scholarly journals Supernovae and transients with circumstellar interaction

2020 ◽  
Vol 7 (7) ◽  
pp. 200467
Author(s):  
Morgan Fraser
Keyword(s):  
Electron Capture ◽  
Low Energy ◽  
Core Collapse ◽  
Low Mass Stars ◽  
Circumstellar Material ◽  
Core Collapse Supernova ◽  
Low Mass

It is 30 years since the characteristic signatures of interaction with circumstellar material (CSM) were first observed in a core-collapse supernova. Since then, CSM interaction has been observed and inferred across a range of transients, from the low-energy explosions of low-mass stars as likely electron-capture supernovae, through to the brightest superluminous supernovae. In this review, I present a brief overview of some of the interacting supernovae and transients that have been observed to date, and attempt to classify and group them together in a phenomenological framework.

scholarly journals A low-energy core-collapse supernova without a hydrogen envelope

Nature ◽  
2009 ◽  
Vol 459 (7247) ◽  
pp. 674-677 ◽  
Author(s):  
S. Valenti ◽  
A. Pastorello ◽  
E. Cappellaro ◽  
S. Benetti ◽  
P. A. Mazzali ◽  
...  
Keyword(s):  
Low Energy ◽  
Core Collapse ◽  
Core Collapse Supernova

scholarly journals Angular momentum transport in massive stars and natal neutron star rotation rates

2019 ◽  
Vol 488 (3) ◽  
pp. 4338-4355 ◽  
Author(s):  
Linhao Ma ◽  
Jim Fuller
Keyword(s):  
Angular Momentum ◽  
Massive Stars ◽  
Baroclinic Instability ◽  
Core Collapse ◽  
Slow Rotation ◽  
Low Mass Stars ◽  
Rotation Rates ◽  
Rotation Periods ◽  
Low Mass ◽  
Binary Evolution

Abstract The internal rotational dynamics of massive stars are poorly understood. If angular momentum (AM) transport between the core and the envelope is inefficient, the large core AM upon core-collapse will produce rapidly rotating neutron stars (NSs). However, observations of low-mass stars suggest an efficient AM transport mechanism is at work, which could drastically reduce NS spin rates. Here, we study the effects of the baroclinic instability and the magnetic Tayler instability in differentially rotating radiative zones. Although the baroclinic instability may occur, the Tayler instability is likely to be more effective for AM transport. We implement Tayler torques as prescribed by Fuller, Piro, and Jermyn into models of massive stars, finding they remove the vast majority of the core’s AM as it contracts between the main-sequence and helium-burning phases of evolution. If core AM is conserved during core-collapse, we predict natal NS rotation periods of $P_{\rm NS} \approx 50\!-\!200 \, {\rm ms}$, suggesting these torques help explain the relatively slow rotation rates of most young NSs, and the rarity of rapidly rotating engine-driven supernovae. Stochastic spin-up via waves just before core-collapse, asymmetric explosions, and various binary evolution scenarios may increase the initial rotation rates of many NSs.

scholarly journals The Peculiar Ca-rich SN2019ehk: Evidence for a Type IIb Core-collapse Supernova from a Low-mass Stripped Progenitor

2021 ◽  
Vol 907 (1) ◽  
pp. L18
Author(s):  
Kishalay De ◽  
U. Christoffer Fremling ◽  
Avishay Gal-Yam ◽  
Ofer Yaron ◽  
Mansi M. Kasliwal ◽  
...  
Keyword(s):  
Core Collapse ◽  
Core Collapse Supernova ◽  
Low Mass

scholarly journals Three-dimensional models of core-collapse supernovae from low-mass progenitors with implications for Crab

2020 ◽  
Vol 496 (2) ◽  
pp. 2039-2084 ◽  
Author(s):  
G Stockinger ◽  
H-T Janka ◽  
D Kresse ◽  
T Melson ◽  
T Ertl ◽  
...  
Keyword(s):  
Three Dimensional ◽  
Iron Core ◽  
Core Collapse ◽  
Crab Pulsar ◽  
Core Collapse Supernova ◽  
Spin Period ◽  
The Core ◽  
Low Mass ◽  
Catch Up ◽  
Three Dimensional Models

ABSTRACT We present 3D full-sphere supernova simulations of non-rotating low-mass (∼9 M⊙) progenitors, covering the entire evolution from core collapse through bounce and shock revival, through shock breakout from the stellar surface, until fallback is completed several days later. We obtain low-energy explosions (∼0.5–1.0 × 1050 erg) of iron-core progenitors at the low-mass end of the core-collapse supernova (LMCCSN) domain and compare to a super-AGB (sAGB) progenitor with an oxygen–neon–magnesium core that collapses and explodes as electron-capture supernova (ECSN). The onset of the explosion in the LMCCSN models is modelled self-consistently using the vertex-prometheus code, whereas the ECSN explosion is modelled using parametric neutrino transport in the prometheus-HOTB code, choosing different explosion energies in the range of previous self-consistent models. The sAGB and LMCCSN progenitors that share structural similarities have almost spherical explosions with little metal mixing into the hydrogen envelope. A LMCCSN with less second dredge-up results in a highly asymmetric explosion. It shows efficient mixing and dramatic shock deceleration in the extended hydrogen envelope. Both properties allow fast nickel plumes to catch up with the shock, leading to extreme shock deformation and aspherical shock breakout. Fallback masses of $\mathord {\lesssim }\, 5\, \mathord {\times }\, 10^{-3}$ M⊙ have no significant effects on the neutron star (NS) masses and kicks. The anisotropic fallback carries considerable angular momentum, however, and determines the spin of the newly born NS. The LMCCSN model with less second dredge-up results in a hydrodynamic and neutrino-induced NS kick of >40 km s−1 and a NS spin period of ∼30 ms, both not largely different from those of the Crab pulsar at birth.

scholarly journals Synthetic observables for electron-capture supernovae and low-mass core collapse supernovae

2021 ◽  
Vol 503 (1) ◽  
pp. 797-814
Author(s):  
Alexandra Kozyreva ◽  
Petr Baklanov ◽  
Samuel Jones ◽  
Georg Stockinger ◽  
Hans-Thomas Janka
Keyword(s):  
Radiative Transfer ◽  
Light Curve ◽  
Electron Capture ◽  
Mass Range ◽  
Light Curves ◽  
Initial Mass ◽  
Core Collapse ◽  
Initial Composition ◽  
Solar Metallicity ◽  
Low Mass

ABSTRACT Stars in the mass range from 8 M⊙ to 10 M⊙ are expected to produce one of two types of supernovae (SNe), either electron-capture supernovae (ECSNe) or core-collapse supernovae (CCSNe), depending on their previous evolution. Either of the associated progenitors retain extended and massive hydrogen-rich envelopes and the observables of these SNe are, therefore, expected to be similar. In this study, we explore the differences in these two types of SNe. Specifically, we investigate three different progenitor models: a solar-metallicity ECSN progenitor with an initial mass of 8.8 M⊙, a zero-metallicity progenitor with 9.6 M⊙, and a solar-metallicity progenitor with 9 M⊙, carrying out radiative transfer simulations for these progenitors. We present the resulting light curves for these models. The models exhibit very low photospheric velocity variations of about 2000 km s−1; therefore, this may serve as a convenient indicator of low-mass SNe. The ECSN has very unique light curves in broad-bands, especially the U band, and does not resemble any currently observed SN. This ECSN progenitor being part of a binary will lose its envelope for which reason the light curve becomes short and undetectable. The SN from the 9.6 M⊙ progenitor exhibits also quite an unusual light curve, explained by the absence of metals in the initial composition. The artificially iron-polluted 9.6 M⊙ model demonstrates light curves closer to normal SNe IIP. The SN from the 9 M⊙ progenitor remains the best candidate for so-called low-luminosity SNe IIP like SN 1999br and SN 2005cs.

scholarly journals Electron-capture and Low-mass Iron-core-collapse Supernovae: New Neutrino-radiation-hydrodynamics Simulations

2017 ◽  
Vol 850 (1) ◽  
pp. 43 ◽  
Author(s):  
David Radice ◽  
Adam Burrows ◽  
David Vartanyan ◽  
M. Aaron Skinner ◽  
Joshua C. Dolence
Keyword(s):  
Electron Capture ◽  
Iron Core ◽  
Radiation Hydrodynamics ◽  
Core Collapse ◽  
Neutrino Radiation ◽  
Low Mass

scholarly journals The evolution of red supergiants to supernovae

2016 ◽  
Vol 12 (S329) ◽  
pp. 59-63
Author(s):  
Emma R. Beasor ◽  
Ben Davies
Keyword(s):  
Mass Loss ◽  
Early Stage ◽  
Initial Mass ◽  
Core Collapse ◽  
Circumstellar Material ◽  
Core Collapse Supernova ◽  
Evolved Stars ◽  
Circumstellar Extinction ◽  
Red Supergiants ◽  
Loss Rates

AbstractWith red supergiants (RSGs) predicted to end their lives as Type IIP core collapse supernova (CCSN), their behaviour before explosion needs to be fully understood. Mass loss rates govern RSG evolution towards SN and have strong implications on the appearance of the resulting explosion. To study how the mass-loss rates change with the evolution of the star, we have measured the amount of circumstellar material around 19 RSGs in a coeval cluster. Our study has shown that mass loss rates ramp up throughout the lifetime of an RSG, with more evolved stars having mass loss rates a factor of 40 higher than early stage RSGs. Interestingly, we have also found evidence for an increase in circumstellar extinction throughout the RSG lifetime, meaning the most evolved stars are most severely affected. We find that, were the most evolved RSGs in NGC2100 to go SN, this extra extinction would cause the progenitor’s initial mass to be underestimated by up to 9M⊙.

scholarly journals Understanding Galactic planetary nebulae with precise/reliable nebular abundances

2016 ◽  
Vol 12 (S323) ◽  
pp. 95-98
Author(s):  
D. A. García-Hernández ◽  
P. Ventura ◽  
G. Delgado-Inglada ◽  
F. Dell'Agli ◽  
M. Di Criscienzo ◽  
...  
Keyword(s):  
Planetary Nebulae ◽  
Asymptotic Giant Branch ◽  
High Mass ◽  
Binary Interaction ◽  
Core Collapse ◽  
Agb Stars ◽  
Stellar Rotation ◽  
Low Mass Stars ◽  
Low Mass ◽  
High Metallicity

AbstractWe compare recent precise/reliable nebular abundances - as derived from high-quality optical spectra and the most recent ICFs - in a sample of Galactic planetary nebulae (PNe) with nucleosynthesis predictions (HeCNOCl) from asymptotic giant branch (AGB) ATON models in the metallicity range Z⊙/4 < Z < 2Z⊙. According to the infrared dust features, the sample is divided among carbon-, oxygen-, and double-dust chemistry (CC, OC, and DC, respectively), providing an independent proxy for the nature of the PNe progenitors. Our AGB models, with diffusive overshooting from all the convective borders, nicely reproduce the O overabundances observed in CC PNe, indicating that they evolve from low-Z low-mass (∼1 −3 M⊙) AGB stars. This indicates that O is not always a good indicator of the original ISM metallicity and that the O production by low-mass stars should be considered in galactic-evolution models. The lowest metallicity OC PNe evolve from low-mass (∼1 M⊙) O-rich AGBs, while the higher metallicity ones (all with uncertain dust classifications) display a chemical pattern similar to the DC PNe. In agreement with the recent literature, the DC PNe mostly descend from high-mass (M > 3.5 M⊙) solar/supersolar metallicity AGBs that experience hot bottom burning (HBB), but other formation channels in low-mass AGBs like extra mixing, stellar rotation, binary interaction, or He pre-enrichment cannot be disregarded until more accurate C/O ratios can be obtained. Two DC PNe show the imprint of advanced CNO processing and deep second dredge-up, suggesting progenitors masses close to the limit to evolve as core collapse supernovae (above 6 M⊙). Their actual C/O ratios, if confirmed, indicate contamination from the third dredge-up, rejecting the hypothesis that the chemical composition of such high-metallicity massive AGBs is modified exclusively by HBB.

scholarly journals Multimessenger analysis strategy for core-collapse supernova search: gravitational waves and low-energy neutrinos

2021 ◽  
Vol 2021 (11) ◽  
pp. 021
Author(s):  
Odysse Halim ◽  
Claudio Casentini ◽  
Marco Drago ◽  
Viviana Fafone ◽  
Kate Scholberg ◽  
...  
Keyword(s):  
Gravitational Waves ◽  
Low Energy ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Analysis Strategy
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