Journal articles on the topic 'Supernovae'
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1
Arcavi, Iair. "Type II SN Light Curves from the Caltech Core Collapse Project." Proceedings of the International Astronomical Union 7, S285 (September 2011): 431–53. http://dx.doi.org/10.1017/s1743921312001329.
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We presented our analysis of a sample of type II supernova (SN) light curves measured by the Caltech Core Collapse Project (CCCP). CCCP is a large observational program which made use of the robotic 60-in and the Hale 200-in telescopes to obtain optical photometry, spectroscopy and IR photometry of 49 nearby core-collapse supernovae (SNe). It provides a fair sample of core-collapse events, with well-defined selection criteria, and uniform, high-quality optical/IR observations. Our goal is to characterize the little-studied properties of core-collapse supernovae as a population. Preliminary data indicate a diverse set of sub-populations including “standard” type IIP supernovæ, declining supernovæ (at different rates) and slowly rising peculiar supernovæ. Work is in progress to map and quantify that diversity better. It is hoped that a single tunable formula will be able to describe most light-curve shapes, thereby helping us attain a better understanding of the physical mechanisms underlying these results.
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Nomoto, Ken'ichi. "Core Collapse Supernova Models and Nucleosynthesis." Proceedings of the International Astronomical Union 9, S296 (January 2013): 27–36. http://dx.doi.org/10.1017/s1743921313009198.
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AbstractAfter the Big Bang, production of heavy elements in the early Universe takes place in the first stars and their supernova explosions. The nature of the first supernovae, however, has not been well understood. The signature of nucleosynthesis yields of the first supernovae can be seen in the elemental abundance patterns observed in extremely metal-poor stars. Interestingly, those abundance patterns show some peculiarities relative to the solar abundance pattern, which should provide important clues to understanding the nature of early generations of supernovae. We review the recent results of the nucleosynthesis yields of massive stars. We examine how those yields are affected by some hydrodynamical effects during the supernova explosions, namely, explosion energies from those of hypernovae to faint supernovae, mixing and fallback of processed materials, asphericity, etc. Those parameters in the supernova nucleosynthesis models are constrained from observational data of supernovae and metal-poor stars.
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Wang, Lifan, Dietrich Baade, and Ferdinando Patat. "Spectropolarimetric Diagnostics of Thermonuclear Supernova Explosions." Science 315, no. 5809 (November 30, 2006): 212–14. http://dx.doi.org/10.1126/science.1121656.
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Even at extragalactic distances, the shape of supernova ejecta can be effectively diagnosed by spectropolarimetry. We present results for 17 type Ia supernovae that allow a statistical study of the correlation among the geometric structures and other observable parameters of type Ia supernovae. These observations suggest that type Ia supernova ejecta typically consist of a smooth, central, iron-rich core and an outer layer with chemical asymmetries. The degree of this peripheral asphericity is correlated with the light-curve decline rate of type Ia supernovae. These results lend strong support to delayed-detonation models of type Ia supernovae.
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Murphey, C. Tanner, Jacob W. Hogan, Brian D. Fields, and Gautham Narayan. "Witnessing history: sky distribution, detectability, and rates of naked-eye Milky Way supernovae." Monthly Notices of the Royal Astronomical Society 507, no. 1 (July 29, 2021): 927–43. http://dx.doi.org/10.1093/mnras/stab2182.
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ABSTRACT The Milky Way hosts on average a few supernova explosions per century, yet in the past millennium only five supernovae have been identified confidently in the historical record. This deficit of naked-eye supernovae is at least partly due to dust extinction in the Galactic plane. We explore this effect quantitatively, developing a formalism for the supernova probability distribution in space and on the sky, accounting for dust and for the observer’s flux limit. We then construct a fiducial axisymmetric model for the spatial supernova and dust densities, featuring an exponential dependence on galactocentric radius and height, with core-collapse events in a thin disc and Type Ia events including a thick disc component. When no flux limit is applied, our model predicts that on the sky, supernovae are intrinsically concentrated in the Galactic plane, with Type Ia events extending to higher latitudes. We then apply a flux limit and include dust effects, to predict the sky distribution of historical supernovae. We use well-observed supernovae as light-curve templates, and introduce naked-eye discovery criteria. The resulting sky distributions are strikingly inconsistent with the locations of confident historical supernovae, none of which lie near our model’s central peaks. Indeed, SN 1054 lies off the plane almost exactly in the anticentre, and SN 1181 is in the second Galactic quadrant. We discuss possible explanations for these discrepancies. We calculate the percentage of all supernovae bright enough for historical discovery: $\simeq 13{{\ \rm per\ cent}}$ of core-collapse and $\simeq 33{{\ \rm per\ cent}}$ of Type Ia events. Using these and the confident historical supernovae, we estimate the intrinsic Galactic supernova rates, finding general agreement with other methods. Finally, we urge searches for supernovae in historical records from civilizations in the Southern hemisphere.
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Weiler, Kurt W., and Richard A. Sramek. "Supernovae and Supernova Remnants." Annual Review of Astronomy and Astrophysics 26, no. 1 (September 1988): 295–341. http://dx.doi.org/10.1146/annurev.aa.26.090188.001455.
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Green, D. A. "Historical Supernovae and their Remnants." Highlights of Astronomy 12 (2002): 350–53. http://dx.doi.org/10.1017/s1539299600013721.
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AbstractHistorical records are available for nine supernova explosions seen in our Galaxy over the last two millennia. The observations of these ‘historical’ supernovae are very useful for the modern astrophysical interpretation of the remnants of these supernovae. The ages of the remnants of these historical supernovae are definitively known, which greatly aids understanding of the nature of the remnants. Also, the fact that the parent supernova was seen implies that it was relatively nearby in the Galaxy, giving further constraints on the distance, and hence other properties of their remnants. Here I briefly review the historical supernovae in our Galaxy, in the context of our understanding of their remnants from modern observations.
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Waldman, Roni. "Around the Pair Instability Valley – Massive SN Progenitors." Proceedings of the International Astronomical Union 4, S252 (April 2008): 329–32. http://dx.doi.org/10.1017/s1743921308023120.
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AbstractThe discovery of the extremely luminous supernova SN 2006gy, possibly interpreted as a pair instability supernova, renewed the interest in very massive stars. We explore the evolution of these objects, which end their life as pair instability supernovae or as core collapse supernovae with relatively massive iron cores, up to about 3 M⊙.
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Nomoto, Ken'ichi, and Tomoharu Suzuki. "Supernova Yields for Chemical Evolution Modeling." Proceedings of the International Astronomical Union 9, S298 (May 2013): 154–66. http://dx.doi.org/10.1017/s1743921313006327.
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AbstractWe review the recent results of the nucleosynthesis yields of massive stars. We examine how those yields are affected by some hydrodynamical effects during the supernova explosions, namely, explosion energies from those of hypernovae to faint supernovae, mixing and fallback of processed materials, asphericity, etc. Those parameters in the supernova nucleosynthesis models are constrained from observational data of supernovae and metal-poor stars. The elemental abundance patterns observed in extremely metal-poor stars show some peculiarities relative to the solar abundance pattern, which suggests the important contributions of hypernovae and faint supernovae in the early chemical enrichment of galaxies. These constraints on supernova nucleosynthesis are taken into account in the latest yield table for chemical evolution modeling.
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Abe, S., S. Asami, M. Eizuka, S. Futagi, A. Gando, Y. Gando, T. Gima, et al. "Search for Supernova Neutrinos and Constraint on the Galactic Star Formation Rate with the KamLAND Data." Astrophysical Journal 934, no. 1 (July 1, 2022): 85. http://dx.doi.org/10.3847/1538-4357/ac7a3f.
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Abstract We present the results of a search for core-collapse supernova neutrinos, using long-term KamLAND data from 2002 March 9 to 2020 April 25. We focus on the electron antineutrinos emitted from supernovae in the energy range of 1.8–111 MeV. Supernovae will make a neutrino event cluster with the duration of ∼10 s in the KamLAND data. We find no neutrino clusters and give the upper limit on the supernova rate to be 0.15 yr−1 with a 90% confidence level. The detectable range, which corresponds to a >95% detection probability, is 40–59 kpc and 65–81 kpc for core-collapse supernovae and failed core-collapse supernovae, respectively. This paper proposes to convert the supernova rate obtained by the neutrino observation to the Galactic star formation rate. Assuming a modified Salpeter-type initial mass function, the upper limit on the Galactic star formation rate is <(17.5–22.7) M ⊙ yr−1 with a 90% confidence level.
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Gomez, H. L., S. A. Eales, and L. Dunne. "Smoking supernovae." International Journal of Astrobiology 6, no. 2 (February 28, 2007): 159–67. http://dx.doi.org/10.1017/s1473550407003552.
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AbstractThe question ‘Are supernovae important sources of dust?’ is a contentious one. Observations with the Infrared Astronomical Satellite (IRAS) and the Infrared Space Observatory (ISO) only detected very small amounts of hot dust in supernova remnants. Here, we review observations of two young Galactic remnants with the Submillimetre Common User Bolometer Array (SCUBA), which imply that large quantities of dust are produced by supernovae. The association of dust with the Cassiopeia A remnant is in question owing to the contamination of foreground material. In this paper, we compare the emission from cold dust with CO emission towards Kepler’s supernova remnant. We detect very little CO at the location of the submillimetre peaks. A comparison of masses from the CO and the dust clouds are made, and we estimate the 3σ upper limit on the gas-to-dust ratios to be in the range 20–60. These results suggest that we cannot yet rule out freshly-formed or swept-up circumstellar dust in Kepler’s supernova remnant.
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Winkler, P. Frank, and Wolfgang Hillebrandt. "Joint Discussion 9 Supernovae: one millennium after SN 1006." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 299–300. http://dx.doi.org/10.1017/s1743921307010691.
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The year 2006 marks the 1000th anniversary of the supernova of 1006 C.E., the brightest supernova in all of recorded human history. This is also a time of great excitement in the supernova community: Observations from space observatories including Hubble, Chandra, XMM-Newton, and Spitzer, together with ones from powerful new ground-based telescopes and instruments, are revealing supernova remnants in the Galaxy and beyond in unprecedented detail. Fully three-dimensional computational codes and simulations running on powerful new machines are providing insight into the physics of supernovae freed from the simplifying assumptions that have restricted past understanding. Automated supernova searches are discovering hundreds of new supernovae every year, some at redshifts of 1 or beyond. And supernovae have revolutionized cosmology through the discovery of an accelerating universe, and they hold promise for deepening our understanding of the ‘dark energy’ that drives the acceleration.
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Daishido, T., K. Asuma, S. Inoue, K. Nishibori, H. Ohara, S. Komatsu, and K. Nagane. "Radio Patrol Camera for Supernovae Search." International Astronomical Union Colloquium 108 (1988): 458–59. http://dx.doi.org/10.1017/s0252921100094410.
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Zwicky started extragalactic supernovae patrol using 10 inch Schmidt camera about fifty years ago. After that the research of supernovae was accelerated, because the wide view of the Schmidt camera made it possible to watch large field of the sky. The key technology of the Schmidt camera was its sophisticated optical system.Anticipated next supernova in our Galaxy may be undetectable by the optical instrument due to the Galactic extinction. However, supernovae are now known to be intense radio sources after a year or so of the explosion. Even if the positions are beyond the Galactic center, the radio supernova could be observed using middle size radio telescope.
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Quimby, Robert M. "Superluminous Supernovae." Proceedings of the International Astronomical Union 9, S296 (January 2013): 68–76. http://dx.doi.org/10.1017/s1743921313009253.
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AbstractNot long ago the sample of well studied supernovae, which were gathered mostly through targeted surveys, was populated exclusively by events with absolute peak magnitudes fainter than about −20. Modern searches that select supernovae not just from massive hosts but from dwarfs as well have produced a new census with a surprising difference: a significant percentage of supernovae found in these flux limited surveys peak at −21 magnitude or brighter. The energy emitted by these superluminous supernovae in optical light alone rivals the total explosion energy available to typical core collapse supernovae (>1051 erg). This makes superluminous supernovae difficult to explain through standard models. Adding further complexity to this picture are the distinct observational properties of various superluminous supernovae. Some may be powered in part by interactions with a hydrogen-rich, circumstellar material but others appear to lack hydrogen altogether. Some could be powered by large stores of radioactive material, while others fade quickly and have stringent limits on 56-Ni production. In this talk I will discuss the current observational constrains on superluminous supernova and the prospects for revealing their origins.
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Resmi, Lekshmi, and Kuntal Misra. "A comparative study of GRB-Supernovae." Proceedings of the International Astronomical Union 9, S296 (January 2013): 354–55. http://dx.doi.org/10.1017/s1743921313009794.
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AbstractOptical afterglow observations hold the indirect key to type-Ic Supernovae associated with Gamma Ray Bursts. In several cases where there is no spectroscopic confirmation available, presence of the supernova is inferred from the red bump seen in late afterglow light-curves. We do extensive afterglow modeling to extract the supernova contribution as residue. We compare the residual lightcurves of Supernovae associated with GRB041006, GRB030329, GRB050525A and GRB090618.
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Wang, Zhenru. "Historical Supernovae and Supernova Remnants." International Astronomical Union Colloquium 145 (1996): 323–31. http://dx.doi.org/10.1017/s0252921100008174.
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The oldest historical supernova (SN), recorded by ancient Chinese in 14th Century B.C. on pieces of tortoise shells or bones, is identified with the aid of modern space γ-ray observations. Hard X-rays with energy up to 20 keV were observed from IC 443 by the X-ray satellite Ginga. We infer from these observations the age of IC 443 is ∼ 1000 — 1400 yrs. The result supports the hypothesis that IC 443 is the remnant of the historical SN 837 that occurred during the Tang Dynasty. The association between the supernova remnant (SNR) CTB 80 and SN 1408 has been hotly debated for about ten years and is briefly reviewed and discussed here. A new picture is presented to explain this association. High energy emission from historical SNRs can persist in a multiphase interstellar medium (ISM). As a result, the study of the relationship between SNRs and ancient guest stars has gained new vitality.
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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 lifetimes.
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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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Moriya, Takashi J. "Light-curve and spectral properties of ultra-stripped core-collapse supernovae." Proceedings of the International Astronomical Union 12, S329 (November 2016): 426. http://dx.doi.org/10.1017/s1743921317000187.
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AbstractWe discuss light-curve and spectral properties of ultra-stripped core-collapse supernovae. Ultra-stripped supernovae are supernovae with ejecta masses of only ~0.1M⊙ whose progenitors lose their envelopes due to binary interactions with their compact companion stars. We follow the evolution of an ultra-stripped supernova progenitor until core collapse and perform explosive nucleosynthesis calculations. We then synthesize light curves and spectra of ultra-stripped supernovae based on the nucleosynthesis results. We show that ultra-stripped supernovae synthesize ~0.01M⊙ of the radioactive 56Ni, and their typical peak luminosity is around 1042 erg s−1 or −16 mag. Their typical rise time is 5 − 10 days. By comparing synthesized and observed spectra, we find that SN 2005ek and some of so-called calcium-rich gap transients like PTF10iuv may be related to ultra-stripped supernovae.
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Ellis, Richard, and Mark Sullivan. "Verifying the Use of Supernovae as Probes of the Cosmic Expansion." Symposium - International Astronomical Union 201 (2005): 231–40. http://dx.doi.org/10.1017/s007418090021629x.
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We present preliminary results of a follow-up survey which aims to characterise in detail those galaxies which hosted Type Ia supernovae found by the Supernova Cosmology Project. Our survey has two components: Hubble Space Telescope imaging with STIS and Keck spectroscopy with ESI, the goal being to classify each host galaxy into one of three broad morphological/spectral classes and hence to investigate the dependence of supernovae properties on host galaxy type over a large range in redshift. Of particular interest is the supernova Hubble diagram characterised by host galaxy class which suggests that most of the scatter arises from those occurring in late-type irregulars. Supernovae hosted by (presumed dust-free) E/SO galaxies closely follow the adopted SCP cosmological model. Although larger datasets are required, we cannot yet find any significant difference in the light curves of distant supernovae hosted in different galaxy types.
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Quimby, Robert M. "Superluminous Supernovae." Proceedings of the International Astronomical Union 7, S279 (April 2011): 22–28. http://dx.doi.org/10.1017/s174392131201263x.
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AbstractNot long ago the sample of well studied supernovae, which were gathered mostly through targeted surveys, was populated exclusively by events with absolute peak magnitudes fainter than about −20. Modern searches that select supernovae not just from massive hosts but from dwarfs as well have produced a new census with a surprising difference: a significant percentage of supernovae found in these flux limited surveys peak at −21 magnitude or brighter. The energy emitted by these superluminous supernovae in optical light alone rivals the total explosion energy available to typical core collapse supernovae (> 1051 erg). This makes superluminous supernovae difficult to explain through standard models. Adding further complexity to this picture are the distinct observational properties of various superluminous supernovae. Some may be powered in part by interactions with a hydrogen-rich, circumstellar material but others appear to lack hydrogen altogether. Some appear to be powered by large stores of radioactive material, while others fade quickly and have stringent limits on 56-Ni production. In this talk I will discuss the current observational constrains on superluminous supernova and the prospects for revealing their origins.
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Simoni, Rachel, Nigel Maxted, Mathieu Renaud, and Jacco Vink. "Upper Limits on Gamma-ray Emission from Supernovae Serendipitously Observed with H.E.S.S." Proceedings of the International Astronomical Union 12, S331 (February 2017): 325–28. http://dx.doi.org/10.1017/s1743921317004628.
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AbstractIt is hypothesized that some young supernovae might have the correct properties to accelerate cosmic rays, which in turn might generate gamma-ray emission by-products. We search for gamma-ray excesses towards supernovae in nearby galaxies which were serendipitously within the field of view of the HESS telescopes within a year of the supernova event. HESS cherenkov air-shower data collected between December 2003 and March 2015 were considered and compared to recent catalogs. Nine candidate supernovae were identified and analysed. No significant emission from these supernovae has been found, and upper limits for their very high energy emission are reported.
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Sakakibara, Hinako, Atsushi J. Nishizawa, Masamune Oguri, Masayuki Tanaka, Bau-Ching Hsieh, and Kenneth C. Wong. "Effect of lensing magnification on type Ia supernova cosmology." Monthly Notices of the Royal Astronomical Society 486, no. 3 (May 2, 2019): 4365–76. http://dx.doi.org/10.1093/mnras/stz1117.
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ABSTRACT Effect of gravitational magnification on the measurement of distance modulus of type Ia supernovae is presented. We investigate a correlation between magnification and Hubble residual to explore how the magnification affects the estimation of cosmological parameters. We estimate magnification of type Ia supernovae in two distinct methods: one is based on convergence mass reconstruction under the weak lensing limit and the other is based on the direct measurement from galaxies distribution. Both magnification measurements are measured from Subaru Hyper Suprime-Cam survey catalogue. For both measurements, we find no significant correlation between Hubble residual and magnification. Furthermore, we correct for the apparent supernovae fluxes obtained by Supernova Legacy Survey 3-yr sample using direct measurement of the magnification. We find $\Omega _{\rm m0}= 0.282 ^{+0.109} _{-0.086}$ and $w = -1.132 ^{+0.571}_{-0.340}$ for supernovae samples corrected for lensing magnification when we use photometric redshift catalogue of Mizuki, while $\Omega _{\rm m0}= 0.267 ^{+0.114} _{-0.088}$ and $w = -1.074 ^{+0.504} _{-0.312}$ for DEmP photo-z catalogue. Therefore, we conclude that the effect of magnification on the supernova cosmology is negligibly small for the current surveys; however, it has to be considered for the future supernova survey like LSST.
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Chen, Ke-Jung. "Supernovae at the Extremes." Proceedings of the International Astronomical Union 11, A29B (August 2015): 218–19. http://dx.doi.org/10.1017/s1743921316004981.
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AbstractDuring a supernova explosion, fluid instabilities are generated because the star is in a hydrodynamically unstable situation, which is like the effects of stirring a fire or blowing air into a hot grill. The resulting mixing of the supernova ejecta may be observable. Here, we briefly discuss the multidimensional simulations of supernovae from very massive stars.
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Maund, Justyn R., Paul A. Crowther, Hans-Thomas Janka, and Norbert Langer. "Bridging the gap: from massive stars to supernovae." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, no. 2105 (September 18, 2017): 20170025. http://dx.doi.org/10.1098/rsta.2017.0025.
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Almost since the beginning, massive stars and their resultant supernovae have played a crucial role in the Universe. These objects produce tremendous amounts of energy and new, heavy elements that enrich galaxies, encourage new stars to form and sculpt the shapes of galaxies that we see today. The end of millions of years of massive star evolution and the beginning of hundreds or thousands of years of supernova evolution are separated by a matter of a few seconds, in which some of the most extreme physics found in the Universe causes the explosive and terminal disruption of the star. Key questions remain unanswered in both the studies of how massive stars evolve and the behaviour of supernovae, and it appears the solutions may not lie on just one side of the explosion or the other or in just the domain of the stellar evolution or the supernova astrophysics communities. The need to view massive star evolution and supernovae as continuous phases in a single narrative motivated the Theo Murphy international scientific meeting ‘Bridging the gap: from massive stars to supernovae’ at Chicheley Hall, UK, in June 2016, with the specific purpose of simultaneously addressing the scientific connections between theoretical and observational studies of massive stars and their supernovae, through engaging astronomers from both communities. This article is part of the themed issue ‘Bridging the gap: from massive stars to supernovae’.
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Pooley, David. "X-ray Spectra of Young Supernovae." International Astronomical Union Colloquium 192 (2005): 201–5. http://dx.doi.org/10.1017/s0252921100009192.
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SummaryX-ray spectra of young supernovae (SNe) can provide information on the progenitor star and the interaction of the supernova ejecta and the circumstellar material. I will discuss some examples, with particular emphasis on SN 1998S, whose X-ray spectrum revealed for the first time in a young supernova a wealth of heavy element emission features (Ne, Al, Si, S, Ar, and Fe). By comparison with detailed calculations of supernova explosion elemental yields, these data can be used to constrain the progenitor mass. With increasingly sophisticated models and additional high quality data, application of this technique could result in many more reliable progenitor mass determinations. In addition, high resolution X-ray spectra allow us to measure the temperature evolution of a supernova and can give us a detailed picture of the progenitor’s pre-supernova evolution. As we build up additional examples from the great diversity of core collapse supernovae, we hope to come to a better understanding of the last stages of massive star evolution.
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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 membership. Binary interactions may be the cause of much of the variability among type II supernova light curves. In particular, many of the peculiarities of SN 1987A and SN 1993J may well have resulted from the prior duplicity of the progenitors.
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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 important grain destruction mechanism in the galaxy. Interstellar dust swept up by the expanding blast wave is predominantly heated and destroyed by collisions with a shocked x-ray emitting plasma. Infrared observations of remnants can therefore provide valuable information on the interaction between dust particles and a hot gas. This interaction can best be studied in supernova remnants detected with the Infrared Astronomical Satellite (IRAS). This paper reviews what we have learned so far on the subjects of grain formation and destruction by studying the infrared emission from supernovae and supernova remnants.
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van den Bergh, S. "Supernova Rates, Starbursts and Galaxy Inclinations." Publications of the Astronomical Society of Australia 9, no. 1 (1991): 13–14. http://dx.doi.org/10.1017/s1323358000024772.
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AbstractThe supernova rate in spirals of types Sc and Sd shows a sharp peak in face-on galaxies with inclination i ≤ 25°. This suggests that most supernovae in late-type galaxies occur in rich clusters or associations that are located at the base of chimney-like structures formed by a previous generation of supernovae. These chimneys are transparent because most of the dust contained in the rising column of gas within them had previously been destroyed in the hot bubble surrounding supernovae.
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Chevalier, R. A. "Supernovae and Stellar Mass Loss." Highlights of Astronomy 7 (1986): 599–609. http://dx.doi.org/10.1017/s1539299600007000.
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AbstractType I supernovae can be modeled as the carbon deflagration of white dwarfs and Type II supernovae as the explosions of massive stars with hydrogen envelopes. The massive stars at the ends of their lives are expected to be red supergiants, which are observed to have slow, dense winds. The interaction of the supernova kinetic energy and radiation with the circumstellar gas gives rise to observational phenomena at a range of wavelengths. Additional phenomena, such as a scattered light echo, are predicted. While the light from a Type II supernova near maximum light is probably from energy deposited in the initial explosion, there is now good evidence that the radioactive decay of 56Co powers the emission at late times. It was been noted that the explosions of massive stars without hydrogen envelopes would be quite unlike normal Type II supernovae. There is now good evidence for such explosions – SN1985f and the class of peculiar Type I supernovae. It is suggested that these supernovae be called Type III with the spectroscopic definition of a) no H lines and b) broad [01] lines at late times. That not all very massive star explosions are of this type is indicated by SN1961v, which was probably a very massive explosion, but in which hydrogen was present.
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Kotak, Rubina. "Core-Collapse Supernovae as Dust Producers." Proceedings of the International Astronomical Union 3, S250 (December 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-Infrared Supernova Consortium, I briefly discuss recent exciting results from mid-IR studies of core-collapse supernovae using Spitzer and attempt to put the role of supernovae as major dust producers into perspective.
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Woosley, S. E., T. A. Weaver, and R. G. Eastman. "Progenitors and Hydrodynamics of Type II and lb Supernovae." International Astronomical Union Colloquium 145 (1996): 137–47. http://dx.doi.org/10.1017/s0252921100008009.
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We review critical physics affecting the observational characteristics of those supernovae that occur in massive stars. Particular emphasis is given to 1) how mass loss, either to a binary companion or by a radiatively driven wind, affects the type and light curve of the supernova, and 2) the interaction of the outgoing supernova shock with regions of increasing pr3 in the stellar mantle. One conclusion is that Type II-L supernovae may occur in mass exchanging binaries very similar to the one that produced SN 1993J, but with slightly larger initial separations and residual hydrogen envelopes (∼1 Mʘ and radius ∼ several AU). The shock interaction, on the other hand, has important implications for the formation of black holes in explosions that are, near peak light, observationally indistinguishable from ordinary Type II-p and lb supernovae.
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Fraser, Morgan. "Supernovae and transients with circumstellar interaction." Royal Society Open Science 7, no. 7 (July 2020): 200467. http://dx.doi.org/10.1098/rsos.200467.
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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.
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McCall, Marshall L., and Fred H. Schmidt. "Supernovae in Flocculent and Grand Design Galaxies." Highlights of Astronomy 7 (1986): 585–88. http://dx.doi.org/10.1017/s1539299600006985.
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AbstractThe arm structure of supernova host galaxies has been studied in order to ascertain whether or not spiral density waves have an impact on supernovae frequencies. The ensembles of Type I and Type II supernova hosts were found to contain identical fractions of grand design spirals consistent with the representations in control samples chosen without regard to supernovae production. The results suggest that a density wave does not greatly enhance the massive star formation rate per unit luminosity of a galaxy. Instead, star formation in most galaxies may be dominated by stochastic processes.
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Vissani, Francesco, and Andrea Gallo Rosso. "On the Time Distribution of Supernova Antineutrino Flux." Symmetry 13, no. 10 (October 2, 2021): 1851. http://dx.doi.org/10.3390/sym13101851.
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Neutrino leptonic flavor symmetry violation is the only evidence for physics beyond the standard model. Much of what we have learned on these particles is derived from the study of their natural sources, such as the Sun or core-collapse supernovae. Neutrino emission from supernovae is particularly interesting and leptonic flavor transformations in supernova neutrinos have attracted a lot of theoretical attention. Unfortunately, the emission of core-collapse supernovae is not fully understood: thus, an inescapable preliminary step to progress is to improve on that, and future neutrino observations can help. One pressing and answerable question concerns the time distribution of the supernova anti-neutrino events. We propose a class of models of the time distribution that describe emission curves similar to those theoretically expected and consistent with available observations from the data of supernova SN1987A. They have the advantages of being motivated on physical bases and easy to interpret; they are flexible and adaptable to the results of the observations from a future galactic supernova. Important general characteristics of these models are the presence of an initial ramp and that a significant portion of the signal is in the first second of the emission.
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Chevalier, R. A. "The Early Evolution of Supernova Remnants." International Astronomical Union Colloquium 101 (1988): 31–42. http://dx.doi.org/10.1017/s0252921100102076.
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AbstractThe density distribution of the supernova ejecta and that of the surrounding medium are the most important parameters for the early evolution of supernova remnants. The distribution of the ejecta depends on the detailed hydrodynamics of the explosion, but the outer parts of a supernova can probably be represented by a steep power law density distribution with radius. Self-similar solutions are especially useful for modeling the interaction of a supernova with its surrounding. The supernova first interacts with mass loss from the progenitor star. Evidence for circumstellar interaction is present in a number of extragalactic supernovae, including SN1987a. The explosions of massive stars probably interact with circumstellar gas for a considerable time while Type Ia supernovae interact more directly with the interstellar medium. X-ray spectroscopy is a good diagnostic for the physical conditions in young supernova remnants and for the composition of the supernova gas.
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Abbasi, R., M. Ackermann, J. Adams, S. K. Agarwalla, J. A. Aguilar, M. Ahlers, J. M. Alameddine, et al. "Constraining High-energy Neutrino Emission from Supernovae with IceCube." Astrophysical Journal Letters 949, no. 1 (May 1, 2023): L12. http://dx.doi.org/10.3847/2041-8213/acd2c9.
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Abstract Core-collapse supernovae are a promising potential high-energy neutrino source class. We test for correlation between seven years of IceCube neutrino data and a catalog containing more than 1000 core-collapse supernovae of types IIn and IIP and a sample of stripped-envelope supernovae. We search both for neutrino emission from individual supernovae as well as for combined emission from the whole supernova sample, through a stacking analysis. No significant spatial or temporal correlation of neutrinos with the cataloged supernovae was found. All scenarios were tested against the background expectation and together yield an overall p-value of 93%; therefore, they show consistency with the background only. The derived upper limits on the total energy emitted in neutrinos are 1.7 × 1048 erg for stripped-envelope supernovae, 2.8 × 1048 erg for type IIP, and 1.3 × 1049 erg for type IIn SNe, the latter disfavoring models with optimistic assumptions for neutrino production in interacting supernovae. We conclude that stripped-envelope supernovae and supernovae of type IIn do not contribute more than 14.6% and 33.9%, respectively, to the diffuse neutrino flux in the energy range of about [ 103–105] GeV, assuming that the neutrino energy spectrum follows a power-law with an index of −2.5. Under the same assumption, we can only constrain the contribution of type IIP SNe to no more than 59.9%. Thus, core-collapse supernovae of types IIn and stripped-envelope supernovae can both be ruled out as the dominant source of the diffuse neutrino flux under the given assumptions.
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Greiner, J., C. Maitra, F. Haberl, R. Willer, J. M. Burgess, N. Langer, J. Bodensteiner, et al. "A helium-burning white dwarf binary as a supersoft X-ray source." Nature 615, no. 7953 (March 22, 2023): 605–9. http://dx.doi.org/10.1038/s41586-023-05714-4.
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AbstractType Ia supernovae are cosmic distance indicators1,2, and the main source of iron in the Universe3,4, but their formation paths are still debated. Several dozen supersoft X-ray sources, in which a white dwarf accretes hydrogen-rich matter from a non-degenerate donor star, have been observed5 and suggested as Type Ia supernovae progenitors6–9. However, observational evidence for hydrogen, which is expected to be stripped off the donor star during the supernova explosion10, is lacking. Helium-accreting white dwarfs, which would circumvent this problem, have been predicted for more than 30 years (refs. 7,11,12), including their appearance as supersoft X-ray sources, but have so far escaped detection. Here we report a supersoft X-ray source with an accretion disk whose optical spectrum is completely dominated by helium, suggesting that the donor star is hydrogen-free. We interpret the luminous and supersoft X-rays as resulting from helium burning near the surface of the accreting white dwarf. The properties of our system provide evidence for extended pathways towards Chandrasekhar-mass explosions based on helium accretion, in particular for stable burning in white dwarfs at lower accretion rates than expected so far. This may allow us to recover the population of the sub-energetic so-called Type Iax supernovae, up to 30% of all Type Ia supernovae13, within this scenario.
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Sadler, Elaine M., and Duncan Campbell-Wilson. "A Search for Radio-loud Supernovae." Publications of the Astronomical Society of Australia 14, no. 2 (1997): 159–63. http://dx.doi.org/10.1071/as97159.
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AbstractSome extragalactic supernovae, such as SN 1986J in NGC 891 (Rupen et al. 1987), are unusually strong radio sources. Their radio emission typically peaks a few years after the supernova explodes, and appears to arise from the interaction of the supernova shock with a dense stellar wind shed by the progenitor star. Since two radio-loud and possibly optically faint supernovae have recently been found serendipitously in nearby spiral galaxies, it is possible that such objects are common. If so, this would have important consequences for our understanding of both the chemical enrichment history of galaxies and the radio emission from starburst galaxies. Preliminary results from a survey of nearby spiral galaxies with the Molonglo Observatory Synthesis Telescope (MOST) allow us to make a first estimate of the radio supernova rate. A larger study now in progress will provide a much more sensitive measurement.
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Jerkstrand, Anders, Keiichi Maeda, and Koji S. Kawabata. "A type Ia supernova at the heart of superluminous transient SN 2006gy." Science 367, no. 6476 (January 23, 2020): 415–18. http://dx.doi.org/10.1126/science.aaw1469.
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Superluminous supernovae radiate up to 100 times more energy than normal supernovae. The origin of this energy and the nature of the stellar progenitors of these transients are poorly understood. We identify neutral iron lines in the spectrum of one such supernova, SN 2006gy, and show that they require a large mass of iron (≳0.3 solar masses) expanding at 1500 kilometers per second. By modeling a standard type Ia supernova hitting a shell of circumstellar material, we produce a light curve and late-time iron-dominated spectrum that match the observations of SN 2006gy. In such a scenario, common envelope evolution of a progenitor binary system can synchronize envelope ejection and supernova explosion and may explain these bright transients.
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Hook, I. M. "Supernovae and cosmology with future European facilities." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 371, no. 1992 (June 13, 2013): 20120282. http://dx.doi.org/10.1098/rsta.2012.0282.
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Prospects for future supernova surveys are discussed, focusing on the European Space Agency’s Euclid mission and the European Extremely Large Telescope (E-ELT), both expected to be in operation around the turn of the decade. Euclid is a 1.2 m space survey telescope that will operate at visible and near-infrared wavelengths, and has the potential to find and obtain multi-band lightcurves for thousands of distant supernovae. The E-ELT is a planned, general-purpose ground-based, 40-m-class optical–infrared telescope with adaptive optics built in, which will be capable of obtaining spectra of type Ia supernovae to redshifts of at least four. The contribution to supernova cosmology with these facilities will be discussed in the context of other future supernova programmes such as those proposed for DES, JWST, LSST and WFIRST.
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Hjorth, Jens. "The supernova–gamma-ray burst–jet connection." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 371, no. 1992 (June 13, 2013): 20120275. http://dx.doi.org/10.1098/rsta.2012.0275.
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The observed association between supernovae and gamma-ray bursts represents a cornerstone in our understanding of the nature of gamma-ray bursts. The collapsar model provides a theoretical framework for this connection. A key element is the launch of a bipolar jet (seen as a gamma-ray burst). The resulting hot cocoon disrupts the star, whereas the 56 Ni produced gives rise to radioactive heating of the ejecta, seen as a supernova. In this discussion paper, I summarize the observational status of the supernova–gamma-ray burst connection in the context of the ‘engine’ picture of jet-driven supernovae and highlight SN 2012bz/GRB 120422A—with its luminous supernova but intermediate high-energy luminosity—as a possible transition object between low-luminosity and jet gamma-ray bursts. The jet channel for supernova explosions may provide new insights into supernova explosions in general.
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Harada, Akira, Yudai Suwa, Masayuki Harada, Yusuke Koshio, Masamitsu Mori, Fumi Nakanishi, Ken’ichiro Nakazato, Kohsuke Sumiyoshi, and Roger A. Wendell. "Observing Supernova Neutrino Light Curves with Super-Kamiokande. IV. Development of SPECIAL BLEND: A New Public Analysis Code for Supernova Neutrinos." Astrophysical Journal 954, no. 1 (August 22, 2023): 52. http://dx.doi.org/10.3847/1538-4357/ace52e.
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Abstract Supernova neutrinos are invaluable signals that offer information about the interior of supernovae. Because a nearby supernova can occur at any time, preparing for future supernova neutrino observation is an urgent task. For the prompt analysis of supernova neutrinos, we have developed a new analysis code, the “Supernova Parameter Estimation Code based on Insight on Analytic Late-time Burst Light curve at Earth Neutrino Detector” (SPECIAL BLEND). This code estimates the parameters of supernovae based on an analytic model of supernova neutrinos from the proto-neutron star cooling phase. For easy availability to the community, this code is public and easily runs in web environments. SPECIAL BLEND can estimate the parameters better than the analysis pipeline we developed in a previous paper. By using SPECIAL BLEND, we can estimate the supernova parameters within 10% precision up to ∼20 and ∼60 kpc (Large Magellanic Cloud contained) with Super-Kamiokande and Hyper-Kamiokande, respectively.
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Podsiadlowski, Philipp. "Binary Effects on Supernovae." Proceedings of the International Astronomical Union 9, S296 (January 2013): 45–52. http://dx.doi.org/10.1017/s1743921313009216.
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AbstractHere we review how binary interactions affect the final pre-supernova structure of massive stars and the resulting supernova explosions. (1) Binary-induced mass loss and mass accretion determine the final envelope structure, the mass, radius and chemical composition, which are mainly responsible for the supernova appearance and supernova (sub-)type. (2) Mass loss can also drastically change the core evolution and hence the final fate of a star; specifically, around 10 M⊙, it determines whether a star explodes in a supernova or forms a white dwarf, while for larger masses it can dramatically increase the minimum main-sequence mass above which a star is expected to collapse to a black hole. (3) Mass loss before the supernova directly affects the circumstellar medium (CSM) which can affect the supernova spectrum (e.g. account for the IIn phenomenon), produce powerful radio emission and, in extreme cases, lead to a strong interaction with the supernova ejecta and thus strongly modify the lightcurve shape; it may even be responsible for some of the superluminous supernovae that have recently been discovered.
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Phillips, M. M., C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, et al. "The Absolute Magnitudes of 1991T-like Supernovae *." Astrophysical Journal 938, no. 1 (October 1, 2022): 47. http://dx.doi.org/10.3847/1538-4357/ac9305.
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Abstract 1991T-like supernovae are the luminous, slow-declining extreme of the Branch shallow-silicon (SS) subclass of Type Ia supernovae. They are distinguished by extremely weak Ca ii H & K and Si ii λ6355 and strong Fe iii absorption features in their optical spectra at pre-maximum phases, and have long been suspected to be over-luminous compared to normal Type Ia supernovae. In this paper, the pseudo-equivalent width of the Si ii λ6355 absorption obtained at light curve phases from ≤ +10 days is combined with the morphology of the i-band light curve to identify a sample of 1991T-like supernovae in the Carnegie Supernova Project II. Hubble diagram residuals show that, at optical as well as near-infrared wavelengths, these events are over-luminous by ∼0.1–0.5 mag with respect to the less extreme Branch SS (1999aa-like) and Branch core-normal supernovae with similar B-band light-curve decline rates.
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Chevalier, Roger A. "Supernovae and their Evolution in a Low Metallicity ISM." Proceedings of the International Astronomical Union 4, S255 (June 2008): 175–81. http://dx.doi.org/10.1017/s1743921308024782.
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AbstractObservations of core collapse supernovae and their progenitors generally support expectations of increasing mass loss with increasing initial mass. Mass loss rates are expected to decline at lower metallicity, and there are prospects for directly testing this for the red supergiant progenitors of Type IIP supernovae. However, there are indications that mass loss rates for high mass early type stars may be overestimated and that there are mass loss mechanisms that do not decline at lower metallicity. In this case, there may be supernova emission from strong circumstellar interaction even at low metallicity. Although there is evidence for dust formation in freely expanding ejecta of supernovae, the quantities are relatively small. Another promising site of dust formation is the circumstellar interaction region, but this should occur in only a fraction of supernovae.
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Fryer, Chris L., Carola Ellinger, Patrick A. Young, and Gregory Vance. "Diagnostics of the Supernova Engine." Proceedings of the International Astronomical Union 12, S331 (February 2017): 86–95. http://dx.doi.org/10.1017/s174392131700641x.
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AbstractThe standard engine behind core-collapse supernovae is continuously evolving with increasingly detailed models. At this time, most simulations focus on an engine invoking turbulence above the proto-neutron star, sometimes termed the “convection-enhanced” engine. Here we review this engine and why it has become the standard for normal supernovae, focusing on a wide set of observations that provide insight into the supernova engine.
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Godani, Nisha. "FRW cosmology in f(R,T) gravity." International Journal of Geometric Methods in Modern Physics 16, no. 02 (February 2019): 1950024. http://dx.doi.org/10.1142/s0219887819500245.
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In the present paper, the work of Moreas et al. [P. H. R. S. Moraes, G. Ribeiro and R. A. C. Correa, A transition from a decelerated to an accelerated phase of the universe expansion from the simplest non-trivial polynomial function of T in the [Formula: see text] formalism, Astrophys. Space Sci. 361 (2016) 227–231] is extended to study the FRW model in [Formula: see text] gravity. The expressions for deceleration and Hubble parameters are determined in terms of redshift. The age of the universe is established using [Formula: see text] high-redshift type Ia supernovae data from the Supernova cosmology project and 15 low-redshift type Ia supernovae data from the Calán/Tolono Supernova survey [S. Permutter et al., Measurements of Omega and Lambda from 42 High-Redshift Supernovae, Astrophys. J. 517 (1999) 565–585]. For these redshifts, the data of observed apparent magnitude and luminosity distance are used for the comparison with the obtained theoretical values.
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Godłewski, Włodzimierz, and Marek Szydłowski. "Brane Universes Tested by Supernovae." International Astronomical Union Colloquium 192 (2005): 579–84. http://dx.doi.org/10.1017/s0252921100009696.
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SummaryWe discuss observational constrains coming from supernovae Ia imposed on the behavior of the Randall-Sundrum models. It is interesting that brane models predict brighter galaxies for such redshifts which is in agreement with the measurement of the z = 1.7 supernova. We also demonstrate that the fit to supernovae data can also be obtained, if we admit the “super-negative” dark energy p = − (4/3) ϱ on the brane, where the dark energy in a way mimics the influence of the cosmological constant.
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Williams, Andrew J. "Initial Statistics from the Perth Automated Supernova Search." Publications of the Astronomical Society of Australia 14, no. 2 (1997): 208–13. http://dx.doi.org/10.1071/as97208.
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AbstractThe Perth Automated Supernova Search uses the 61-cm PLAT (Perth Lowell Automated Telescope) at Perth Observatory, Western Australia. Since 1993 January 1, five confirmed supernovae have been found by the search. The analysis of the first three years of data is discussed, and preliminary results presented. We find a Type Ib/c rate of 0·43±0·43 SNu, and a Type IIP rate of 0·86±0·49 SNu, where SNu are ‘supernova units’, expressed in supernovae per 1010 LB⊙ galaxy per century. These values are for a Hubble constant of 75 kms−1 Mpc−1, and scale as (H0/75)2.
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Bendahman, Meriem. "Neutrinos from core-collapse supernovae at KM3NeT." EPJ Web of Conferences 280 (2023): 05003. http://dx.doi.org/10.1051/epjconf/202328005003.
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The SN1987A supernova was the first extragalactic neutrino de- tection, but no further observations have been made since. Detecting neutrinos from a galactic supernova would provide invaluable information on the supernova mechanism and particle behavior in dense environments, hence, improving the sensitivity of current and upcoming neutrino experiments is crucial. In this contribution, we discuss how the optical module design of the KM3NeT neutrino experiment would allow to observe supernova neutrinos. We present KM3NeT’s sensitivity to galactic supernovae and describe its associated online alert system for multi-messenger studies. Finally, we discuss KM3NeT’s ability to infer the supernova evolution from the time profile of the associated neutrino emission.