Stellar wind yields of very massive stars

被引:19
作者
Higgins, Erin R. [1 ]
Vink, Jorick S. [1 ]
Hirschi, Raphael [2 ,3 ]
Laird, Alison M. [4 ]
Sabhahit, Gautham N. [1 ]
机构
[1] Armagh Observ & Planetarium, Coll Hill, Armagh BT61 9DG, North Ireland
[2] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England
[3] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwanoha, Kashiwa 2778583, Japan
[4] Univ York, Sch Phys Engn & Technol, York YO10 5DD, England
基金
美国国家科学基金会;
关键词
stars: massive; stars: evolution; stars: abundances; stars: mass-loss; stars: interiors; nuclear reactions; nucleosynthesis; abundances; CONVECTIVE BOUNDARIES; ABUNDANCE PATTERNS; GLOBULAR-CLUSTERS; MODULES; EVOLUTION; METALLICITY; NUCLEOSYNTHESIS; POPULATIONS; DEPENDENCE; ROTATION;
D O I
10.1093/mnras/stad2537
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The most massive stars provide an essential source of recycled material for young clusters and galaxies. While very massive stars (VMSs, M > 100 M-circle dot) are relatively rare compared to O stars, they lose disproportionately large amounts of mass already from the onset of core H-b urning. VMS ha ve optically thick winds with ele v ated mass-loss rates in comparison to optically thin standard O-star winds. We compute wind yields and ejected masses on the main sequence, and we compare enhanced mass-loss rates to standard ones. We calculate solar metallicity wind yields from MESA stellar evolution models in the range 50-500 M-circle dot , including a large nuclear network of 92 isotopes, investigating not only the CNO-cycle, but also the Ne-Na and Mg-Al cycles. VMS with enhanced winds eject 5-10 times more H-processed elements (N, Ne, Na, Al) on the main sequence in comparison to standard winds, with possible consequences for observed anticorrelations, such as C-N and Na-O, in globular clusters. We find that for VMS 95 per cent of the total wind yields is produced on the main sequence, while only similar to 5 per cent is supplied by the post-main sequence. This implies that VMS with enhanced winds are the primary source of Al-26, contrasting previous works where classical Wolf-Rayet winds had been suggested to be responsible for galactic Al-26 enrichment. Finally, 200 M-circle dot stars eject 100 times more of each heavy element in their winds than 50 M-circle dot stars, and even when weighted by an IMF their wind contribution is still an order of magnitude higher than that of 50 M-circle dot stars.
引用
收藏
页码:534 / 547
页数:14
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