Handbook of Supernovae
01 Jan 2017-
About: The article was published on 2017-01-01. It has received 298 citations till now.
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TL;DR: In this paper, the authors constructed a chemical evolution model for all stable elements from C (A = 12) to U (A=238) from first principles, i.e., using theoretical nucleosynthesis yields and event rates of all chemical enrichment sources.
Abstract: To reach a deeper understanding of the origin of elements in the periodic table, we construct Galactic chemical evolution (GCE) models for all stable elements from C (A=12) to U (A=238) from first principles, i.e., using theoretical nucleosynthesis yields and event rates of all chemical enrichment sources. This enables us to predict the origin of elements as a function of time and environment. In the solar neighborhood, we find that stars with initial masses of M>30M_\odot can become failed supernovae if there is a significant contribution from hypernovae (HNe) at M~20-50M_\odot. The contribution to GCE from super asymptotic giant branch (AGB) stars (with M~8-10M_\odot at solar metallicity) is negligible, unless hybrid white dwarfs from low-mass super-AGB stars explode as so-called Type Iax supernovae, or high-mass super-AGB stars explode as electron-capture supernovae (ECSNe). Among neutron-capture elements, the observed abundances of the second (Ba) and third (Pb) peak elements are well reproduced with our updated yields of the slow neutron-capture process (s-process) from AGB stars. The first peak elements, Sr, Y, and Zr, are sufficiently produced by ECSNe together with AGB stars. Neutron star mergers can produce rapid neutron-capture process (r-process) elements up to Th and U, but the timescales are too long to explain observations at low metallicities. The observed evolutionary trends, such as for Eu, can well be explained if ~3% of 25-50 M_\odot hypernovae are magneto-rotational supernovae producing r-process elements. Along with the solar neighborhood, we also predict the evolutionary trends in the halo, bulge, and thick disk for future comparison with galactic archaeology surveys.
282 citations
Liverpool John Moores University1, Max Planck Society2, California Institute of Technology3, University of California, Santa Cruz4, Goddard Space Flight Center5, University of Copenhagen6, University of Maryland, College Park7, Indian Institute of Science8, Indian Institute of Astrophysics9, Konan University10, University of Tokyo11, Tohoku University12, National Autonomous University of Mexico13, Florida State University14, Indian Institute of Technology Bombay15, University of California, Berkeley16, Arizona State University17, Stockholm University18, San Diego State University19, Tokyo Institute of Technology20, Kyoto University21, National Central University22, Soka University of America23, INAF24, National University of Singapore25
TL;DR: In this article, the spectrum remains extremely hot throughout its evolution, and the photospheric radius contracts with time (receding below R <10^14 cm after 1 month).
Abstract: Wide-field optical surveys have begun to uncover large samples of fast (t_rise 10 days. The spectrum remains extremely hot throughout its evolution, and the photospheric radius contracts with time (receding below R<10^14 cm after 1 month). This behavior does not match that of any known supernova, although a relativistic jet within a fallback supernova could explain some of the observed features. Alternatively, the transient could originate from the disruption of a star by an intermediate-mass black hole, although this would require long-lasting emission of highly super-Eddington thermal radiation. In either case, AT 2018cow suggests that the population of fast luminous transients represents a new class of astrophysical event. Intensive follow-up of this event in its late phases, and of any future events found at comparable distance, will be essential to better constrain their origins.
148 citations
Cites background from "Handbook of Supernovae"
...Most corecollapse SNe are believed to exhibit an early shock-breakout and shock-cooling phase in which the stellar photosphere is nearly-instantaneously heated to X-ray temperatures by the emergence of the SN shock, producing a rapid rise in the light curve (Waxman & Katz 2017)....
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University of Southampton1, University of Queensland2, University of California, Santa Cruz3, Swinburne University of Technology4, University of Pennsylvania5, University of Chicago6, Australian Astronomical Observatory7, University of Sydney8, Australian National University9, University of Portsmouth10, Chinese Academy of Sciences11, Rhodes University12, University College London13, Fermilab14, SLAC National Accelerator Laboratory15, Stanford University16, University of Illinois at Urbana–Champaign17, National Center for Supercomputing Applications18, IFAE19, Spanish National Research Council20, California Institute of Technology21, Steward Health Care System22, Autonomous University of Madrid23, ETH Zurich24, Ohio State University25, Harvard University26, University of São Paulo27, Brandeis University28, State University of Campinas29, Oak Ridge National Laboratory30, University of Michigan31
TL;DR: In this article, the results of a search for rapidly evolving transients in the Dark Energy Survey Supernova Programme were presented, including 72 events, including 37 transients with a spectroscopic redshift from host galaxy spectral features.
Abstract: We present the results of a search for rapidly evolving transients in the Dark Energy Survey Supernova Programme. These events are characterized by fast light-curve evolution (rise to peak in≲10 d and exponential decline in≲30 d after peak).We discovered 72 events, including 37 transients with a spectroscopic redshift from host galaxy spectral features. The 37 events increase the total number of rapid optical transients by more than a factor of two. They are found at a wide range of redshifts (0.05 M > -22.25). The multiband photometry is well fit by a blackbody up to few weeks after peak. The events appear to be hot (T ≈ 10 000-30 000 K) and large (R ≈ 10 - 2 × 10 cm) at peak, and generally expand and cool in time, though some events show evidence for a receding photosphere with roughly constant temperature. Spectra taken around peak are dominated by a blue featureless continuum consistent with hot, optically thick ejecta. We compare our events with a previously suggested physical scenario involving shock breakout in an optically thick wind surrounding a core-collapse supernova, we conclude that current models for such a scenario might need an additional power source to describe the exponential decline. We find that these transients tend to favour star-forming host galaxies, which could be consistent with a core-collapse origin. However, more detailed modelling of the light curves is necessary to determine their physical origin.
130 citations
TL;DR: In this article, the authors presented multidimensional hydrodynamical studies of explosions and associated nucleosynthesis in near-Chandrasekhar-mass carbon-oxygen (CO) white dwarfs (WDs) for a wide range of parameters.
Abstract: Recent observations of Type Ia supernovae (SNe Ia) have shown diversified properties of the explosion strength, light curves, and chemical composition. To investigate possible origins of such diversities in SNe Ia, we have presented multidimensional hydrodynamical studies of explosions and associated nucleosynthesis in near-Chandrasekhar-mass carbon–oxygen (CO) white dwarfs (WDs) for a wide range of parameters. In the present paper, we extend our wide parameter survey of models to the explosions of sub-Chandrasekhar-mass CO WDs. We take the double-detonation model for the explosion mechanism. The model parameters of the survey include a metallicity of Z = 0–5 Z⊙, a CO WD mass of M = 0.90–1.20 M⊙, and a He envelope mass of M_(He) = 0.05–0.20 M⊙. We also study how the initial He detonation configuration, such as spherical, bubble, and ring shapes, triggers the C detonation. For these parameters, we derive the minimum He envelope mass necessary to trigger the C detonation. We then examine how the explosion dynamics and associated nucleosynthesis depend on these parameters, and we compare our results with the previous representative models. We compare our nucleosynthesis yields with the unusual abundance patterns of Fe-peak elements and isotopes observed in SNe Ia SN 2011fe, SN 2012cg, and SN 2014J, as well as SN Ia remnant 3C 397, to provide constraints on their progenitors and environments. We provide the nucleosynthesis yields table of the sub-Chandrasekhar-mass explosions, to discuss their roles in the galactic chemical evolution and archaeology.
119 citations
TL;DR: Lamberts et al. as mentioned in this paper presented the first combination of a high-resolution cosmological simulation of a Milky Way-mass galaxy with a binary population synthesis model in this context, which provided a cosmologically realistic star formation history for the galaxy, its stellar halo, and satellites.
Abstract: Author(s): Lamberts, A; Garrison-Kimmel, S; Hopkins, PF; Quataert, E; Bullock, JS; Faucher-Giguere, CA; Wetzel, A; Keres, D; Drango, K; Sanderson, RE | Abstract: Binary black holes are the primary endpoint of massive stars. Their properties provide a unique opportunity to constrain binary evolution, which remains poorly understood. We predict the main properties of binary black holes and their merger products in/around the Milky Way. We present the first combination of a high-resolution cosmological simulation of a Milky Way-mass galaxy with a binary population synthesis model in this context. The hydrodynamic simulation, taken from the FIRE project, provides a cosmologically realistic star formation history for the galaxy, its stellar halo, and satellites. During post-processing, we apply a metallicity-dependent evolutionary model to the star particles to produce individual binary black holes. We find that 7 × 105 binary black holes have merged in the model Milky Way, and 1.2 × 106 binaries are still present, with a mean mass of 28M⊙. Because the black hole progenitors are strongly biased towards low-metallicity stars, half reside in the stellar halo and satellites and a third were formed outside the main galaxy. The numbers and mass distribution of the merged systems is broadly compatible with the LIGO/Virgo detections. Our simplified binary evolution models predict that LISA will detect more than 20 binary black holes, but that electromagnetic observations will be challenging. Our method will allow for constraints on the evolution of massive binaries based on comparisons between observations of compact objects and the predictions of varying binary evolution models. We provide online data of our star formation model and binary black hole distribution.
93 citations