What do models and helioseismology tell us about the solar evolution?

Yildiz M.

SOHO 10/GONG 2000 Workshop on Helio- and Asteroseismology at the Dawn of the Millennium, SANTA CRUZ TENERI, İspanya, 2 - 06 Ekim 2000, cilt.464, ss.571-573 identifier

  • Cilt numarası: 464
  • Basıldığı Şehir: SANTA CRUZ TENERI
  • Basıldığı Ülke: İspanya
  • Sayfa Sayıları: ss.571-573


Helioseismology puts very important constraints on the Solar models. which can not be available by another way. Surface helium abundance and base radius of the convective zone are known very precisely from inversion of p-mode oscillations. Also from inversion. almost from center to surface of the Sun. the sound speed was accurately determined. In this study, in the light of these constraints, two tests are done on the solar models. In tile first test we assume that the convective parameter nas larger than die present value. and. in that case, sound speed difference between the standard solar models and tile Stun just beneath die convective zone can be removed. In the second test. we assume that the Sun rotated with a certain value of angular momentum up to a time, and, after this time, it lost its whole angular momentum. The result of this test implies that, for a significant time after ZAMS, the central region of the Sun rotated faster than the outer regions and nle can get further information about the angular momentum evolution of the Sun bq; comparing tile sound speed differences between models and the Sun.