Abstract
In order to explore various aspects of stellar evolution, supernovae, gamma ray bursts, and nucleosynthesis, we have developed a new efficient stellar evolution code. In this paper, we describe this new code and compare the results with those calculated by the previous code. Specifically, we focus on the progenitor evolution of the lower end of Fe-core-collapse supernovae, and the mass distribution of remnant neutron stars. We describe how different assumptions will lead to different neutron star mass distributions. We also review some of the recent work by our research group.
Highlights
Massive stars end their life as supernovae leaving neutron stars behind, or by forming blackholes without explosions if they are not rotating
In this paper we describe this new code, the Yoshida-Umeda (YU) code,20) and compare the results with the ones calculated by one of the author, H.U., using the Umeda-Nomoto (UN) code.16), 17), 21), 22) We briefly review some of the recent works using the Yoshida & Umeda (YU) code and other works in our research group
Before describing the YU code, we briefly describe the UN code because we will compare the results of these codes
Summary
Massive stars end their life as supernovae leaving neutron stars behind, or by forming blackholes without explosions if they are not rotating. Calculations for the progenitors of such low mass core-collapse supernovae with updated input physics are interesting and important Their evolution can be quite different if the initial mass is only slightly different, say by 0.01-0.1 M⊙ (e.g., Ref. 8); see Sec. 3.1). In the NH code time-dependent mixing length theory26), 27) can be included for convective energy transfer, though this effect is not so important for the massive star evolution forming an Fe-core. In order to calculate nuclear energy generation rates, in the UN code nuclear reaction networks are solved simultaneously with Henyey relaxation, while in the NH and SNK codes abundance is fixed during Henyey relaxation. Solving abundance implicitly is the best way to obtain consistency in the energy generation rates and the abundance evolution This has a disadvantage in efficient calculations because solving large reaction networks involves time consuming matrix inversion calculations.
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