Some MHD solutions for the bottom of the solar convective layer

ÇAVUŞ H., Karafistan A. I.

Workshop on Solar and Stellar Physics through Eclipses, Antalya, Türkiye, 27 - 29 Mart 2006, cilt.370, ss.74-75 identifier

  • Yayın Türü: Bildiri / Tam Metin Bildiri
  • Cilt numarası: 370
  • Basıldığı Şehir: Antalya
  • Basıldığı Ülke: Türkiye
  • Sayfa Sayıları: ss.74-75
  • Çanakkale Onsekiz Mart Üniversitesi Adresli: Evet

Özet

The magnetic field responsible for the solar activity is stored in the base of the convective zone. Applying this knowledge to the bottom of the convection zone in the Sun our objective was to investigate some magnetohydrodynamical (MHD) solutions. The first order perturbation approximation was used in order to calculate the small perturbations on the physical parameters of a Standard Solar Model (SSM) excluding both rotation and magnetic field (Christensen-Dalsgaard et al. 1996) in the unperturbed equilibrium case. The validity of each approximation is tested and examined from the SSM. The MHD results thus obtained are presented graphically and compared with those of the SSM.