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Journal articles on the topic 'Supernovae: individual (SN 1987A)'

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Published: 4 June 2021

Last updated: 1 February 2022

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1

Liljegren, S., A. Jerkstrand, and J. Grumer. "Carbon monoxide formation and cooling in supernovae." Astronomy & Astrophysics 642 (October 2020): A135. http://dx.doi.org/10.1051/0004-6361/202038116.

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Context. The inclusion of molecular physics is an important piece that tends to be missing from the puzzle when modeling the spectra of supernovae (SNe). Molecules have both a direct impact on the spectra, particularly in the infrared, and an indirect one as a result of their influence on certain physical conditions, such as temperature. Aims. In this paper, we aim to investigate molecular formation and non-local thermodynamic equilibrium (NLTE) cooling, with a particular focus on CO, the most commonly detected molecule in supernovae. We also aim to determine the dependency of supernova chemis

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2

Cappellaro, Enrico. "The Rate of Supernovae in Normal Galaxies." Symposium - International Astronomical Union 171 (1996): 81–84. http://dx.doi.org/10.1017/s0074180900232191.

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The rate of supernovae (SNe) is a key number linking stellar evolution with galaxy evolution models. Stellar evolution theories predict life times, fates and nucleosysntesis yields of individual stars which are used to predicted the galaxy chemical evolution once the star formation history in the galaxy is known. Constraints to the models are the present chemical content of galaxies but also the present observed SN rate (Arimoto & Yoshi, 1987; Ferrini & Poggianti, 1993; Matteucci, 1994; Renzini et al., 1993; Bressan et al., 1994; Elbaz et al., 1995).

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Alexeyeva, L. N. "Neutrinos: Detection and Interpretation." Highlights of Astronomy 8 (1989): 229–37. http://dx.doi.org/10.1017/s1539299600007838.

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AbstractObservations of the neutrino burst from Supernova 1987A by water Cherenkov detectors (KAMIOKANDE II, IMB) and liquid scintillator detectors (Baksan, Mont Blanc) are reviewed. It is shown that neutrino signal from SN 1987A was observed. There are 24 events in three detectors (KAMIOKANDE II, IMB, Baksan) recorded at 7:35 UT. The average properties of the signal (effective neutrino temperature, total energy of neutrino emission, burst duration) are consistent with the general theoretical description of supernova explosions. Special attention is concentrated on individual characteristics o

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Dopita, Michael A. "SN 1987A: an Overview." Publications of the Astronomical Society of Australia 7, no. 4 (1988): 344–51. http://dx.doi.org/10.1017/s1323358000022451.

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5

Chevalier, R. A. "Type II Supernovae SN 1987A and SN 1993J." Science 276, no. 5317 (1997): 1374–78. http://dx.doi.org/10.1126/science.276.5317.1374.

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6

Fu, Albert. "Simple Perspectives on SN 1987A." Publications of the Astronomical Society of Australia 7, no. 4 (1988): 505–12. http://dx.doi.org/10.1017/s1323358000022700.

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AbstractThis conference has shown that the accumulated wealth of data on SN 1987A has enabled us to learn an unprecedented amount of physical information about a single supernova event and supernovae in general, as well as to confirm much of the heretofore established theory. While some difficult problems remain, I discuss some particularly simple and useful theoretical notions concerning the bolometric and γ-ray light curves which can be gleaned from our current body of knowledge, drawing primarily upon results of analytic work performed by W.D. Arnett and myself. Also, the work of Lamb, Meli

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Lundqvist, P., and C. Fransson. "The Circumstellar Structure Around Supernovae." International Astronomical Union Colloquium 101 (1988): 15–18. http://dx.doi.org/10.1017/s0252921100102039.

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AbstractThe time dependent ionization and temperature structure of the circumstellar medium around supernovae has been calculated, in order to interpret recent supernova radio observations. For a stellar wind origin of the circumstellar medium, we relate the time of radio turn-on to the progenitor mass loss rate. We also show that large column densities for the UV resonance lines are expected. The results are applied to SN 1979c, SN 1980k and SN 1987A.

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Filippenko, Alexei V. "Taxonomy of Supernovae." Publications of the Astronomical Society of Australia 7, no. 4 (1988): 540–47. http://dx.doi.org/10.1017/s132335800002275x.

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AbstractI review the observed properties of supernovae (SNe), concentrating on recent results obtained from high-quality optical spectra. Although most SNe Ia have similar characteristics at comparable phases, there are some notable variations, particularly in the velocities of the ejecta. Moreover, there is very preliminary evidence for significant differences between the spectra of SNe Ia in H II regions and in elliptical galaxies. SNe II exhibit a wide range of spectral properties, as expected if they are produced by massive stars. At late times strong lines of [O I] and [Ca II] appear in m

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van den Bergh, Sidney, and R. D. McClure. "The intrinsic frequency of faint supernovae resembling SN 1987A." Astrophysical Journal 347 (December 1989): L29. http://dx.doi.org/10.1086/185599.

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10

Wood, K. S., and P. F. Michelson. "Delayed gravity wave emission from supernovae: application to SN 1987A." Monthly Notices of the Royal Astronomical Society 232, no. 2 (1988): 225–37. http://dx.doi.org/10.1093/mnras/232.2.225.

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11

Itoh, Hiroshi, Kuniaki Masai, and Ken’ichi Nomoto. "The X-ray Emission from SN 1987A and the Remnant of SN 1572 (Tycho)." International Astronomical Union Colloquium 101 (1988): 149–52. http://dx.doi.org/10.1017/s0252921100102271.

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AbstractThe thermal X-ray emission from SN 1987A may be enhanced to a detectable level when the blast shock hits the circumstellar medium which has formed in the red-supergiant stage of the progenitor.The X-ray spectrum of Tycho observed with the satellite Tenma can be explained approximately within the context of a carbon deflagration model for Type la supernovae, if the ejecta are assumed to be mixed partially.

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12

Nomoto, K., T. Shigeyama, and T. Tsujimoto. "Supernova Abundance Generation." Symposium - International Astronomical Union 145 (1991): 21–38. http://dx.doi.org/10.1017/s007418090022723x.

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Theoretical models of supernova explosions of various types are reviewed to obtain heavy element yields from supernovae. We focus on new models for SN 1987A, and Type Ia, Ib, and Ic supernovae. Maximum brightness and decline rate of their light curves suggest that 12–18 M⊙ stars produce larger amount of 56Ni than more massive stars. We discuss relative roles of various types of supernovae in the chemical evolution of galaxies.

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13

McCray, Richard. "Understanding the Nebular Spectrum of SN 1987A." International Astronomical Union Colloquium 145 (1996): 223–34. http://dx.doi.org/10.1017/s0252921100008095.

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The nebular spectra of supernovae differ from those of better-known emission nebulae in that many of the emission lines are optically thick. Here we sketch the theory for interpreting such spectra, and show how it can be used to interpret prominent emission line systems in the spectrum of SN 1987A. As examples, we describe: (1) a simple method to infer the density of OI from observations of the evolution of the doublet ratio in [O I]λλ6300; (2) new kind of hydrogen recombination hne spectrum; (3) an analysis showing that the Call infrared emission lines must come from primordial, not newly-syn

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Lucy, L. B., I. J. Danziger, C. Gouiffes, and P. Bouchet. "Dust Condensation in the Ejecta of SN 1987A." International Astronomical Union Colloquium 120 (1989): 164–79. http://dx.doi.org/10.1017/s025292110002368x.

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AbstractAn asymmetry of optical emission lines that appeared in Sept. 1988 is interpreted as evidence of dust condensation within the metal-rich ejecta of SN 1987A. A quantitative analysis of this spectroscopic effect is given and shown to be compatible with the photometric record. Moreover, observational and theoretical estimates of the bolometric light curve come into agreement when the far-IR excess is interpreted as thermal emission by grains in the ejecta. A grain population comprising small silicate grains with an admixture of graphite or amorphous carbon particles is suggested by the da

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Menon, Athira, and Alexander Heger. "The quest for blue supergiants: Evolution of binary merger progenitors of Type-II peculiar supernovae and SN 1987A." Proceedings of the International Astronomical Union 11, A29B (2015): 460. http://dx.doi.org/10.1017/s1743921316005846.

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AbstractWe construct stellar evolution models until core collapse using KEPLER (Woosley & Heger (2007)) to reproduce the observed signatures of the blue supergiant (BSG) progenitor of SN 1987A. This is based on the binary merger scenario proposed by Podsiadlowski (1992) and Ivanova et al. (2002). Various combinations of initial parameters for the binary components (M1=16–18 M⊙ and M2=5–10 M⊙) and their merging, successfully match the He, N/C and N/O ratios, along with the luminosity and effective temperature of the progenitor. Most of our models end their lives as BSGs. Thus we may be able

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Taddia, Francesco. "The Type II supernovae 2006V and 2006au: two SN 1987A-like events." Proceedings of the International Astronomical Union 7, S279 (2011): 403–4. http://dx.doi.org/10.1017/s1743921312013555.

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AbstractWe studied optical and near-infrared (NIR) light curves, and optical spectra of Supernovae (SNe) 2006V and 2006au, two objects monitored by the Carnegie Supernova Project (CSP) and displaying remarkable similarity to SN 1987A, although they were brighter, bluer and with higher expansion velocities. SN 2006au also shows an initial dip in the light curve, which we have interpreted as the cooling tail of the shock break-out. By fitting semi-analytic models to the UVOIR light curve of each object, we derive the physical properties of the progenitors and we conclude that SNe 2006V and 2006a

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Dessart, Luc, and D. John Hillier. "Supernovae from blue supergiant progenitors: What a mess!" Astronomy & Astrophysics 622 (January 29, 2019): A70. http://dx.doi.org/10.1051/0004-6361/201833966.

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Supernova (SN) 1987A was classified as a peculiar Type II SN because of its long rising light curve and the persistent presence of H I lines in optical spectra. It was subsequently realized that its progenitor was a blue supergiant (BSG), rather than a red supergiant (RSG) as for normal, Type II-P, SNe. Since then, the number of Type II-pec SNe has grown, revealing a rich diversity in photometric and spectroscopic properties. In this study, using a single 15 M⊙ low-metallicity progenitor that dies as a BSG, we have generated explosions with a range of energies and 56Ni masses. We then performe

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Cigan, Phil, Haley Gomez, and Mikako Matsuura. "High-Resolution Observations of Dust in SN 1987A." Proceedings of the International Astronomical Union 12, S331 (2017): 290–93. http://dx.doi.org/10.1017/s1743921317004604.

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AbstractThe dust produced by supernovae is an important topic for understanding supernova physics and the chemical evolution of galaxies. Recent ALMA observations of SN 1987A have allowed us to peer into the inner ejecta to the cool dust, with spatial resolution from 0.″3 at ~300 GHz down to 0.″09 at ~680 GHz – an improvement over the previous 300 GHz Cycle 0 observations at 0.″69. Comparison of the dust location and morphology with other multiwavelength emission presents an interesting picture of the role dust plays in the ejecta. The mm-FIR SED is compared to radiative models to study the du

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Kirshner, Robert P. "Supernova Remnants and their Supernovae." International Astronomical Union Colloquium 101 (1988): 1–14. http://dx.doi.org/10.1017/s0252921100102027.

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AbstractObserving supernova remnants provides important clues to the nature of supernova explosions. Conversely, the late stages of stellar evolution and the mechanism of supernova explosions affect supernova remnants through circumstellar matter, stellar remnants, and nucleosynthesis. The elements of supernova classification and the connection between supernova type and remnant properties are explored. A special emphasis is placed on SN 1987a which provides a unique opportunity to learn the connection between the star that exploded (whose name we know) and the remnant that will develop in our

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Panagia, Nino. "SUPERNOVA 1987A: CELEBRATING A SILVER JUBILEE." Acta Polytechnica 53, A (2013): 606–11. http://dx.doi.org/10.14311/ap.2013.53.0606.

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The story of the SN 1987A explosion is briefly reviewed. Although this supernova was somewhat peculiar, the study of SN 1987A has clarified quite a number of important aspects of the nature and the properties of supernovae, such as the confirmation of the core collapse of a massive star as the cause of the explosion, as well the confirmation that the decays 56Ni–56Co–56Fe at early times and 44Ti–44Sc at late times, are the main sources of the energy radiated by the ejecta. Still we have not been able to ascertain whether the progenitor was a single star or a binary system, nor have we been abl

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Baes, Maarten, Peter Camps, Phil J. Cigan, Christopher L. Fryer, Mikako Matsuura, and Sam Verstocken. "Measuring the dust content and formation in SN 1987A using detailed radiative transfer modelling." Proceedings of the International Astronomical Union 12, S331 (2017): 300–303. http://dx.doi.org/10.1017/s1743921317004562.

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AbstractCore-collapse supernovae are expected to be efficient producers of dust, and recent Herschel and ALMA observations have revealed up to 1 M⊙ of cold dust in the inner ejecta of SN 1987A. The formation time scale, spatial distribution and clumpiness, and the importance of the different heating sources of the dust remain poorly understood. We have started a project to make detailed 3D dust radiative transfer models for SN 1987A, based on a combination of the latest observational constraints and input from 3D hydrodynamical models and dust formation models. Preliminary results seem to indi

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Ray, Alak, Sayan Chakraborti, Naveen Yadav, Randall Smith, Poonam Chandra, and David Pooley. "A tale of two shocks in SN 2004dj." Proceedings of the International Astronomical Union 9, S296 (2013): 108–11. http://dx.doi.org/10.1017/s1743921313009319.

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AbstractType IIP SNe constitute a major fraction of all core-collapse supernovae and arise from massive stars that end their lives close to Red Supergiants. The blastwave from the SN interacting with the progenitor's circumstellar matter produces a hot region bounded by a forward and a reverse shock from which most of the X-ray emission originates. Analysis of archival Chandra observations of SN 2004dj, one of the nearest supernovae since SN 1987A, together with published data from radio and optical bands determines the pre-explosion mass-loss rate, blastwave speed, electron acceleration and m

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Joss, P. C. "Type II Supernovae in Binary Systems." Symposium - International Astronomical Union 165 (1996): 141–49. http://dx.doi.org/10.1017/s0074180900055637.

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The presence of a close binary companion can affect the evolution of a massive star through one or more episodes of mass transfer, or by merger in a common-envelope phase. Monte Carlo calculations indicate that ∼20–35% of all massive supernovae are affected by such processes, and that a substantial fraction of these events will be supernovae of type II. The properties of the progenitor star, the distribution of circumstellar material, the peak supernova luminosity, the shape of the supernova light curve, and other observable features of the supernova event can be affected by prior binary membe

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Kumagai, S. "X-Rays and γ-Rays from SN 1987A". International Astronomical Union Colloquium 145 (1996): 173–81. http://dx.doi.org/10.1017/s0252921100008046.

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Theoretical light curves and spectra of X-rays and γ-rays from SN 1987A are calculated by the Monte Carlo method, based on a model built up from the early observations of neutrinos and optical light. Comparison of the predicted radiation with observational results obtained later confirms the radiation mechanism of supernovae: γ-rays are emitted in the decays of radioactive 56Co and X-rays are generated by the Compton degradation of these γ-rays. It also suggests that large scale mixing occurred and clumpy structure was formed inside the ejecta. These findings lead us to construct the model wit

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Hauschildt, P. H., W. Spies, R. Wehrse, and G. Shaviv. "Calculated Energy Distributions for SN II." International Astronomical Union Colloquium 108 (1988): 412–14. http://dx.doi.org/10.1017/s0252921100094197.

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AbstractWe have calculated a large grid of hydrogen-rich supernova photospheres, in which radii, effective temperatures, density profiles, and expansion velocities have been varied. Spherical geometry, radiative equilibrium and LTE level populations are assumed. In the quasi-exact radiative transfer, the dilution of the radiation field, and scattering as well as absorption (by all relevant continuous processes and up to 150 000 lines in some models) are accurately considered. Good agreement can be obtained with the UV and IR spectra of supernovae 1979C, 1980K, and 1987A as observed during the

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Taddia, F., M. D. Stritzinger, J. Sollerman, et al. "The Type II supernovae 2006V and 2006au: two SN 1987A-like events." Astronomy & Astrophysics 537 (January 2012): A140. http://dx.doi.org/10.1051/0004-6361/201118091.

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Maeda, Keiichi, Yukikatsu Terada, and Aya Bamba. "Expected Hard X-Ray and Soft Gamma-Ray from Supernovae." Acta Polytechnica CTU Proceedings 1, no. 1 (2014): 205–9. http://dx.doi.org/10.14311/app.2014.01.0205.

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High energy emissions from supernovae (SNe), originated from newly formed radioactive species, provide direct evidence of nucleosynthesis at SN explosions. However, observational diculties in the MeV range have so far allowed the signal detected only from the extremely nearby core-collapse SN 1987A. No solid detection has been reported for thermonuclear SNe Ia, despite the importance of the direct conrmation of the formation of <sup>56</sup>Ni, which is believed to be a key ingredient in their nature as distance indicators. In this paper, we show that the new generation hard X-ray

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Matsuura, M., R. Indebetouw, S. Woosley, et al. "ALMA observations of Molecules in Supernova 1987A." Proceedings of the International Astronomical Union 12, S331 (2017): 294–99. http://dx.doi.org/10.1017/s1743921317004719.

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AbstractSupernova (SN) 1987A has provided a unique opportunity to study how SN ejecta evolve in 30 years time scale. We report our ALMA spectral observations of SN 1987A, taken in 2014, 2015 and 2016, with detections of CO, 28SiO, HCO+ and SO, with weaker lines of 29SiO.We find a dip in the SiO line profiles, suggesting that the ejecta morphology is likely elongated. The difference of the CO and SiO line profiles is consistent with hydrodynamic simulations, which show that Rayleigh-Taylor instabilities causes mixing of gas, with heavier elements much more disturbed, making more elongated struc

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Orlando, S., M. Miceli, and O. Petruk. "Bridging the gap between supernovae and their remnants through multi-dimensional hydrodynamic modeling." Proceedings of the International Astronomical Union 12, S331 (2017): 258–67. http://dx.doi.org/10.1017/s1743921317004380.

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AbstractSupernova remnants (SNRs) are diffuse extended sources characterized by a complex morphology and a non-uniform distribution of ejecta. Such a morphology reflects pristine structures and features of the progenitor supernova (SN) and the early interaction of the SN blast wave with the inhomogeneous circumstellar medium (CSM). Deciphering the observations of SNRs might open the possibility to investigate the physical properties of both the interacting ejecta and the shocked CSM. This requires accurate numerical models which describe the evolution from the SN explosion to the remnant devel

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France, Kevin. "Recent Hubble Space Telescope Observations of SN 1987A: Broad Emission Lines." Proceedings of the International Astronomical Union 9, S296 (2013): 1–8. http://dx.doi.org/10.1017/s1743921313009150.

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AbstractObservations with the Hubble Space Telescope (HST), conducted since 1990, have allowed us to create a “movie” of the evolution of the core-collapse supernova SN 1987A from 3–25 years after the explosion. Critical to understanding the late time evolution of SN 1987A was the successful HST Servicing Mission 4 in May 2009. The repair of the STIS instrument and the installation of the WFC3 imager and COS spectrograph have provided crucial data points for understanding the temporal variability in the physical structure and energy sources for SN 1987A, as well as measurements of the chemical

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Wheeler, J. Craig, Robert P. Harkness, and Zalman Barkat. "Spectroscopic Diagnosis of SN1987A and Lesser Lights." International Astronomical Union Colloquium 108 (1988): 305–18. http://dx.doi.org/10.1017/s0252921100094069.

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AbstractSN 1987A gives a unique chance to study both the precursor star and the subsequent dynamical evolution of the explosion. Comparison of the light curves shows that either H0 ∼ 100 km/s/Mpc, or SN 1987A ejected significantly less 56Ni than ordinary Type II supernovae. Investigation of the stellar structure pertinent to SK -69 202 reveals multiple solutions. For given luminosity, effective temperature, core mass and core radius, there are two families of envelope mass, one with large envelope mass and one with small envelope mass. The small envelope mass solutions can be ruled out by cons

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P. Kirshner, Robert. "Supernovae and the Cosmic Distance Scale." International Astronomical Union Colloquium 145 (1996): 19–28. http://dx.doi.org/10.1017/s0252921100007879.

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Knowledge of the size and age of the Universe depends on understanding supernovae. The direct geometric measurement of the circumstellar ring of SN 1987A using IUE spectra and HST images provides an independent test of the Cepheid distance scale to the Large Magellanic Cloud. Understanding the details of the mass distribution in the circumstellar matter is important to improving the precision of this distance. Type la supernovae have a narrow distribution in absolute magnitude, and new Cepheid distances to IC 4182 (the site of SN 1937C) and to NGC 5253 (the site of SN 1972E) obtained with HST

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Menon, Athira, and Alexander Heger. "Blue supergiant progenitors from binary mergers for SN 1987A and other Type II-peculiar supernovae." Proceedings of the International Astronomical Union 12, S329 (2016): 64–68. http://dx.doi.org/10.1017/s1743921317003003.

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AbstractWe present results of a systematic and detailed stellar evolution study of binary mergers for blue supergiant (BSG) progenitors of Type II supernovae, particularly for SN 1987A. We are able to reproduce nearly all observational aspects of the progenitor of SN 1987A, Sk –69 °202, such as its position in the HR diagram, the enrichment of helium and nitrogen in the triple-ring nebula and its lifetime before its explosion. We build our evolutionary model based on the merger model of Podsiadlowski et al. (1992), Podsiadlowski et al. (2007) and empirically explore an initial parameter consis

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Kotak, Rubina. "Core-Collapse Supernovae as Dust Producers." Proceedings of the International Astronomical Union 3, S250 (2007): 437–42. http://dx.doi.org/10.1017/s1743921308020802.

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AbstractAlthough it has long been hypothesised that core-collapse supernovae may produce large quantities of dust, interest in this problem has recently been rekindled given the enormous dust masses inferred at very high redshifts (z ≳ 6), when conventional low-mass dust-producing stars would fail to contribute significantly to the universal dust budget. Emission due to warm dust peaks at mid-IR wavelengths. However, with the notable exception of SN 1987A, supernova studies in the mid-IR have been virtually non-existent until the advent of the Spitzer Space Telescope. On behalf of the Mid-Infr

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Pettini, M. "AAT Observations of the Interstellar Medium towards SN 1987A." Publications of the Astronomical Society of Australia 7, no. 4 (1988): 527–34. http://dx.doi.org/10.1017/s1323358000022736.

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AbstractThe exceptional brightness of SN 1987A has provided a unique opportunity to probe intervening gas clouds in the disk and halo of our Galaxy and in the Large Magellanic Cloud, as well as intergalactic matter between the two. At the AAO we have exploited this opportunity in two ways: in searches for very weak interstellar features requiring exceptionally high signal-to-noise ratio spectra, and in recording known interstellar lines with unprecedentedly high spectral resolution. We are also monitoring photographically the evolution of the light-echoes to map the three-dimensional distribut

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Nozawa, Takaya. "Mass of dust in core-collapse supernovae as viewed from energy balance in the ejecta." Proceedings of the International Astronomical Union 12, S329 (2016): 431. http://dx.doi.org/10.1017/s1743921317001582.

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AbstractRecent far-infrared (FIR) observations have revealed the presence of freshly formed dust with the masses exceeding 0.1 M⊙ in young remnants of core-collapse supernovae (CCSNe) such as SN 1987A and Cassiopeia A. Meanwhile, dust masses derived from near- to mid-infrared (N/MIR) observations of CCSNe a few years after explosions are on the order of 10−5–10−3M⊙. Here, we demonstrate that such small dust masses as seen from N/MIR observations would not necessarily reflect the formation history of dust but could be just limited by the luminosity of the SN that can heat up dust formed in the

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Martellini, Cristina, Stefano Maria Mari, Paolo Montini, and Giulio Settanta. "Towards a reconstruction of Supernova Neutrino Spectra in JUNO." EPJ Web of Conferences 209 (2019): 01012. http://dx.doi.org/10.1051/epjconf/201920901012.

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Observation of supernovae (SN) through their neutrino emission is a fundamental point to understand both SN dynamics and neutrino physical properties. JUNO is a 20kton liquid scintillator detector, under construction in Jiangmen, China. The main aim of the experiment is to determine neutrino mass hierarchy by precisely measuring the energy spectrum of reactor electron antineutrinos. However due to its properties, JUNO has the capability of detecting a high statistics of SN events too. Existing data from SN neutrino consists only of 24 events coming from the SN 1987A,the detection of a SN burst

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Chevalier, R. A. "High-energy Emission from Supernovae and Remnants." Symposium - International Astronomical Union 195 (2000): 135–42. http://dx.doi.org/10.1017/s0074180900162874.

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An early burst of energetic radiation is expected from a supernova at the time of shock breakout. This emission has not been directly observed but has been inferred from the photoionization around SN 1987A. X-ray emission has been detected from core-collapse supernovae in the days to years after the explosion as they interact with their circumstellar winds. Young Galactic supernova remnants provide the possibility of determining the composition structure of the ejecta through X-ray spectroscopy. An exciting finding for older remnants is that a number of remnants that appear to be interacting w

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Höflich, Peter A., Dietrich Baade, Alexei M. Khokhlov, Lifan Wang, and J. Craig Wheeler. "Aspherical supernova explosions." Symposium - International Astronomical Union 212 (2003): 387–94. http://dx.doi.org/10.1017/s0074180900212473.

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Core collapse supernovae (SN) are the final stages of stellar evolution in massive stars during which the central region collapses, forms a neutron star (NS), and the outer layers are ejected. Recent explosion scenarios assumed that the ejection is due to energy deposition by neutrinos into the envelope, but detailed models do not produce powerful explosions. There is new and mounting evidence for an asphericity and, in particular, for axial symmetry in several supernovae which may be hard to reconcile within the spherical picture. This evidence includes the observed high polarization and its

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Janka, Hans-Thomas, Michael Gabler, and Annop Wongwathanarat. "Spatial distribution of radionuclides in 3D models of SN 1987A and Cas A." Proceedings of the International Astronomical Union 12, S331 (2017): 148–56. http://dx.doi.org/10.1017/s1743921317004549.

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AbstractFostered by the possibilities of multi-dimensional computational modeling, in particular the advent of three-dimensional (3D) simulations, our understanding of the neutrino-driven explosion mechanism of core-collapse supernovae (SNe) has experienced remarkable progress over the past decade. First self-consistent, first-principle models have shown successful explosions in 3D, and even failed cases may be cured by moderate changes of the microphysics inside the neutron star (NS), better grid resolution, or more detailed progenitor conditions at the onset of core collapse, in particular l

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Craig Wheeler, J., and Alexei V. Filippenko. "Review of Contributions to the Workshop on SN1993J." International Astronomical Union Colloquium 145 (1996): 241–76. http://dx.doi.org/10.1017/s0252921100008113.

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At its peak, SN 1993J was one of the brightest supernovae in this century, and it is being studied more thoroughly than any supernova except SN 1987A. It is proving to be similar to the transition object SN 1987K, which metamorphosed from being a hydrogen-rich Type II near peak to having a hydrogen-deficient nebular phase. SN 1993J has been observed throughout the electromagnetic spectrum and with optical spectropolarimetry. It is interacting with a dense circumstellar nebula and is generating radio and X-ray flux, but it has probably not been detected in gamma rays. The photometric and spectr

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Orellana, Mariana, Melina C. Bersten, and Takashi J. Moriya. "Systematic study of magnetar-powered hydrogen-rich supernovae." Astronomy & Astrophysics 619 (November 2018): A145. http://dx.doi.org/10.1051/0004-6361/201832661.

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Context. It has been suggested that some supernovae (SNe) may be powered by a magnetar formed at the moment of the explosion. While this scenario has mostly been applied to hydrogen-free events, it may also be possible for hydrogen-rich objects. Aims. We aim to explore the effect of including a magnetar on the light curves of supernovae with H-rich progenitors. Methods. We have applied a version of our one-dimensional local thermodynamic equilibrium radiation hydrodynamics code that takes into account the relativistic motion of the ejecta caused by the extra energy provided by the magnetar. Fo

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Ertl, Thomas. "The Progenitor-Remnant Connection of Neutrino-Driven Supernovae Across the Stellar Mass Range." Proceedings of the International Astronomical Union 12, S329 (2016): 74–77. http://dx.doi.org/10.1017/s1743921317001843.

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AbstractWe perform hydrodynamic supernova (SN) simulations in spherical symmetry for progenitor models with solar metallicity across the stellar mass range from 9.0 to 120 M⊙ to explore the progenitor-explosion and progenitor-remnant connections based on the neutrino-driven mechanism. We use an approximative treatment of neutrino transport and replace the high-density interior of the neutron star (NS) by an inner boundary condition based on an analytic proto-NS core-cooling model, whose free parameters are chosen to reproduce the observables of SN 1987A and the Crab SN for theoretical models o

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Dwek, Eli. "Infrared Emission from Dust in Supernovae and Supernova Remnants." Symposium - International Astronomical Union 135 (1989): 479–86. http://dx.doi.org/10.1017/s0074180900125471.

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The need to replenish the reservoir of interstellar dust grains that are continuously being destroyed in the interstellar medium, and the presence of isotopic anomalies in meteorites, suggest that supernovae may be important sources of interstellar dust. Infrared observations of supernovae or their unmixed ejecta may provide the first direct evidence for newly-formed grains in this environment. The recently discovered supernova, SN 1987A, currently offers the best prospects for observing the actual process of dust formation in a supernova.In contrast, supernova remnants constitute the most imp

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KRIVOSHEINA, I. V. "SN 1987A — HISTORICAL VIEW ABOUT REGISTRATION OF THE NEUTRINO SIGNAL WITH BAKSAN, KAMIOKANDE II AND IMB DETECTORS." International Journal of Modern Physics D 13, no. 10 (2004): 2085–105. http://dx.doi.org/10.1142/s0218271804006607.

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The detection of neutrinos from SN 1987A opened a new era in neutrino astrophysics in the last century. We present a historical view about registration of the neutrino signal from supernova SN 1987A in the Large Magellanic Cloud by the BAKSAN liquid scintillator detector and by the two water Cherenkov detectors — Kamiokande-II and IMB. All three detectors observed a total neutrino signal of 24 events at 7:35 UT 23 February, 1987. I will concentrate mostly about the BAKSAN supernova group analysis of the neutrino signal, which was already done in the years 1987 and 1988. The results of this ana

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Blum, Kfir, and Doron Kushnir. "NEUTRINO SIGNAL OF COLLAPSE-INDUCED THERMONUCLEAR SUPERNOVAE: THE CASE FOR PROMPT BLACK HOLE FORMATION IN SN 1987A." Astrophysical Journal 828, no. 1 (2016): 31. http://dx.doi.org/10.3847/0004-637x/828/1/31.

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NADYOZHIN, D. K., and V. S. IMSHENNIK. "PHYSICS OF SUPERNOVAE." International Journal of Modern Physics A 20, no. 29 (2005): 6597–611. http://dx.doi.org/10.1142/s0217751x05029630.

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The origin of cosmic rays (CR) is supposed to be closely connected with supernovae (SNe) which create the conditions favorable for various mechanisms of the CR acceleration to operate effectively. First, modern ideas about the physics of the SN explosion are briefly discussed: the explosive thermonuclear burning in degenerate white dwarfs resulting in Type Ia SNe and the gravitational collapse of stellar cores giving rise to other types of SNe (Ib, Ic, IIL, IIP). Next, we survey some global properties of the SNe of different types: the total explosion energy distribution of various components

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Perego, A., M. Hempel, C. Fröhlich, et al. "PUSHING CORE-COLLAPSE SUPERNOVAE TO EXPLOSIONS IN SPHERICAL SYMMETRY. I. THE MODEL AND THE CASE OF SN 1987A." Astrophysical Journal 806, no. 2 (2015): 275. http://dx.doi.org/10.1088/0004-637x/806/2/275.

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Chechetkin, V. M., A. A. Denisov, A. V. Koldoba, Yu A. Poveschenko, and Yu P. Popov. "Asymmetrical Ejection of Matter in a Thermonuclear Model of a Supernova Explosion." International Astronomical Union Colloquium 101 (1988): 27–30. http://dx.doi.org/10.1017/s0252921100102064.

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With the recent Supernova 1987a in the LMC, new and interesting possibilities have arisen for the solution of a problem relating to the explosion mechanism of supernovae. The presupernova was probably a B3Ia, the blue supergiant, and not a red giant as it was earlier thought likely. Calculations of the evolution, which have been made recently, show that the loss of hydrodynamical stability may be connected with carbon burning in the stellar core during the blue giant stage. This loss of stability of the CO core is the main factor in our explanation of the recent event of SN 1987a.Before we con

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Alp, Dennis, Josefin Larsson, Keiichi Maeda, et al. "X-Ray and Gamma-Ray Emission from Core-collapse Supernovae: Comparison of Three-dimensional Neutrino-driven Explosions with SN 1987A." Astrophysical Journal 882, no. 1 (2019): 22. http://dx.doi.org/10.3847/1538-4357/ab3395.

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