In:
Publications of the Astronomical Society of Japan, Oxford University Press (OUP), Vol. 56, No. 2 ( 2004-04-25), p. 407-414
Abstract:
Taking into account the increasing mass of a central object through fall-back, we investigated nucleosynthesis inside an accretion disk formed during a core collapse of a massive star. It has been confirmed that the disk is an advection-dominated accretion flow supported by gas or radiation pressure. A sequence of ($\alpha, \gamma$) reactions take place and Fe-group elements are produced inside the disk. At the early phase of the fall-back, when O-rich materials inflow, the ejected gas contains abundant ${{54\atop} \mathrm{Fe}}$ and ${{56, 58\atop} \mathrm{Ni}}$. At the late phase the in-coming material is He-rich and the out-going gas is abundant of ${{44\atop} \mathrm{Ti}}$ as well as Fe and Ni. Provided that the processed gas outflows from the inner region up to the ejection radius, $r_\mathrm{ej}$, we find that the ejected mass of the heavy elements is not very sensitive to $r_\mathrm{ej}$, as long as we take $r_\mathrm{ej} \ge 50 \,r_\mathrm{g}$, because these elements are produced mainly in the region $20 \hbox{--} 100 \,r_\mathrm{g}$.
Type of Medium:
Online Resource
ISSN:
0004-6264
,
2053-051X
DOI:
10.1093/pasj/56.2.407
Language:
English
Publisher:
Oxford University Press (OUP)
Publication Date:
2004
detail.hit.zdb_id:
2206640-8
detail.hit.zdb_id:
2083084-1
SSG:
16,12
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