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Journal articles on the topic 'Failed supernova'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

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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5

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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6

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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7

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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8

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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9

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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10

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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11

Gould, Andrew, and Samir Salim. "Searching for Failed Supernovae with Astrometric Binaries." Astrophysical Journal 572, no. 2 (2002): 944–49. http://dx.doi.org/10.1086/340435.

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12

Fryer, Chris L., Peter J. Brown, Filomena Bufano, et al. "SPECTRA AND LIGHT CURVES OF FAILED SUPERNOVAE." Astrophysical Journal 707, no. 1 (2009): 193–207. http://dx.doi.org/10.1088/0004-637x/707/1/193.

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13

Kochanek, C. S. "FAILED SUPERNOVAE EXPLAIN THE COMPACT REMNANT MASS FUNCTION." Astrophysical Journal 785, no. 1 (2014): 28. http://dx.doi.org/10.1088/0004-637x/785/1/28.

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14

Fernández, Rodrigo, Eliot Quataert, Kazumi Kashiyama, and Eric R. Coughlin. "Mass ejection in failed supernovae: variation with stellar progenitor." Monthly Notices of the Royal Astronomical Society 476, no. 2 (2018): 2366–83. http://dx.doi.org/10.1093/mnras/sty306.

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15

Coughlin, Eric R., Eliot Quataert, Rodrigo Fernández, and Daniel Kasen. "A physical model of mass ejection in failed supernovae." Monthly Notices of the Royal Astronomical Society 477, no. 1 (2018): 1225–38. http://dx.doi.org/10.1093/mnras/sty667.

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16

Nakazato, Ken'ichiro, Shun Furusawa, Kohsuke Sumiyoshi, Akira Ohnishi, Shoichi Yamada, and Hideyuki Suzuki. "HYPERON MATTER AND BLACK HOLE FORMATION IN FAILED SUPERNOVAE." Astrophysical Journal 745, no. 2 (2012): 197. http://dx.doi.org/10.1088/0004-637x/745/2/197.

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17

MacFadyen, A. I., and S. E. Woosley. "Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”." Astrophysical Journal 524, no. 1 (1999): 262–89. http://dx.doi.org/10.1086/307790.

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18

Sumiyoshi, K., K. Nakazato, C. Ishizuka, A. Ohnishi, S. Yamada, and H. Suzuki. "Emergence of hyperons in failed supernovae with short neutrino bursts." Nuclear Physics A 835, no. 1-4 (2010): 295–302. http://dx.doi.org/10.1016/j.nuclphysa.2010.01.205.

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19

Kotake, Kei. "Gravitational-wave signatures in successful vs. failed core-collapse supernovae." Journal of Physics: Conference Series 314 (September 22, 2011): 012080. http://dx.doi.org/10.1088/1742-6596/314/1/012080.

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20

Plewa, Tomasz. "Detonating Failed Deflagration Model of Thermonuclear Supernovae. I. Explosion Dynamics." Astrophysical Journal 657, no. 2 (2007): 942–60. http://dx.doi.org/10.1086/511412.

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21

Kasen, Daniel, and Tomasz Plewa. "Detonating Failed Deflagration Model of Thermonuclear Supernovae. II. Comparison to Observations." Astrophysical Journal 662, no. 1 (2007): 459–71. http://dx.doi.org/10.1086/516834.

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22

Wehmeyer, B., C. Fröhlich, B. Côté, M. Pignatari, and F.-K. Thielemann. "Using failed supernovae to constrain the Galactic r-process element production." Monthly Notices of the Royal Astronomical Society 487, no. 2 (2019): 1745–53. http://dx.doi.org/10.1093/mnras/stz1310.

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ABSTRACT Rapid neutron capture process (r-process) elements have been detected in a large fraction of metal-poor halo stars, with abundances relative to iron (Fe) that vary by over two orders of magnitude. This scatter is reduced to less than a factor of 3 in younger Galactic disc stars. The large scatter of r-process elements in the early Galaxy suggests that the r-process is made by rare events, like compact binary mergers and rare sub-classes of supernovae. Although being rare, neutron star mergers alone have difficulties to explain the observed enhancement of r-process elements in the lowest metallicity stars compared to Fe. The supernovae producing the two neutron stars already provide a substantial Fe abundance where the r-process ejecta from the merger would be injected. In this work we investigate another complementary scenario, where the r-process occurs in neutron star-black hole mergers in addition to neutron star mergers. Neutron star-black hole mergers would eject similar amounts of r-process matter as neutron star mergers, but only the neutron star progenitor would have produced Fe. Furthermore, a reduced efficiency of Fe production from single stars significantly alters the age–metallicity relation, which shifts the onset of r-process production to lower metallicities. We use the high-resolution [(20 pc)3/cell] inhomogeneous chemical evolution tool ‘ICE’ to study the outcomes of these effects. In our simulations, an adequate combination of neutron star mergers and neutron star-black hole mergers qualitatively reproduces the observed r-process abundances in the Galaxy.

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23

Kochanek, Christopher S., John F. Beacom, Matthew D. Kistler, et al. "A Survey About Nothing: Monitoring a Million Supergiants for Failed Supernovae." Astrophysical Journal 684, no. 2 (2008): 1336–42. http://dx.doi.org/10.1086/590053.

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24

Jordan, George C., Hagai B. Perets, Robert T. Fisher, and Daniel R. van Rossum. "FAILED-DETONATION SUPERNOVAE: SUBLUMINOUS LOW-VELOCITY Ia SUPERNOVAE AND THEIR KICKED REMNANT WHITE DWARFS WITH IRON-RICH CORES." Astrophysical Journal 761, no. 2 (2012): L23. http://dx.doi.org/10.1088/2041-8205/761/2/l23.

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25

Sumiyoshi, K., C. Ishizuka, A. Ohnishi, S. Yamada, and H. Suzuki. "EMERGENCE OF HYPERONS IN FAILED SUPERNOVAE: TRIGGER OF THE BLACK HOLE FORMATION." Astrophysical Journal 690, no. 1 (2008): L43—L46. http://dx.doi.org/10.1088/0004-637x/690/1/l43.

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26

Gerke, J. R., C. S. Kochanek, and K. Z. Stanek. "The search for failed supernovae with the Large Binocular Telescope: first candidates." Monthly Notices of the Royal Astronomical Society 450, no. 3 (2015): 3289–305. http://dx.doi.org/10.1093/mnras/stv776.

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27

Ivanov, Mario, and Rodrigo Fernández. "Mass Ejection in Failed Supernovae: Equation of State and Neutrino Loss Dependence." Astrophysical Journal 911, no. 1 (2021): 6. http://dx.doi.org/10.3847/1538-4357/abe59e.

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28

Fraser, Morgan. "The progenitors of core-collapse supernovae." Proceedings of the International Astronomical Union 12, S329 (2016): 32–38. http://dx.doi.org/10.1017/s1743921317002885.

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AbstractLinking core-collapse SNe to their stellar progenitors is a major ongoing challenge. To date, H rich Type IIP SNe have been shown to come from red supergiants, while there is increasing evidence that the majority of stripped envelope SNe come from binary systems. The first candidates for failed SNe, where a massive star collapses to form a black hole without a bright optical display have been identified, while the range of outbursts and eruptions from pre-SN stars are just beginning to be revealed.

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29

Coughlin, Eric R., Eliot Quataert, and Stephen Ro. "Weak Shock Propagation with Accretion. I. Self-similar Solutions and Application to Failed Supernovae." Astrophysical Journal 863, no. 2 (2018): 158. http://dx.doi.org/10.3847/1538-4357/aad198.

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30

Quataert, E., D. Lecoanet, and E. R. Coughlin. "Black hole accretion discs and luminous transients in failed supernovae from non-rotating supergiants." Monthly Notices of the Royal Astronomical Society: Letters 485, no. 1 (2019): L83—L88. http://dx.doi.org/10.1093/mnrasl/slz031.

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ABSTRACT We show that for supergiants, net angular momentum is not a necessary condition for forming accretion discs during core collapse. Even absent net rotation, convective motions in the outer parts of supergiants generate mean horizontal flows at a given radius with velocities of ${\sim } 1 \, {\rm km \, s}^{-1}$; the direction of the mean flow will vary as a function of height through the convection zone. We confirm these analytic estimates using Cartesian Boussinesq convection simulations. These mean horizontal flows lead to a random angular momentum in supergiant convection zones that exceeds that of the last stable circular orbit of a black hole by a factor of ∼10. As a result, failed explosions of supergiants – in which the accretion shock on to the neutron star does not revive, leading to black hole formation – may often produce accretion discs that can power day–week (blue supergiants) or week–year (yellow and red supergiants) non-thermal and thermal transients through winds and jets. These transients will be especially time variable because the angular momentum of the accreting material will vary substantially in time. Observed sources such as Swift J1644+57, iPTF14hls, and SN 2018cow, as well as energetic Type II supernovae (OGLE-2014-SN-073), may be produced by this mechanism.

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31

Vincenzo, Fiorenzo, and Chiaki Kobayashi. "Extragalactic archaeology with the C, N, and O chemical abundances." Astronomy & Astrophysics 610 (February 2018): L16. http://dx.doi.org/10.1051/0004-6361/201732395.

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We predict how the C, N, and O abundances within the interstellar medium of galaxies evolve as functions of the galaxy star formation history (SFH). We adopt a hydrodynamical cosmological simulation, focusing on three star-forming disc galaxies with different SFHs. By assuming failed supernovae, we can predict an increasing trend of the gas-phase N/O–O/H abundance diagram, which was not produced in our previous simulations without failed supernovae. At high redshifts, contrary to the predictions of classical chemical evolution models with instantaneous mixing approximation, we find almost flat trends in the N/O–O/H diagram, which are due to the contribution of intermediate-mass stars together with an inhomogeneous chemical enrichment. Finally, we also predict that the average N/O and C/O steadily increase as functions of time, while the average C/N decreases, due to the mass and metallicity dependence of the yields of asymptotic giant branch stars; such variations are more marked during more intense star formation episodes. Our predictions on the CNO abundance evolution can be used to study the SFH of disc galaxies with the James Webb Space Telescope.

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32

Adams, S. M., C. S. Kochanek, J. R. Gerke, K. Z. Stanek, and X. Dai. "The search for failed supernovae with the Large Binocular Telescope: confirmation of a disappearing star." Monthly Notices of the Royal Astronomical Society 468, no. 4 (2017): 4968–81. http://dx.doi.org/10.1093/mnras/stx816.

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33

Sumiyoshi, K., S. Yamada, and H. Suzuki. "Dynamics and Neutrino Signal of Black Hole Formation in Nonrotating Failed Supernovae. II. Progenitor Dependence." Astrophysical Journal 688, no. 2 (2008): 1176–85. http://dx.doi.org/10.1086/592183.

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Adams, S. M., C. S. Kochanek, J. R. Gerke, and K. Z. Stanek. "The search for failed supernovae with the Large Binocular Telescope: constraints from 7 yr of data." Monthly Notices of the Royal Astronomical Society 469, no. 2 (2017): 1445–55. http://dx.doi.org/10.1093/mnras/stx898.

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35

Sumiyoshi, K., S. Yamada, and H. Suzuki. "Dynamics and Neutrino Signal of Black Hole Formation in Nonrotating Failed Supernovae. I. Equation of State Dependence." Astrophysical Journal 667, no. 1 (2007): 382–94. http://dx.doi.org/10.1086/520876.

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36

Rhode, Katherine L., John J. Salzer, and David J. Westpfahl. "What Causes the HI Holes in Gas-Rich LSB Dwarfs?" International Astronomical Union Colloquium 171 (1999): 221–23. http://dx.doi.org/10.1017/s0252921100054361.

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AbstractWe have carried out a deep, multi-color imaging study of Holmberg II (Ho II) and several other nearby LSB dwarf galaxies for which detailed HI maps exist. The formation of the HI holes in these galaxies has been attributed to multiple supernovae (SNe) occurring within windblown shells around young, massive star clusters. To search for evidence of the clusters, we have compared optical images with the HI maps and measured magnitudes and colors of objects in and around the HI holes.Although the SN scenario requires that detectable star clusters should often be present in the centers of the HI holes, our observations have in most cases failed to reveal these clusters at the expected magnitudes. In fact, many of the HI holes are located in regions of very low optical surface brightness, which show no evidence of recent star formation.

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37

Prieto, J. L., K. Z. Stanek, C. S. Kochanek, and D. R. Weisz. "LBT Discovery of a Yellow Supergiant Eclipsing Binary in the Dwarf Galaxy Holmberg IX." Proceedings of the International Astronomical Union 3, S250 (2007): 333–38. http://dx.doi.org/10.1017/s1743921308020668.

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AbstractIn a variability survey of M81 using the Large Binocular Telescope we have discovered a peculiar eclipsing binary (MV ≃ −7.1) in the field of the dwarf galaxy Holmberg IX. It has a period of 271 days and the light curve is well-fit by an overcontact model in which both stars are overflowing their Roche lobes. It is composed of two yellow supergiants (V − I ≃ 1 mag, Teff = 4800 K), rather than the far more common red or blue supergiants. Such systems must be rare. While we failed to find any similar systems in the literature, we did, however note a second example. The SMC F0 supergiant R47 is a bright (MV ≃ −7.5) periodic variable whose All Sky Automated Survey (ASAS) light curve is well-fit as a contact binary with a 181 day period. We propose that these massive systems are the progenitors of supernovae like SN 2004et and SN 2006ov, which appeared to have yellow progenitors. The binary interactions (mass transfer, mass loss) limit the size of the supergiant to give it a higher surface temperature than an isolated star at the same core evolutionary stage.

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38

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 large-scale perturbations in the convective Si and O burning shells. 3D simulations have also achieved to follow neutrino-driven explosions continuously from the initiation of the blast wave, through the shock breakout from the progenitor surface, into the radioactively powered evolution of the SN, and towards the free expansion phase of the emerging remnant. Here we present results from such simulations, which form the basis for direct comparisons with observations of SNe and SN remnants in order to derive constraints on the still disputed explosion mechanism. It is shown that predictions based on hydrodynamic instabilities and mixing processes associated with neutrino-driven explosions yield good agreement with measured NS kicks, light-curve properties of SN 1987A and asymmetries of iron and 44Ti distributions observed in SN 1987A and Cassiopeia A.

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Gänsicke, Boris T., Detlev Koester, Roberto Raddi, Odette Toloza, and S. O. Kepler. "SDSS J124043.01+671034.68: the partially burned remnant of a low-mass white dwarf that underwent thermonuclear ignition?" Monthly Notices of the Royal Astronomical Society 496, no. 4 (2020): 4079–86. http://dx.doi.org/10.1093/mnras/staa1761.

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ABSTRACT The white dwarf SDSS J124043.01+671034.68 (SDSS J1240+6710) was previously found to have an oxygen-dominated atmosphere with significant traces of neon, magnesium, and silicon. A possible origin via a violent late thermal pulse or binary interactions has been suggested to explain this very unusual photospheric composition. We report the additional detection of carbon, sodium, and aluminium in far-ultraviolet and optical follow-up spectroscopy. No iron-group elements are detected, with tight upper limits on titanium, iron, cobalt, and nickel, suggesting that the star underwent partial oxygen burning, but failed to ignite silicon burning. Modelling the spectral energy distribution and adopting the distance based on the Gaia parallax, we infer a low white dwarf mass, $M_\mathrm{wd}=0.41\pm 0.05\, \mathrm{M}_\odot$. The large space velocity of SDSS J1240+6710, computed from the Gaia proper motion and its radial velocity, is compatible with a Galactic rest-frame velocity of ≃ 250 km s−1 in the opposite direction with respect to the Galactic rotation, strongly supporting a binary origin of this star. We discuss the properties of SDSS J1240+6710 in the context of the recently identified survivors of thermonuclear supernovae, the D6 and LP 40−365 stars, and conclude that it is unlikely related to either of those two groups. We tentatively suggest that SDSS J1240+6710 is the partially burned remnant of a low-mass white dwarf that underwent a thermonuclear event.

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Rajwade, K. M., M. B. Mickaliger, B. W. Stappers, et al. "Limits on absorption from a 332-MHz survey for fast radio bursts." Monthly Notices of the Royal Astronomical Society 493, no. 3 (2020): 4418–27. http://dx.doi.org/10.1093/mnras/staa616.

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ABSTRACT Fast radio bursts (FRBs) are bright, extragalactic radio pulses whose origins are still unknown. Until recently, most FRBs have been detected at frequencies greater than 1 GHz with a few exceptions at 800 MHz. The recent discoveries of FRBs at 400 MHz from the Canadian Hydrogen Intensity Mapping Experiment (CHIME) telescope have opened up possibilities for new insights about the progenitors while many other low-frequency surveys in the past have failed to find any FRBs. Here, we present results from an FRB survey recently conducted at the Jodrell Bank Observatory at 332 MHz with the 76-m Lovell telescope for a total of 58 d. We did not detect any FRBs in the survey and report a 90${{\ \rm per\ cent}}$ upper limit of 5500 FRBs per day per sky for a Euclidean Universe above a fluence threshold of 46 Jy ms. We discuss the possibility of absorption as the main cause of non-detections in low-frequency (&lt;800 MHz) searches and invoke different absorption models to explain the same. We find that Induced Compton Scattering alone cannot account for absorption of radio emission and that our simulations favour a combination of Induced Compton Scattering and Free-Free Absorption to explain the non-detections. For a free–free absorption scenario, our constraints on the electron density are consistent with those expected in the post-shock region of the ionized ejecta in superluminous supernovae.

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Hicks, E. P. "Rayleigh–Taylor unstable flames at higher Reynolds number." Monthly Notices of the Royal Astronomical Society 489, no. 1 (2019): 36–51. http://dx.doi.org/10.1093/mnras/stz2080.

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ABSTRACT Rayleigh–Taylor (RT) unstable flames are a key component of Type Ia and Iax supernovae explosions, but their complex hydrodynamics is still not well understood. These flames are affected not only by the RT instability, but also by the turbulence it generates. Both processes can increase the flame speed by stretching and wrinkling the flame. This makes it hard to choose a subgrid model for the flame speed in full star Type Ia or Iax simulations. Commonly used subgrid models get around this difficulty by assuming that either the RT instability or turbulence is dominant and sets the flame speed. In previous work, we evaluated the physical assumptions and predictive abilities of these two types of models by analysing a large parameter study of 3D direct numerical simulations of RT unstable flames. Surprisingly, we found that the flame dynamics is dominated by the RT instability and that RT unstable flames are very different from turbulent flames. In particular, RT unstable flames are thinner rather than thicker when turbulence is strong. In addition, none of the turbulent flame speed models adequately predicted the flame speed. We also showed that the RT flame speed model failed when the RT instability was strong, suggesting that geometrical burning effects also influence the flame speed. However, these results depended on simulations with Re ≲ 720. In this paper, we extend the parameter study to higher Reynolds number and show that the basic conclusions of our previous study still hold when the RT-generated turbulence is stronger.

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White, Simon D. M. "Simulations of Disk Galaxy Formation in their Cosmological Context." Proceedings of the International Astronomical Union 4, S254 (2008): 19–20. http://dx.doi.org/10.1017/s1743921308027336.

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AbstractTogether with the discovery of the accelerated expansion of the present Universe and measurements of large-scale structure at low redshift, observations of the cosmic microwave background have established a standard paradigm in which all cosmic structure grew from small fluctuations generated at very early times in a flat universe which today consists of 72% dark energy, 23.5% dark matter and 4.5% ordinary baryons. The CMB sky provides us with a direct image of this universe when it was 400,000 years old and very nearly uniform. The galaxy formation problem is then to understand how observed galaxies with all their regularity and diversity arose from these very simple initial conditions. Although gravity is the prime driver, many physical processes appear to play an important role in this transformation, and direct numerical simulation has become the principal tool for detailed investigation of the complex and strongly nonlinear interactions between them.The evolution of structure in the gravitationally dominant Cold Dark Matter distribution can now be simulated in great detail, provided the effects of the baryons are ignored, and there is general consensus for the results on scales relevant to the formation of galaxies like our own. The basic nonlinear units are so-called “dark matter halos”, slowly rotating, triaxial, quasi-equilibrium systems with a universal cusped density profile and substantial substructure in the form of a host of much less massive subhalos which are concentrated primarily in their outer regions.Attempts to include the baryons, and so to model the formation of the visible parts of galaxies, have given much more diverse results. It has been known for 30 years that substantial feedback, presumably from stellar winds and supernovae, is required to prevent overcooling of gas and excessive star formation in the early stages of galaxy assembly. When realistic galaxy formation simulations first became possible in the early 1990's, this problem was immediately confirmed. Without effective feedback, typical halos produced galaxies which were too massive, too concentrated and had too little disk to be consistent with observation.Simple models for disk formation from the mid 1990's show that the angular momentum predicted for collapsing dark halos is sufficient for them to build a disk population similar to that observed. Direct simulations have repeatedly failed to confirm this picture, however, because nonlinear effects lead to substantial transfer of angular momentum between the various components. In most cases the condensing baryonic material loses angular momentum to the dark matter, and the final galaxy ends up with a disk that is too compact or contains too small a fraction of the stars.These problems have been reduced as successive generations of simulations have dramatically improved the numerical resolution and have introduced “better” implementations of feedback (i.e. more successful at building disks). Despite this, no high-resolution simulation has so far been able to produce a present-day disk galaxy with a bulge-to-disk mass ratio much less than one in a proper ΛCDM context. Such galaxies are common in the real Universe; our own Milky Way is a good example. The variety of results obtained by different groups show that this issue is very sensitive to how star formation and feedback are treated, and all implementations of these processes to date have been much too schematic to be confident of their predictions.The major outstanding issues I see related to disk galaxies and their formation are the following: Do real disk galaxies have the NFW halos predicted by the ΛCDM cosmology? If not, could the deviations have been produced by the formation of the observed baryonic components, or must the basic structure formation picture be changed? How are Sc and later type galaxies made? Why don't our simulations produce them? What determines which galaxies become barred and which not? Can we demonstrate that secular evolution produces the observed population of (pseudo)bulges from pre-existing disks? How does the observed population of thin disks survive bombardment by substructure and the other transient potential fluctuations expected in ΛCDM halos? Is a better treatment of feedback really the answer? If so, can we demonstrate it using chemical abundances as fossil tracers? And how can we best use observations at high redshift to clarify these formation issues?

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Neustadt, J. M. M., C. S. Kochanek, K. Z. Stanek, et al. "The search for failed supernovae with the Large Binocular Telescope: a new candidate and the failed SN fraction with 11 yr of data." Monthly Notices of the Royal Astronomical Society, September 13, 2021. http://dx.doi.org/10.1093/mnras/stab2605.

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Abstract We present updated results of the Large Binocular Telescope Search for Failed Supernovae. This search monitors luminous stars in 27 nearby galaxies with a current baseline of 11 yr of data. We re-discover the failed supernova (SN) candidate N6946-BH1 as well as a new candidate, M101-OC1. M101-OC1 is a blue supergiant that rapidly disappears in optical wavelengths with no evidence for significant obscuration by warm dust. While we consider other options, a good explanation for the fading of M101-OC1 is a failed SN, but follow-up observations are needed to confirm this. Assuming only one clearly detected failed SN, we find a failed SN fraction $f = 0.16^{+0.23}_{-0.12}$ at 90 per cent confidence. We also report on a collection of stars that show slow (∼decade), large amplitude (ΔL/L &gt; 3) luminosity changes.

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Mühlbeier, T., H. Nunokawa, and R. Zukanovich Funchal. "Revisiting the triangulation method for pointing to supernova and failed supernova with neutrinos." Physical Review D 88, no. 8 (2013). http://dx.doi.org/10.1103/physrevd.88.085010.

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"Failed stellar bombs hint at supernova tipping point." New Scientist 204, no. 2735 (2009): 17. http://dx.doi.org/10.1016/s0262-4079(09)63049-9.

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"Disappearing star might be first known failed supernova." Physics Today, 2016. http://dx.doi.org/10.1063/pt.5.0210116.

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Doherty, Carolyn L., Pilar Gil-Pons, Lionel Siess, and John C. Lattanzio. "Super-AGB Stars and their Role as Electron Capture Supernova Progenitors." Publications of the Astronomical Society of Australia 34 (2017). http://dx.doi.org/10.1017/pasa.2017.52.

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AbstractWe review the lives, deaths and nucleosynthetic signatures of intermediate-mass stars in the range ≈6–12 M⊙, which form super-AGB stars near the end of their lives. The critical mass boundaries both between different types of massive white dwarfs (CO, CO–Ne, ONe), and between white dwarfs and supernovae, are examined along with the relative fraction of super-AGB stars that end life either as an ONe white dwarf or as a neutron star (or an ONeFe white dwarf), after undergoing an electron capture supernova event. The contribution of the other potential single-star channel to electron-capture supernovae, that of the failed massive stars, is also discussed. The factors that influence these different final fates and mass limits, such as composition, rotation, the efficiency of convection, the nuclear reaction rates, mass-loss rates, and third dredge-up efficiency, are described. We stress the importance of the binary evolution channels for producing electron-capture supernovae. Recent nucleosynthesis calculations and elemental yield results are discussed and a new set of s-process heavy element yields is presented. The contribution of super-AGB star nucleosynthesis is assessed within a Galactic perspective, and the (super-)AGB scenario is considered in the context of the multiple stellar populations seen in globular clusters. A brief summary of recent works on dust production is included. Last, we conclude with a discussion of the observational constraints and potential future advances for study into these stars on the low mass/high mass star boundary.

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Smartt, S. J. "Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars." Publications of the Astronomical Society of Australia 32 (2015). http://dx.doi.org/10.1017/pasa.2015.17.

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AbstractOver the last 15 years, the supernova community has endeavoured to directly identify progenitor stars for core-collapse supernovae discovered in nearby galaxies. These precursors are often visible as resolved stars in high-resolution images from space-and ground-based telescopes. The discovery rate of progenitor stars is limited by the local supernova rate and the availability and depth of archive images of galaxies, with 18 detections of precursor objects and 27 upper limits. This review compiles these results (from 1999 to 2013) in a distance-limited sample and discusses the implications of the findings. The vast majority of the detections of progenitor stars are of type II-P, II-L, or IIb with one type Ib progenitor system detected and many more upper limits for progenitors of Ibc supernovae (14 in all). The data for these 45 supernovae progenitors illustrate a remarkable deficit of high-luminosity stars above an apparent limit of logL/L⊙ ≃ 5.1 dex. For a typical Salpeter initial mass function, one would expect to have found 13 high-luminosity and high-mass progenitors by now. There is, possibly, only one object in this time- and volume-limited sample that is unambiguously high-mass (the progenitor of SN2009ip) although the nature of that supernovae is still debated. The possible biases due to the influence of circumstellar dust, the luminosity analysis, and sample selection methods are reviewed. It does not appear likely that these can explain the missing high-mass progenitor stars. This review concludes that the community’s work to date shows that the observed populations of supernovae in the local Universe are not, on the whole, produced by high-mass (M ≳ 18 M⊙) stars. Theoretical explosions of model stars also predict that black hole formation and failed supernovae tend to occur above an initial mass of M ≃ 18 M⊙. The models also suggest there is no simple single mass division for neutron star or black-hole formation and that there are islands of explodability for stars in the 8–120 M⊙ range.The observational constraints are quite consistent with the bulk of stars above M ≳ 18 M⊙ collapsing to form black holes with no visible supernovae.

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Nakazato, Ken’ichiro, Kohsuke Sumiyoshi, Hideyuki Suzuki, and Shoichi Yamada. "Oscillation and future detection of failed supernova neutrinos from a black-hole-forming collapse." Physical Review D 78, no. 8 (2008). http://dx.doi.org/10.1103/physrevd.78.083014.

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Fischer, Tobias. "QCD phase transition drives supernova explosion of a very massive star." European Physical Journal A 57, no. 9 (2021). http://dx.doi.org/10.1140/epja/s10050-021-00571-z.

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AbstractThe nature of core-collapse supernova (SN) explosions is yet incompletely understood. The present article revisits the scenario in which the release of latent heat due to a first-order phase transition, from normal nuclear matter to the quark–gluon plasma, liberates the necessary energy to explain the observed SN explosions. Here, the role of the metallicity of the stellar progenitor is investigated, comparing a solar metallicity and a low-metallicity case, both having a zero-age main sequence (ZAMS) mass of 75 M$$_\odot $$ ⊙ . It is found that low-metallicity models belong exclusively to the failed SN branch, featuring the formation of black holes without explosions. It excludes this class of massive star explosions as possible site for the nucleosynthesis of heavy elements at extremely low metallicity, usually associated with the early universe.

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