On the viscosity effects in the shock wave observed in the solar wind after the December 13, 2006 coronal mass ejection

Cavus H.

ASTROPHYSICAL BULLETIN, vol.70, no.1, pp.117-122, 2015 (SCI-Expanded) identifier identifier

  • Publication Type: Article / Article
  • Volume: 70 Issue: 1
  • Publication Date: 2015
  • Doi Number: 10.1134/s1990341315010137
  • Journal Name: ASTROPHYSICAL BULLETIN
  • Journal Indexes: Science Citation Index Expanded (SCI-EXPANDED), Scopus
  • Page Numbers: pp.117-122
  • Keywords: solar wind, Sun: coronal mass ejections (CMEs), Sun: activity, REGION
  • Çanakkale Onsekiz Mart University Affiliated: Yes

Abstract

Coronal mass ejections (CMEs) and solar wind are the main results of solar activity. These events can drive interplanetary shock waves and produce geomagnetic storms. The study of these events is very important for space weather purposes. The shock waves occur where the solar wind changes its characteristics from being supersonic (with respect to the surrounding interplanetary medium) to being subsonic. In the supersonic regime of compressible gas flow, the interaction of shock waves with viscosity is one of the central problems. The main purpose of this study is to search for the effects of viscosity in the shock wave observed after the December 13, 2006 coronal mass ejection.