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
  • Help & Advice
University of Warwick

The Library

  • Login
  • Admin

Seismological demonstration of perpendicular density structuring in the solar corona

Tools
- Tools
+ Tools

Van Doorsselaere, Tom, Brady, Christopher S., Verwichte, E. (Erwin) and Nakariakov, V. M. (Valery M.) (2008) Seismological demonstration of perpendicular density structuring in the solar corona. Astronomy & Astrophysics, Vol.491 (No.2). L9-L12. doi:10.1051/0004-6361:200810659 ISSN 0004-6361.

[img] PDF
WRAP_VanDoorsselaere_34_seismological_aa10659-08[1].pdf - Requires a PDF viewer.

Download (468Kb)
Official URL: http://dx.doi.org/10.1051/0004-6361:200810659

Request Changes to record.

Abstract

The peculiarities of the propagating transverse waves observed in the solar corona with the CoronalMulti-channel Polarimeter (CoMP)indicate the existence of fine field structuring in the coronal density. We present results of numerical simulations studying the evolution of a localised transverse magneto-hydrodynamic wave in a uniform magnetic field. We consider two initial low plasma-beta
equilibria: one with a homogeneous density, and one with a field-aligned dense structure (such as a loop or a plume). The perpendicular localisation of the wave strongly determines the angular distribution of the energy propagation. If the perpendicular scale of the wave is significantly smaller than the parallel scale (e.g. wavelength), as established by CoMP, the wave develops as an oblique fast magneto-acoustic wave. In an unstructured medium, the energy of such a wave is transferred mainly across the magnetic field.
However, it is possible to channel the energy of the transverse wave along the magnetic field in the presence of a field-aligned density enhancement. We conclude that the CoMP results provide an independent seismological proof that the corona is structured in density
in the perpendicular direction.

Item Type: Journal Article
Subjects: Q Science > QB Astronomy
Divisions: Faculty of Science, Engineering and Medicine > Science > Physics
Library of Congress Subject Headings (LCSH): Sun -- Corona -- Magnetic fields -- Mathematical models, Magnetohydrodynamic waves -- Mathematical models, Solar oscillations
Journal or Publication Title: Astronomy & Astrophysics
Publisher: E D P Sciences
ISSN: 0004-6361
Official Date: November 2008
Dates:
DateEvent
November 2008Published
Volume: Vol.491
Number: No.2
Page Range: L9-L12
DOI: 10.1051/0004-6361:200810659
Status: Peer Reviewed
Access rights to Published version: Open Access (Creative Commons)
Funder: Seventh Framework Programme (European Commission) (FP7), Science and Technology Facilities Council (Great Britain) (STFC)

Data sourced from Thomson Reuters' Web of Knowledge

Request changes or add full text files to a record

Repository staff actions (login required)

View Item View Item

Downloads

Downloads per month over past year

View more statistics

twitter

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