our model, the flat temperature profile is a consequence of the coronal loop consisting of filaments, which have different temperatures but almost similar emission measures in the cross-field direction. Furthermore, when we assume certain errors in the simulated loop emissions (e.g., due to photometric uncertainties in the TRACE filters) and use the triple-filter analysis, our simulated loop conditions become consistent with those of an isothermal plasma. This implies that the use of TRACE or EUV Imaging Telescope triple filters for observation of a warm coronal loop may not help in determining whether the cross-field isothermal assumption is satisfied or not.
- OSTI ID:
- 21392414
- Journal Information:
- Astrophysical Journal, Vol. 708, Issue 2; Other Information: DOI: 10.1088/0004-637X/708/2/1281; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
COSMOLOGY AND ASTRONOMY
ACCELERATION
ALFVEN WAVES
EMISSION
EXTREME ULTRAVIOLET RADIATION
ION PLASMA WAVES
MAGNETIC FIELDS
PARTICLE INTERACTIONS
SIMULATION
SUN
TELESCOPES
ELECTROMAGNETIC RADIATION
HYDROMAGNETIC WAVES
INTERACTIONS
ION WAVES
MAIN SEQUENCE STARS
PLASMA WAVES
RADIATIONS
STARS
ULTRAVIOLET RADIATION