Skip to content Skip to navigation
University of Warwick
  • Study
  • |
  • Research
  • |
  • Business
  • |
  • Alumni
  • |
  • News
  • |
  • About

University of Warwick
Publications service & WRAP

Highlight your research

  • WRAP
    • Home
    • Search WRAP
    • Browse by Warwick Author
    • Browse WRAP by Year
    • Browse WRAP by Subject
    • Browse WRAP by Department
    • Browse WRAP by Funder
    • Browse Theses by Department
  • Publications Service
    • Home
    • Search Publications Service
    • Browse by Warwick Author
    • Browse Publications service by Year
    • Browse Publications service by Subject
    • Browse Publications service by Department
    • Browse Publications service by Funder
  • Statistics
  • Help & Advice
University of Warwick

The Library

  • Login

MHD seismology of the solar corona with SOHO and TRACE

Tools
- Tools
+ Tools

UNSPECIFIED (2001) MHD seismology of the solar corona with SOHO and TRACE. In: 24th General Assembly of the International-Astronomical-Union, AUG 07-18, 2000, MANCHESTER, ENGLAND.

Full text not available from this repository.

Abstract

Recent discoveries of MHD wave motions in the solar corona done with EUV imaging telescopes onboard SOHO and TRACE provide an observational basis for the MHD seismology of the corona. Measuring the properties of MHD waves and oscillations (periods, wavelengths, amplitudes, temporal and spatial signatures), combined with theoretical modeling of the wave phenomena, allow us to determine values of the mean parameters of the corona (the magnetic field strength, transport coefficients, etc.). As an example, we consider post-flare decaying oscillations of loops, observed with TRACE (14th July 1998 at 12:55 UT). An analysis of the oscillations shows that they are quasi-harmonic, with a period of about 265 s, and quickly decaying with the decay time of about 14.5 min. The period of oscillations allows us to determine the Alfven speed in the oscillating loop about 770 km/s. This value can be used for deduction of the value of the magnetic field in the loop (giving 10-30 G). The decay time, in the assumption that the decay is caused by viscous (or resistive) dissipation, gives us the Reynolds number of 10(5.3-6.1) (or the Lundquist number of 10(5.0-5.8)).

Item Type: Conference Item (UNSPECIFIED)
Subjects: Q Science > QB Astronomy
Series Name: IAU SYMPOSIA
Journal or Publication Title: RECENT INSIGHTS INTO THE PHYSICS OF THE SUN AND HELIOSPHERE: HIGHLIGHTS FROM SOHO AND OTHER SPACE MISSIONS
Publisher: ASTRONOMICAL SOC PACIFIC
ISBN: 1-58381-069-2
ISSN: 0074-1809
Editor: Brekke, P and Fleck, B and Gurman, JB
Date: 2001
Number: 203
Number of Pages: 3
Page Range: pp. 353-355
Publication Status: Published
Title of Event: 24th General Assembly of the International-Astronomical-Union
Location of Event: MANCHESTER, ENGLAND
Date(s) of Event: AUG 07-18, 2000
URI: http://wrap.warwick.ac.uk/id/eprint/10867

Data sourced from Thomson Reuters' Web of Knowledge

Request changes to a record

Actions (login required)

View Item View Item
twitter

Email us: publications@warwick.ac.uk
Contact Details
About Us