Line formation in solar granulation: III. The photospheric Si and meteoritic Fe abundances

Details Line formation in solar granulation: III. The photospheric Si and meteoritic Fe abundances Line formation in solar granulation: III. The photospheric Si and meteoritic Fe abundances

2000-05-15

arxiv.org/abs/astro-ph/0005322v1

Astron.Astrophys.359:755-758,2000

Astronomy and Astrophysics

Astrophysics

Accepted for A&A

Scientific paper

Using realistic hydrodynamical simulations of the solar surface convection as 3D, time-dependent, inhomogeneous model atmospheres, the solar photospheric Si abundance has been determined to be log Si = 7.51 +- 0.04. This constitutes a difference of 0.04 dex compared with previous estimates based on the 1D Holweger-M\"uller (1974) model, of which half is attributable to the adopted model atmosphere and the remaining part to the improved quantum mechanical broadening treatment. As a consequence, all meteoritic abundances should be adjusted downwards by the same amount. In particular the meteoritic Fe abundance will be log Fe = 7.46 +- 0.01, in good agreement with the recently determined photospheric Fe abundance (Asplund et al. 2000b). The existing uncertainties unfortunately prevent an observational confirmation of the postulated effects of elemental migration of metals in the Sun.

Affiliated with

Also associated with

No associations

Rating

Line formation in solar granulation: III. The photospheric Si and meteoritic Fe abundances does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Line formation in solar granulation: III. The photospheric Si and meteoritic Fe abundances, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Line formation in solar granulation: III. The photospheric Si and meteoritic Fe abundances will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-441115