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Relevant bibliographies by topics / Failed supernova

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Academic literature on the topic 'Failed supernova'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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Journal articles on the topic "Failed supernova"

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Tsuna, Daichi. "Failed supernova remnants." Publications of the Astronomical Society of Japan 73, no. 3 (2021): L6—L11. http://dx.doi.org/10.1093/pasj/psab041.

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Abstract In a failed supernova, partial ejection of the progenitor’s outer envelope can occur due to weakening of the core’s gravity by neutrino emission in the protoneutron star phase. We consider emission when this ejecta sweeps up the circumstellar material, analogous to supernova remnants (SNRs). We focus on failed explosions of blue supergiants, and find that the emission can be bright in soft X-rays. Due to its soft emission, we find that sources in the Large Magellanic Cloud (LMC) are more promising for detection than those in the Galactic disk. These remnants are characteristic in their small size (≲10 pc) and slow speed (100s of km s−1) compared to typical SNRs. Although the expected number of detectable sources is small (up to a few by the eROSITA four-year all-sky survey), prospects are better for deeper surveys targeting the LMC. Detection of these “failed SNRs” will realize observational studies of mass ejection following black hole formation.

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Mathews, Grant J., Jun Hidaka, Toshitaka Kajino, and Jyutaro Suzuki. "SUPERNOVA RELIC NEUTRINOS AND THE SUPERNOVA RATE PROBLEM: ANALYSIS OF UNCERTAINTIES AND DETECTABILITY OF ONeMg AND FAILED SUPERNOVAE." Astrophysical Journal 790, no. 2 (2014): 115. http://dx.doi.org/10.1088/0004-637x/790/2/115.

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Jones, Samuel, Raphael Hirschi, Falk Herwig, Bill Paxton, Francis X. Timmes, and Ken'ichi Nomoto. "Progenitors of electron-capture supernovae." Proceedings of the International Astronomical Union 7, S279 (2011): 341–42. http://dx.doi.org/10.1017/s1743921312013257.

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AbstractWe investigate the lowest mass stars that produce Type-II supernovae, motivated by recent results showing that a large fraction of type-II supernova progenitors for which there are direct detections display unexpectedly low luminosity (for a review see e.g. Smartt 2009). There are three potential evolutionary channels leading to this fate. Alongside the standard ‘massive star’ Fe-core collapse scenario we investigate the likelihood of electron capture supernovae (EC-SNe) from super-AGB (S-AGB) stars in their thermal pulse phase, from failed massive stars for which neon burning and other advanced burning stages fail to prevent the star from contracting to the critical densities required to initiate rapid electron-capture reactions and thus the star's collapse. We find it indeed possible that both of these relatively exotic evolutionary channels may be realised but it is currently unclear for what proportion of stars. Ultimately, the supernova light curves, explosion energies, remnant properties (see e.g. Knigge et al. 2011) and ejecta composition are the quantities desired to establish the role that these stars at the lower edge of the massive star mass range play.

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Melson, Tobias, Hans-Thomas Janka, Alexander Summa, Robert Bollig, Andreas Marek, and Bernhard Müller. "Exploring the explosion mechanism of core-collapse supernovae in three dimensions." Proceedings of the International Astronomical Union 12, S329 (2016): 424. http://dx.doi.org/10.1017/s1743921317001181.

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AbstractWe present the first successful simulations of neutrino-driven supernova explosions in three dimensions (3D) using the Vertex-Prometheus code including sophisticated energy-dependent neutrino transport. The simulated models of 9.6 and 20 solar-mass iron-core stars demonstrate that successful explosions can be obtained in self-consistent 3D simulations, where previous models have failed. New insights into the supernova mechanism can be gained from these explosions. The first 3D model (Melson et al. 2015a) explodes at the same time but more energetically than its axially symmetric (2D) counterpart. Turbulent energy cascading reduces the kinetic energy dissipation in the cooling layer and therefore suppresses neutrino cooling. The consequent inward shift of the gain radius increases the gain layer mass, whose recombination energy provides the surplus for the explosion energy.The second explosion (Melson et al. 2015b) is obtained through a moderate reduction of the neutral-current neutrino opacity motivated by strange-quark contributions to the nucleon spin. A corresponding reference model without these corrections failed, which demonstrates how close current 3D models are to explosion. The strangeness adjustment is meant as a prototype for remaining neutrino opacity uncertainties.

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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 of their progenitor stars.Judging the fate of a massive star, either a neutron star (NS) or a black hole (BH), solely by its structure prior to collapse has been ambiguous. Our work and previous attempts find a non-monotonic variation of successful and failed supernovae with zero-age main-sequence mass. We identify two parameters based on the “critical luminosity” concept for neutrino-driven explosions, which in combination allows for a clear separation of exploding and non-exploding cases.Continuing our simulations beyond shock break-out, we are able to determine nucleosynthesis, light curves, explosion energies, and remnant masses. The resulting NS initial mass function has a mean gravitational mass near 1.4 M⊙. The average BH mass is about 9 M⊙ if only the helium core implodes, and 14 M⊙ if the entire pre-SN star collapses. Only ~10% of SNe come from stars over 20 M⊙, and some of these are Type Ib or Ic.

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Farrell, Eoin J., Jose H. Groh, Georges Meynet, and J. J. Eldridge. "The uncertain masses of progenitors of core-collapse supernovae and direct-collapse black holes." Monthly Notices of the Royal Astronomical Society: Letters 494, no. 1 (2020): L53—L58. http://dx.doi.org/10.1093/mnrasl/slaa035.

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ABSTRACT We show that it is not possible to determine the final mass Mfin of a red supergiant (RSG) at the pre-supernova (SN) stage from its luminosity L and effective temperature Teff alone. Using a grid of stellar models, we demonstrate that for a given value of L and Teff, an RSG can have a range of Mfin as wide as 3 to 45 M⊙. While the probability distribution within these limits is not flat, any individual determination of Mfin for an RSG will be degenerate. This makes it difficult to determine its evolutionary history and to map Mfin to an initial mass. Single stars produce a narrower range that is difficult to accurately determine without making strong assumptions about mass-loss, convection, and rotation. Binaries would produce a wider range of RSG Mfin. However, the final Helium core mass $M_{\operatorname{He-core}}$ is well determined by the final luminosity and we find $\log (M_{\operatorname{He-core}}/\mathrm{M}_{\odot }) = 0.659 \log (L/\mathrm{L}_{\odot }) -2.630$. Using this relationship, we derive $M_{\operatorname{He-core}}$ for directly imaged SN progenitors and one failed SN candidate. The value of Mfin for stripped star progenitors of SNe IIb is better constrained by L and Teff due to the dependence of Teff on the envelope mass Menv for Menv ≲ 1 M⊙. Given the initial mass function, our results apply to the majority of progenitors of core-collapse SNe, failed SNe, and direct-collapse black holes.

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Utrobin, V. P., A. Wongwathanarat, H. Th Janka, E. Müller, T. Ertl, and S. E. Woosley. "Three-dimensional mixing and light curves: constraints on the progenitor of supernova 1987A." Astronomy & Astrophysics 624 (April 2019): A116. http://dx.doi.org/10.1051/0004-6361/201834976.

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With the same method as used previously, we investigate neutrino-driven explosions of a larger sample of blue supergiant models. The blue supergiants were evolved as single-star progenitors. The larger sample includes three new presupernova stars. The results are compared with light-curve observations of the peculiar type IIP supernova 1987A (SN 1987A). The explosions were modeled in 3D with the neutrino-hydrodynamics code PROMETHEUS-HOTB, and light-curve calculations were performed in spherical symmetry with the radiation-hydrodynamics code CRAB, starting at a stage of nearly homologous expansion. Our results confirm the basic findings of the previous work: 3D neutrino-driven explosions with SN 1987A-like energies synthesize an amount of 56Ni that is consistent with the radioactive tail of the light curve. Moreover, the models mix hydrogen inward to minimum velocities below 400 km s−1 as required by spectral observations and a 3D analysis of molecular hydrogen in SN 1987A. Hydrodynamic simulations with the new progenitor models, which possess smaller radii than the older ones, show much better agreement between calculated and observed light curves in the initial luminosity peak and during the first 20 days. A set of explosions with similar energies demonstrated that a high growth factor of Rayleigh–Taylor instabilities at the (C+O)/He composition interface combined with a weak interaction of fast Rayleigh–Taylor plumes, where the reverse shock occurs below the He/H interface, provides a sufficient condition for efficient outward mixing of 56Ni into the hydrogen envelope. This condition is realized to the required extent only in one of the older stellar models, which yielded a maximum velocity of around 3000 km s−1 for the bulk of ejected 56Ni, but failed to reproduce the helium-core mass of 6 M⊙ inferred from the absolute luminosity of the presupernova star. We conclude that none of the single-star progenitor models proposed for SN 1987A to date satisfies all constraints set by observations.

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Totani, Tomonori. "A Failed Gamma‐Ray Burst with Dirty Energetic Jets Spirited Away? New Implications for the Gamma‐Ray Burst–Supernova Connection from SN 2002ap." Astrophysical Journal 598, no. 2 (2003): 1151–62. http://dx.doi.org/10.1086/378936.

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Kochanek, C. S. "Dust formation by failed supernovae." Monthly Notices of the Royal Astronomical Society 444, no. 3 (2014): 2043–47. http://dx.doi.org/10.1093/mnras/stu1559.

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Yan, Zhiqiang, Tereza Jerabkova, and Pavel Kroupa. "Chemical evolution of ultra-faint dwarf galaxies in the self-consistently calculated integrated galactic IMF theory." Astronomy & Astrophysics 637 (May 2020): A68. http://dx.doi.org/10.1051/0004-6361/202037567.

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The galaxy-wide stellar initial mass function (gwIMF) of a galaxy in dependence on its metallicity and star formation rate can be calculated by the integrated galactic IMF (IGIMF) theory. This theory has been applied in a study of the chemical evolution of the ultra-faint dwarf (UFD) satellite galaxies, but failed to reproduce the data. Here, we find that the IGIMF theory is naturally consistent with the data. We applied the time-evolving gwIMF, which was calculated at each time step. The number of type Ia supernova explosions that forms per unit stellar mass was renormalised according to the gwIMF. The chemical evolution of Boötes I, one of the best-observed UFD, was calculated. Our calculation suggests a mildly bottom-light and top-light gwIMF for Boötes I, and that this UFD has the same gas-consumption timescale as other dwarfs, but was quenched about 0.1 Gyr after formation. This is consistent with independent estimations, and it is similar to Dragonfly 44. The recovered best-fitting input parameters in this work are not covered in previous work, creating a discrepancy between our conclusions. In addition, a detailed discussion of the uncertainties is presented to address the dependence of the chemical evolution model results on the applied assumptions. This study demonstrates the power of the IGIMF theory in understanding star formation in extreme environments and shows that UDFs are a promising pathway to constrain the variation of the low-mass stellar IMF.

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Dissertations / Theses on the topic "Failed supernova"

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Gerke, Jill R. "Failed Supernovae, Dusty Stars and Cepheid Distances." The Ohio State University, 2014. http://rave.ohiolink.edu/etdc/view?acc_num=osu1405528289.

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Adams, Scott M. "Stellar Death by Weak or Failed Supernovae." The Ohio State University, 2016. http://rave.ohiolink.edu/etdc/view?acc_num=osu1468850125.

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Dereli, Hüsne. "Découverte et étude d'une population de sursauts gamma cosmiques à décroissance de faible luminosité." Thesis, Nice, 2014. http://www.theses.fr/2014NICE4130/document.

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Les explosions gamma (GRB) sont des évènements extrêmement violents. Ils sont sommairement classifiés en deux groupes par leur durée : les courts et les longs. Cette classification a permis de déterminer l'origine des GRBs : une collision entre deux objets compacts pour les courts ou l'explosion d'une étoile très massive pour les longs. Une meilleure classification des GRBs longs pourrait mieux contraindre leurs propriétés. Dans ma thèse, je présente des évidences de l'existence d'une sous-classification des GRBs basés sur la faible luminosité de leurs derniers reflets. Ces explosions sont appelées Low-Luminosity Afterflow (LLA). Je présente la technique de réduction des données, la méthode de sélection de ces GRBs ainsi que leurs principales propriétés. Leur lien avec les supernovæ (SN) est mis en évidence car 64 % de tous les GRBs associés à des Sns sont des LLA GRBs. Finalement, je présente d'autres propriétés comme leur fréquence, qui semble indiquer une nouvelle distincte classe, les propriétés de leurs galaxies hôte qui montrent que ces explosions ont pour origines des galaxies formant beaucoup d'étoiles. De plus, je montre qu'il est difficile de réconcilier les différences entre les GRBs normaux et les LLA GRBs en ne considérant que des effets instrumentaux et environnementaux, ou bien une géométrie différente. Donc je conclue que les deux classes de GRBs ont des propriétés différentes. En basant l'argumentation sur la fonction de masse initiale, sur la fréquence des LLA GRBs et sur le type de SNs qui les accompagnent, j'indique qu'un système binaire est favorisé pour leur origine<br>Gamma-ray bursts (GRB) are extreme events. They are crudely classified into two groups based on their duration, namely the short and long bursts. Such a classification has proven to be useful to determine their progenitors: the merger of two compact objects for short bursts and the explosion of a massive star for long bursts. Further classifying the long GRBs might give tighter constraints on their progenitor and on the emission mechanism(s). In my thesis, I present evidence for the existence of a sub-class of long GRBs, based on their faint afterglow emission. These bursts were named low-luminosity afterglow (LLA) GRBs. I discuss the data analysis and the selection method, and their main properties are described. Their link to supernova is strong as 64\% of all the bursts firmly associated to SNe is LLA GRBs. Finally, I present additional properties of LLA GRBs: the study of their rate density, which seems to indicate a new distinct third class of events, the properties of their host galaxies, which show that they take place in young star-forming galaxies. Additionally, I show that it is difficult to reconcile all differences between normal long GRBs and LLA GRBs only by considering instrumental or environmental effects, different ejecta content or a different geometry for the burst. Thus, I conclude that LLA GRBs and normal long GRBs should have different properties. In a very rudimentary discussion, I indicate that a binary system is favored in the case of LLA GRB. The argument is based on the initial mass function of massive stars, on the larger rate density of LLA GRBs compared to the rate of normal long GRBs and on the type of accompanying SNe

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Monzani, Maria Elena. "Characterization and calibration of the Borexino detector for solar and supernova neutrinos." Paris 7, 2005. http://www.theses.fr/2005PA077112.

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"Astrophysical neutrinos at the low and high energy frontiers." Doctoral diss., 2013. http://hdl.handle.net/2286/R.I.20985.

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abstract: For this project, the diffuse supernova neutrino background (DSNB) has been calculated based on the recent direct supernova rate measurements and neutrino spectrum from SN1987A. The estimated diffuse electron antineutrino flux is &sim; 0.10 – 0.59 /cm2/s at 99% confidence level, which is 5 times lower than the Super-Kamiokande 2012 upper limit of 3.0 /cm2/s, above energy threshold of 17.3 MeV. With a Megaton scale water detector, 40 events could be detected above the threshold per year. In addition, the detectability of neutrino bursts from direct black hole forming collapses (failed supernovae) at Megaton detectors is calculated. These neutrino bursts are energetic and with short time duration, &sim; 1s. They could be identified by the time coincidence of N ≥2 or N ≥3 events within 1s time window from nearby (4 – 5 Mpc) failed supernovae. The detection rate of these neutrino bursts could get up to one per decade. This is a realistic way to detect a failed supernova and gives a promising method for studying the physics of direct black hole formation mechanism. Finally, the absorption of ultra high energy (UHE) neutrinos by the cosmic neutrino background, with full inclusion of the effect of the thermal distribution of the background on the resonant annihilation channel, is discussed. Results are applied to serval models of UHE neutrino sources. Suppression effects are strong for sources that extend beyond z &sim; 10. This provides a fascinating probe of the physics of the relic neutrino background in the unexplored redshift interval z &sim; 10 – 100. Ultimately this research will examine the detectability of DSNB, neutrino bursts from failed supernovae and absorption effects in the neutrino spectrum.<br>Dissertation/Thesis<br>Ph.D. Physics 2013

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Book chapters on the topic "Failed supernova"

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Moffat, John W. "Stars and Black Holes." In The Shadow of the Black Hole. Oxford University Press, 2020. http://dx.doi.org/10.1093/oso/9780190650728.003.0003.

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Physicists began to believe in black holes when research revealed new information about the constitution of stars and their life cycles, indicating that a black hole represents the death of certain massive stars. Chandrasekhar used quantum mechanics and the notion of a degenerate electron gas to obtain the maximum mass of a white dwarf. A degenerate neutron gas produced enough pressure to stop the gravitational collapse of a massive star, producing a neutron star or pulsar. For a massive-enough star, the degenerate neutron gas fails to prevent gravitational collapse into a black hole. Supernovae explosions and implosions produce a neutron star or black hole as remnants. Oppenheimer and Volkoff used general relativity to derive the maximum mass of a star that would produce a black hole. Wheeler conceived of a “hairless black hole” in which only the mass, charge, and angular momentum determined the properties of the black hole.

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Conference papers on the topic "Failed supernova"

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Hidaka, Jun, Grant J. Mathews, Toshitaka Kajino, and Jutaro Suzuki. "Equation of State of Proto-Neutron Star and Failed Supernova Neutrino." In Proceedings of the Conference on Advances in Radioactive Isotope Science (ARIS2014). Journal of the Physical Society of Japan, 2015. http://dx.doi.org/10.7566/jpscp.6.030137.

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Kotake, Kei. "Gravitational-wave signatures in successful and failed core-collapse supernova explosions." In 25th Texas Symposium on Relativistic Astrophysics. Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.123.0060.

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Lunardini, Cecilia, and Marvin L. Marshak. "Diffuse neutrinos from failed supernovae." In 10TH CONFERENCE ON THE INTERSECTIONS OF PARTICLE AND NUCLEAR PHYSICS. AIP, 2009. http://dx.doi.org/10.1063/1.3293810.

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Sumiyoshi, K., Ken'ichiro Nakazato, Hideyuki Suzuki, and Shoichi Yamada. "Neutrino bursts from failed supernovae as a promising target of neutrino astronomy." In 11th Symposium on Nuclei in the Cosmos. Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.100.0157.

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Nakazato, Ken'ichiro, and Kohsuke Sumiyoshi. "The influence of hyperon potential on the black-hole-forming failed supernovae." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2011. AIP, 2012. http://dx.doi.org/10.1063/1.4763425.

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Wehmeyer, Benjamin, Carla Fröhlich, Benoit Côté, Marco Pignatari, and Friedrich-Karl Thielemann. "Could Failed Supernovae Explain the High r-process Abundances in Some Low Metallicity Stars?" In Proceedings of the 15th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG15). Journal of the Physical Society of Japan, 2020. http://dx.doi.org/10.7566/jpscp.31.011063.

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Sumiyoshi, K., Chikako Ishizuka, Akira Ohnishi, Shoichi Yamada, and H. Suzuki. "Short neutrino burst from failed supernovae as a probe of dense matter with hyperon mixture." In 10th Symposium on Nuclei in the Cosmos. Sissa Medialab, 2009. http://dx.doi.org/10.22323/1.053.0122.

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