scholarly journals Massive star evolution and nucleosynthesis: Lower end of Fe-core-collapse supernova progenitors and remnant neutron star mass distribution

2012 ◽  
Vol 2012 (1) ◽  
pp. 1A302-0 ◽  
Author(s):  
H. Umeda ◽  
T. Yoshida ◽  
K. Takahashi
Keyword(s):  
Neutron Star ◽  
Mass Distribution ◽  
Massive Star ◽  
Core Collapse ◽  
Star Mass ◽  
Core Collapse Supernova ◽  
Star Evolution ◽  
Neutron Star Mass ◽  
Massive Star Evolution

scholarly journals Neutron star masses

2012 ◽  
Vol 8 (S291) ◽  
pp. 146-146
Author(s):  
David Nice
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Observational Data ◽  
Mass Distribution ◽  
Binary Star ◽  
Star Mass ◽  
Star Evolution ◽  
Neutron Star Mass ◽  
Present Understanding

AbstractNeutron star masses can be inferred from observations of binary pulsar systems, particularly by the measurement of relativistic phenomena within these orbits. The observed distribution of masses can be used to infer or constrain the equation of state for nuclear matter and to study astrophysical processes such as supernovae and binary star evolution. In this talk, I will review our present understanding of the neutron star mass distribution with an emphasis on the observational data.

scholarly journals 3D and Some Other Things Missing from the Theory of Massive Star Evolution

2014 ◽  
Vol 9 (S307) ◽  
pp. 459-469 ◽  
Author(s):  
W. David Arnett
Keyword(s):  
Massive Star ◽  
Core Collapse ◽  
Solar Abundance ◽  
Core Collapse Supernova ◽  
Star Evolution ◽  
Massive Star Evolution

AbstractThis is a sketch of a 321D approximation which is nonlocal, and thus has nonzero fluxes of KE (to be published in more detail elsewhere). We plan to add this as an option to MESA. Inclusion of KE fluxes seems to help resolve the solar abundance problem (Asplund et al.2009). Smaller cores may ease the explosion problems with core collapse supernova simulations.

scholarly journals Neutron Star Mass Distribution in Binaries

2016 ◽  
Vol 716 ◽  
pp. 012021
Author(s):  
Chang-Hwan Lee ◽  
Young-Min Kim
Keyword(s):  
Neutron Star ◽  
Mass Distribution ◽  
Star Mass ◽  
Neutron Star Mass

scholarly journals The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations

2019 ◽  
Vol 491 (2) ◽  
pp. 2715-2735 ◽  
Author(s):  
Adam Burrows ◽  
David Radice ◽  
David Vartanyan ◽  
Hiroki Nagakura ◽  
M Aaron Skinner ◽  
...  
Keyword(s):  
Neutron Star ◽  
Massive Star ◽  
State Of The Art ◽  
Mass Range ◽  
Core Collapse ◽  
Final States ◽  
Lower Mass ◽  
Core Collapse Supernova ◽  
Supernova Explosions ◽  
General Range

ABSTRACT We have conducted 19 state-of-the-art 3D core-collapse supernova simulations spanning a broad range of progenitor masses. This is the largest collection of sophisticated 3D supernova simulations ever performed. We have found that while the majority of these models explode, not all do, and that even models in the middle of the available progenitor mass range may be less explodable. This does not mean that those models for which we did not witness explosion would not explode in Nature, but that they are less prone to explosion than others. One consequence is that the ‘compactness’ measure is not a metric for explodability. We find that lower-mass massive star progenitors likely experience lower-energy explosions, while the higher-mass massive stars likely experience higher-energy explosions. Moreover, most 3D explosions have a dominant dipole morphology, have a pinched, wasp-waist structure, and experience simultaneous accretion and explosion. We reproduce the general range of residual neutron-star masses inferred for the galactic neutron-star population. The most massive progenitor models, however, in particular vis à vis explosion energy, need to be continued for longer physical times to asymptote to their final states. We find that while the majority of the inner ejecta have Ye = 0.5, there is a substantial proton-rich tail. This result has important implications for the nucleosynthetic yields as a function of progenitor. Finally, we find that the non-exploding models eventually evolve into compact inner configurations that experience a quasi-periodic spiral SASI mode. We otherwise see little evidence of the SASI in the exploding models.

scholarly journals Identifying Supernova Progenitors and Constraining the Explosion Channels

2011 ◽  
Vol 7 (S279) ◽  
pp. 110-117
Author(s):  
Schuyler D. Van Dyk
Keyword(s):  
Massive Star ◽  
Mass Range ◽  
Initial Mass ◽  
Current Status ◽  
Core Collapse ◽  
Evolutionary Models ◽  
Direct Identification ◽  
Star Evolution ◽  
Red Supergiants ◽  
Massive Star Evolution

AbstractConnecting the endpoints of massive star evolution with the various types of core-collapse supernovae (SNe) is ultimately the fundamental puzzle to be explored and solved. We can assemble clues indirectly, e.g., from information about the environments in which stars explode and establish constraints on the evolutionary phases of these stars. However, this is best accomplished through direct identification of the actual star that has exploded in pre-supernova imaging, preferably in more than one photometric band, where color and luminosity for the star can be precisely measured. We can then interpret the star's properties in light of expectations from the latest massive stellar evolutionary models, to attempt to assign an initial mass to the progenitor. So far, this has been done most successfully for SNe II-P, for which we now know that red supergiants in a relatively limited initial mass range are responsible. More recently, we have limited examples of the progenitors of SNe II-L, IIn, and IIb. The progenitors of SNe Ib and Ic, however, have been elusive so far; I will discuss the current status of our knowledge of this particular channel.

scholarly journals THE NEUTRON STAR MASS DISTRIBUTION

2013 ◽  
Vol 778 (1) ◽  
pp. 66 ◽  
Author(s):  
Bülent Kiziltan ◽  
Athanasios Kottas ◽  
Maria De Yoreo ◽  
Stephen E. Thorsett
Keyword(s):  
Neutron Star ◽  
Mass Distribution ◽  
Star Mass ◽  
Neutron Star Mass

scholarly journals Nucleosynthesis and Kilonovae from Strange Star Mergers

Universe ◽  
2019 ◽  
Vol 5 (6) ◽  
pp. 144
Author(s):  
J. E. Horvath ◽  
O. G. Benvenuto ◽  
E. Bauer ◽  
L. Paulucci ◽  
A. Bernardo ◽  
...  
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Mass Distribution ◽  
A Priori ◽  
Strange Star ◽  
Star Mass ◽  
Full Characterization ◽  
Neutron Star Mass ◽  
A Priori Probability

In this talk, we summarize the work in progress toward a full characterization of strange star–strange star (SS–SS) mergers related to the GW/GRB/kilonova events. In addition, we show that the a priori probability constructed from the observed neutron star mass distribution points toward an asymmetric binary system as the progenitor of the GW170817 event.

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