Hostname: page-component-745bb68f8f-grxwn Total loading time: 0 Render date: 2025-01-31T12:47:57.049Z Has data issue: false hasContentIssue false
  • English
  • Français

The model of coronal hole with microwave observational data taking into account the solar wind flows

Published online by Cambridge University Press:  14 March 2005

V.N. Borovik ,
T.I. Kaltman  and
A.N. Korzhavin
V.N. Borovik
Affiliation:
Central Astronomical observatory, St.-Petersburg, Russia
T.I. Kaltman
Affiliation:
Special Astrophysical observatory, St.-Petersburg, Russia email: kti@saoran.spb.su
A.N. Korzhavin
Affiliation:
Special Astrophysical observatory, St.-Petersburg, Russia email: kti@saoran.spb.su
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The renew non-hydrostatic model of electron density, temperature and velocity distribution with height in coronal hole (CH) is build. The presented model is based on the measurements of magnetic field in CH with RATAN-600 observations and on the assumption about equality of magnetic and kinetic energy of upward plasma flows in CH at heights of generation of radio emission in wavelength range 20–30 cm. To construct this model the observational spectrum of brightness temperatures of CH in wavelength range 2–30 cm is used. The first results of modeling are presented.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS223 , June 2004 , pp. 229 - 230
Copyright
© 2004 International Astronomical Union