CAN STELLAR MIXING EXPLAIN THE LACK OF TYPE Ib SUPERNOVAE IN LONG-DURATION GAMMA-RAY BURSTS?

被引：24

作者：

Frey, Lucille H. ^{[1
,2
]}

Fryer, Chris L. ^{[3
,4
,5
]}

Young, Patrick A. ^{[6
]}

机构：

[1] Los Alamos Natl Lab, HPC 3, Los Alamos, NM 87545 USA

[2] Univ New Mexico, Dept Comp Sci, Albuquerque, NM 87131 USA

[3] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA

[4] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA

[5] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA

[6] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85276 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2013年 / 773卷 / 01期

基金：

美国国家科学基金会;

关键词：

stars: neutron; supernovae: general; TURBULENT CONVECTION; COLLAPSE;

D O I：

10.1088/2041-8205/773/1/L7

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The discovery of supernovae associated with long-duration gamma-ray burst observations is primary evidence that the progenitors of these outbursts are massive stars. One of the principle mysteries in understanding these progenitors has been the fact that all of these gamma-ray-burst-associated supernovae are Type Ic supernovae with no evidence of helium in the stellar atmosphere. Many studies have focused on whether or not this helium is simply hidden from spectral analyses. In this Letter, we show results from recent stellar models using new convection algorithms based on our current understanding of stellar mixing. We demonstrate that enhanced convection may lead to severe depletion of stellar helium layers, suggesting that the helium is not observed simply because it is not in the star. We also present light curves and spectra of these compact helium-depleted stars compared to models with more conventional helium layers.

引用

页数：4