TRACE Observation of Damped Coronal Loop Oscillations: Implications for Coronal Heating-Reference-Cited by-同舟云学术

TRACE Observation of Damped Coronal Loop Oscillations: Implications for Coronal Heating

Published:1999-08-06 Issue:5429 Volume:285 Page:862-864
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Nakariakov V. M.¹,Ofman L.²,DeLuca E. E.³,Roberts B.¹,Davila J. M.⁴

Affiliation:

1. School of Mathematical and Computational Sciences, University of St. Andrews, St. Andrews, Fife KY16 9SS, Scotland.

2. Raytheon ITSS/NASA Goddard Space Flight Center, 682, Greenbelt, MD 20771, USA.

3. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA.

4. NASA Goddard Space Flight Center, 682, Greenbelt, MD 20771, USA.

Abstract

The imaging telescope on board the Transition Region and Coronal Explorer (TRACE) spacecraft observed the decaying transversal oscillations of a long [(130 ± 6) × 10 6 meters], thin [diameter (2.0 ± 0.36) × 10 6 meters], bright coronal loop in the 171 angstrom Fe IX emission line. The oscillations were excited by a solar flare in the adjacent active region. The decay time of the oscillations is 14.5 ± 2.7 minutes for an oscillation with a frequency 3.90 ± 0.13 millihertz. The coronal dissipation coefficient is estimated to be eight to nine orders of magnitude larger than the theoretically predicted classical value. The larger dissipation coefficient may solve existing difficulties with wave heating and reconnection theories.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference30 articles.

1. The TRACE spacecraft contains a 30-cm diameter telescope with 8.66-m Cassegrain focal length. The optics consists of superpolished mirrors individually coated in four quadrants to allow observations of the three extreme ultraviolet emission lines of 171 Å (Fe IX ) 195 Å (Fe XII ) and 284 Å (Fe XV ) and between 1200 and 7000 Å. Focal plane filters allow TRACE to select ultraviolet passbands around Lyman-α (1216 Å) C IV (1550 Å) the ultraviolet continuum at 1600 Å and 1700 Å and the visible continuum up to 7000 Å wavelengths (26). Additional detail on the TRACE spacecraft can be found in Handy et al. (27) and at . First results from the TRACE mission are reported by Schrijver et al. (28) and by Golub et al. (29).

2. Fast pulsations in the solar corona

3. On coronal oscillations

4. M. J. Aschwanden L. Fletcher C. Schrijver D. Alexander ibid. in press.

5. Ionson J. A. 226 650 (1978).

Cited by 832 articles. 订阅此论文施引文献订阅此论文施引文献，注册后可以免费订阅5篇论文的施引文献，订阅后可以查看论文全部施引文献

1. Propagating kink waves in an open coronal magnetic flux tube with gravitational stratification: Magnetohydrodynamic simulation and forward modelling;Astronomy & Astrophysics;2024-09

2. Three-wave coupling observed between a shear Alfvén wave and a kink-unstable magnetic flux rope;Physics of Plasmas;2024-09-01

3. Transverse Oscillations and Kelvin–Helmholtz Instability in Curved Arcade Loops with Siphon Flows;The Astrophysical Journal;2024-08-23

4. Two successive EUV waves and a transverse oscillation of a quiescent prominence;Monthly Notices of the Royal Astronomical Society;2024-08-10

5. Resonant Absorption of Standing Magnetohydrodynamic Waves in Coronal Loops in the Absence of Directional Symmetry: The Effect of Plasma Flow;The Astrophysical Journal;2024-08-01