Georgy 2009 Ib/c型超新星和伽玛暴的前身星

主要内容:
有WO, WC等. 从诞生率看, 只有一部分超新星产生伽玛暴, 可能是那些旋转速度很快的一部分. (不过不知道他们的伽玛暴诞生率经过了喷流张角改正没有.)

伽玛暴更容易发射在低金属丰度的地方, 而Ic型超新星容易发射在高金属丰度.

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Title:		The different progenitors of type Ib, Ic SNe, and of GRB
Authors:		Georgy, Cyril; Meynet, Georges; Walder, Rolf; Folini, Doris; Maeder, André
Publication:		eprint arXiv:0906.2284
Publication Date:		06/2009
Origin:		ARXIV
Keywords:		Astrophysics - Solar and Stellar Astrophysics
Comment:		13 pages, 10 figures. Accepted for publication in Astronomy and Astrophysics
Bibliographic Code:		2009arXiv0906.2284G

Abstract

We discuss the properties of the progenitors of core collapse SNe, as they can be deduced from rotating stellar models of single stars. The type of the SN progenitor was determined from the surface abundances at the pre-SN stage. The type of the SN event was obtained from the masses of hydrogen and helium ejected at the time of the core-collapse SN event. We find that the minimum amount of helium ejected by a core-collapse SN (of whatever type) is around 0.3 MSun. There is no difference between the WC and WO stars in the ejected masses of helium, CNO elements, and heavy elements. Also no difference is expected between the chemical composition of a WC star resulting from a normal or a homogeneous evolution. The progenitors of type Ib SNe are WNL, WNE, or less massive WC stars. Those of type Ic are WC and WO stars. WO stars are produced in a limited mass range (around 60 MSun) and only at low metallicity (for <= 0.010) as already found. The WO stars are the progenitors of only a small fraction of type Ic. Present stellar models indicate that, at solar metallicity, there is about 1 type Ib SN for 1 type Ic, and this ratio rises to 3 type Ic for 1 type Ib SN at twice solar metallicity. At this metallicity, type Ic's are more frequent than type Ib's because most massive stars that go through a WNE stage evolve further into a WC/WO phase. Current models can account for the observed number ratios SN Ib/SN II and SN Ic/SN II and for their observed variation with the metallicity. In case no supernova occurs when a black hole is formed, single-star models can still account for more than half of the observed (SN Ib+SN Ic)/SN II ratio for Z >= ZSun. For the GRB rate, our models produce too large a number for such an event, even if we restrict the progenitor to the WO stars.

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