Massive stars in the range 13-25 M⊙:: Evolution and nucleosynthesis.: II.: The solar metallicity models

被引：146

作者：

Limongi, M

Straniero, O

Chieffi, A

机构：

[1] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy

[2] Osserv Astron Collurania, I-64100 Teramo, Italy

[3] CNR, Ist Astrofis Spaziale, I-00133 Rome, Italy

来源：

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2000年 / 129卷 / 02期

关键词：

nuclear reactions; nucleosynthesis; abundances; stars : evolution; stars : interiors; supernovae : general;

D O I：

10.1086/313424

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the evolutionary properties of a set of massive stellar models (namely 13, 15, 20, and 25 M-circle dot) from the main-sequence phase up to the onset of the iron core collapse. All these models have initial solar chemical composition, i.e., Y = 0.285 and Z = 0.02. A 179 isotope network, extending from neutron up to Zn-68 and fully coupled to the evolutionary code has been adopted from the carbon burning onward. Our results are compared, whenever possible, to similar computations available in literature.

引用

页码：625 / 664

页数：40

共 39 条

[1]

Arnett W. D., 1996, SUPERNOVAE NUCLEOSYN

[2] ADVANCED EVOLUTION OF MASSIVE STARS .1. HELIUM BURNING [J].