Solar models with revised abundances and opacities

被引:42
作者
Yang, W. M. [1 ]
Bi, S. L. [1 ]
机构
[1] Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, Kunming 650011, Peoples R China
关键词
Sun : abundances; Sun : helioseismology; Sun : interior;
D O I
10.1086/513694
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Using reconstructed opacities, we construct solar models with low heavy-element abundance. Rotational mixing and enhanced diffusion of helium and heavy elements are used to reconcile the recently observed abundances with helioseismology. The sound speed and density of models in which the relative and absolute diffusion coefficients for helium and heavy elements have been increased agree with seismically inferred values at better than the 0.005 and 0.02 fractional levels, respectively. However, the surface helium abundance of the enhanced diffusion model is too low. The low-helium problem in the enhanced diffusion model can be solved to a great extent by rotational mixing. The surface helium and the convection zone depth of rotating model M04R3, which has a surface Z of 0.0154, agree with the seismic results at the levels of 1 sigma and 3 sigma, respectively. M04R3 is almost as good as the standard model M98. Some discrepancies between the models constructed in accord with the new element abundances and seismic constraints can be solved individually, but it seems difficult to resolve them as a whole.
引用
收藏
页码:L67 / L70
页数:4
相关论文
共 34 条
[1]   Determining solar abundances using helioseismology [J].
Antia, H. M. ;
Basu, Sarbani .
ASTROPHYSICAL JOURNAL, 2006, 644 (02) :1292-1298
[2]   The discrepancy between solar abundances and helioseismology [J].
Antia, HM ;
Basu, S .
ASTROPHYSICAL JOURNAL, 2005, 620 (02) :L129-L132
[3]   Line formation in solar granulation -: VI.: [Cl], Cl, CH and C2 lines and the photospheric C abundance [J].
Asplund, M ;
Grevesse, N ;
Sauval, AJ ;
Prieto, CA ;
Blomme, R .
ASTRONOMY & ASTROPHYSICS, 2005, 431 (02) :693-705
[4]   Line formation in solar granulation - IV. [O I], OI and OH lines and the photospheric O abundance [J].
Asplund, M ;
Grevesse, N ;
Sauval, AJ ;
Prieto, CA ;
Kiselman, D .
ASTRONOMY & ASTROPHYSICS, 2004, 417 (02) :751-768
[5]  
ASPLUND M, 2006, IAU S, V239, P9
[6]   Solar carbon monoxide, thermal profiling, and the abundances of C, O, and their isotopes [J].
Ayres, Thomas R. ;
Plymate, Claude ;
Keller, Christoph U. .
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 2006, 165 (02) :618-651
[7]   Updated opacities from the opacity project [J].
Badnell, NR ;
Bautista, MA ;
Butler, K ;
Delahaye, F ;
Mendoza, C ;
Palmeri, P ;
Zeippen, CJ ;
Seaton, MJ .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2005, 360 (02) :458-464
[8]   Helioseismological implications of recent solar abundance determinations [J].
Bahcall, JN ;
Basu, S ;
Pinsonneault, M ;
Serenelli, AM .
ASTROPHYSICAL JOURNAL, 2005, 618 (02) :1049-1056
[9]   How accurately can we calculate the depth of the solar convective zone? [J].
Bahcall, JN ;
Serenelli, AM ;
Pinsonneault, M .
ASTROPHYSICAL JOURNAL, 2004, 614 (01) :464-471
[10]   Constraining solar abundances using helioseismology [J].
Basu, S ;
Antia, HM .
ASTROPHYSICAL JOURNAL, 2004, 606 (01) :L85-L88