To see the other types of publications on this topic, follow the link: Close — supernovae.
Journal articles on the topic 'Close — supernovae'
Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles
Consult the top 50 journal articles for your research on the topic 'Close — supernovae.'
Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.
You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.
Browse journal articles on a wide variety of disciplines and organise your bibliography correctly.
1
Uenishi, Tatsuhiro, Ken'ichi Nomoto, and Izumi Hachisu. "Evolution of Rotating White Dwarfs in Close Binaries and Diversity of Type Ia Supernovae." Symposium - International Astronomical Union 208 (2003): 459–60. http://dx.doi.org/10.1017/s0074180900207754.
Full textAbstract:
Type Ia supernovae are very good, but not perfect, standard candles, because their observed brightness shows a little diversity. The origin of this dibersity needs to be understood for the application to cosmology.In close binary systems, a white dwarf must be rotating faster and faster as it gains angular momentum from the accretion disk. Its rapid rotation affects its final mass and strucure just before a supernova expolosion. Brightness of supernovae can be changed if mass of their progenitors have some diversity.
2
Joss, P. C. "Type II Supernovae in Binary Systems." Symposium - International Astronomical Union 165 (1996): 141–49. http://dx.doi.org/10.1017/s0074180900055637.
Full textAbstract:
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.
3
Nomoto, K., K. Iwamoto, T. Suzuki, et al. "The Origin of Type Ib-Ic-IIb-IIL Supernovae and Binary Star Evolution." Symposium - International Astronomical Union 165 (1996): 119–34. http://dx.doi.org/10.1017/s0074180900055613.
Full textAbstract:
Supernovae are classified as type I and type II and further subdivided into Ia, Ib, Ic, II-P, II-L, and IIb. The origin of this observational diversity has not been well understood. The recent nearby supernovae SN 1993J and SN 1994I have provided particularly useful material to clarify the supernova — progenitor connection. For a progenitor of type IIb supernova 1993J, we propose that merging of two stars in a close binary is responsible for the formation of a thin H-rich envelope. As a progenitor of type Ic supernova 1994I, we propose a bare C+O star that has lost both its H and He envelope after a common-envelope phase. By generalizing these scenarios, we show that common-envelope evolution in massive close binary stars leads to various degrees of stripping off of the envelope of a massive star. This naturally leads to an explanation of the origin of type II-L, IIn, IIb, Ib, and Ic in a unified manner. The binary hypothesis to explain the diversity of supernovae can be substantiated with new information on SN IIb 1993J and SN Ic 1994I. Model light curves are compared with observations. Since extensive mass loss is essential for the binary scenario, circumstellar interactions are examined for comparison with X-ray observations.
4
Angloher, G., M. R. Bharadwaj, M. Cababie, et al. "Neutrino flux sensitivity to the next galactic core-collapse supernova in COSINUS." Journal of Cosmology and Astroparticle Physics 2025, no. 03 (2025): 037. https://doi.org/10.1088/1475-7516/2025/03/037.
Full textAbstract:
Abstract While neutrinos are often treated as a background for many dark matter experiments, these particles offer a new avenue for physics: the detection of core-collapse supernovae. Supernovae are extremely energetic, violent and complex events that mark the death of massive stars. During their collapse stars emit a large number of neutrinos in a short burst. These neutrinos carry 99% of the emitted energy which makes their detection fundamental in understanding supernovae. This paper illustrates how COSINUS (Cryogenic Observatory for SIgnatures seen in Next-generation Underground Searches), a sodium iodide (NaI) based dark matter search, will be sensitive to the next galactic core-collapse supernova. The experiment is composed of two separate detectors which will respond to far away and nearby supernovae. The inner core of the experiment will consist of NaI crystals operating as scintillating calorimeters. These crystals will mainly be sensitive to the Coherent Elastic Neutrino-Nucleus Scattering (CEνNS) against Na and I nuclei. The low mass of the cryogenic detectors enables the experiment to identify close supernovae within 1 kpc without pileup. The crystals will see up to hundreds of CEνNS events from a supernova happening at 200 pc. They reside at the center of a large cylindrical 230 T water tank, instrumented with 30 photomultiplier tubes. This tank acts simultaneously as a passive and active shield able to detect the Cherenkov radiation induced by impinging charged particles from ambient and cosmogenic radioactivity. A supernova near the Milky Way Center (10 kpc) will be easily detected inducing ∼60 measurable events, and the water tank will have a 3σ sensitivity to supernovae up to 22 kpc, seeing ∼10 events. This paper shows how, even without dedicated optimization, modern dark matter experiments will also be able to play their part in the multi-messenger effort to detect the next galactic core-collapse supernova.
5
Sternberg, Assaf. "Evidence for Circumstellar Material in Type Ia Supernovae via Sodium Absorption Features." Proceedings of the International Astronomical Union 7, S281 (2011): 299–302. http://dx.doi.org/10.1017/s1743921312015232.
Full textAbstract:
AbstractType Ia supernovae are very good tools for measuring distances on a cosmic scale. The consensus view is that mass transfer onto a white dwarf in a close binary system leads to a thermonuclear explosion, though the nature of the mass donor is still uncertain. In the single-degenerate model it is a main-sequence star or an evolved star. In the double-degenerate model it is another white dwarf. We study the velocity structure of absorbing material along the line of sight to 35 Type Ia supernovae and find a statistical preference for blueshifted structures, likely arising in gas outflows from the supernova progenitor systems, consistent with a single-degenerate progenitor for a substantial fraction of Type Ia supernovae in nearby spiral galaxies.
6
Meynet, G., J. Groh, C. Georgy, H. Saio, and R. Kudritzki. "Supernovae from yellow, blue supergiants: origin and consequences for stellar evolution." Proceedings of the International Astronomical Union 11, A29B (2015): 211. http://dx.doi.org/10.1017/s1743921316004932.
Full textAbstract:
AbstractA few core collapse supernovae progenitors have been found to be yellow or blue supergiants. Weshall discuss possible scenarios involving single and close binary evolution allowing to explain this kind of corecollapse supernova progenitors. According to stellar models for both single and close binaries, blue supergiants, at theend of their nuclear lifetimes and thus progenitors of core collapse supernovae, present very different characteristicsfor what concerns their surface compositions, rotational surface velocities and pulsational properties with respect toblue supergiants in their core helium burning phase. We discuss how the small observed scatter of the flux-weightedgravity-luminosity (FWGL) relation of blue supergiants constrains the evolution of massive stars after the Main-Sequence phase and the nature of the progenitors of supernovae in the mass range between 12 and 40 solarmasses. The present day observed surface abundances of blue supergiants, of their pulsational properties, as well asthe small scatter of the FWGL relation provide strong constraints on both internal mixing and mass loss in massivestars and therefore on the end point of their evolution.
7
de Angelis, Alessandro, and Selenia Broccio. "First Observations of SN 1604 (Kepler’s Supernova)." Universe 7, no. 11 (2021): 430. http://dx.doi.org/10.3390/universe7110430.
Full textAbstract:
A supernova close enough to the Earth is a spectacular event: it can appear as a “new star” as luminous as Venus, or even more, visible for several days. The rate of Galactic supernovae is expected to be of about one in 30 years, with a fraction visible to the naked eye; however in all the history of human civilization only seven supernovae in the Milky Way have been reported, the last two (1572 and 1604) during Galilei’s life. The supernova of 1604, today called Kepler’s Supernova, was observed by Galilei, Kepler and other astronomers in Europe, Korea, China, Arabia. Like the supernova SN1572, today called Tycho’s supernova, it has been the subject of extensive studies, and inspired observational measurements and philosophical considerations on the nature of the heavens. The remnant of SN1604 has been indicated by recent X- and gamma-ray data to be a likely site of cosmic ray acceleration. The first recorded data of optical observations, together with new data, can still tell us a lot about the early evolution of this supernova.
8
Arbutina, B., D. Urošević, and B. Vukotić. "High supernova rate and enhanced star-formation triggered in M81-M82 encounter." Proceedings of the International Astronomical Union 2, S237 (2006): 391. http://dx.doi.org/10.1017/s1743921307001792.
Full textAbstract:
It is a general belief that the starburst activity of a nearby galaxy M82 was triggered in a close encounter with its massive companion M81, a few tens of million years ago. Despite the lack of supernovae observed, multiwavelength radio observations of M82 discovered a considerable number of compact supernova remnant candidates. We use these remnants to estimate the supernova rate (SNR) and the enhanced star-formation (SFR) rate in M82, and compare them with rates in normal galaxies.
9
Napiwotzki, R., C. Karl, G. Nelemans, et al. "Close Binary White Dwarfs and Supernovae la." International Astronomical Union Colloquium 194 (2004): 113–16. http://dx.doi.org/10.1017/s0252921100152121.
Full textAbstract:
AbstractWe report on the current status of radial velocity surveys for white dwarf binaries (double degenerates DDs) including SPY (ESO Supernovae la progenitor survey) recently carried out at the VLT. A large sample of DD will allow us to put strong constraints on the phases of close binary evolution of the progenitor systems and to perform an observational test of the DD scenario for Supernovae of type Ia.
10
PAULUCCI, L., and J. E. HORVATH. "NU-PROCESS IN EXOTIC MODELS." International Journal of Modern Physics D 19, no. 08n10 (2010): 1731–35. http://dx.doi.org/10.1142/s0218271810017238.
Full textAbstract:
The exact physical conditions generating the abundances of r-elements in environments such as supernovae explosions are still under debate. We evaluated the characteristics expected for the neutrino wind in the proposed model of type-II supernova driven by conversion of nuclear matter to strange matter. Neutrinos will change the final abundance of elements after freeze out of r-process nucleosynthesis, specially those close to mass peaks.
11
Fink, M., M. Kromer, W. Hillebrandt, et al. "Thermonuclear explosions of rapidly differentially rotating white dwarfs: Candidates for superluminous Type Ia supernovae?" Astronomy & Astrophysics 618 (October 2018): A124. http://dx.doi.org/10.1051/0004-6361/201833475.
Full textAbstract:
The observed sub-class of “superluminous” Type Ia supernovae lacks a convincing theoretical explanation. If the emission of such objects were powered exclusively by radioactive decay of 56Ni formed in the explosion, a progenitor mass close to or even above the Chandrasekhar limit for a non-rotating white dwarf star would be required. Masses significantly exceeding this limit can be supported by differential rotation. We, therefore, explore explosions and predict observables for various scenarios resulting from differentially rotating carbon–oxygen white dwarfs close to their respective limit of stability. Specifically, we have investigated a prompt detonation model, detonations following an initial deflagration phase (“delayed detonation” models), and a pure deflagration model. In postprocessing steps, we performed nucleosynthesis and three-dimensional radiative transfer calculations, that allow us, for the first time, to consistently derive synthetic observables from our models. We find that all explosion scenarios involving detonations produce very bright events. The observables predicted for them, however, are inconsistent with any known subclass of Type Ia supernovae. Pure deflagrations resemble 2002cx-like supernovae and may contribute to this class. We discuss implications of our findings for the explosion mechanism and for the existence of differentially rotating white dwarfs as supernova progenitors.
12
Ray, Alak, Sayan Chakraborti, Naveen Yadav, Randall Smith, Poonam Chandra, and David Pooley. "A tale of two shocks in SN 2004dj." Proceedings of the International Astronomical Union 9, S296 (2013): 108–11. http://dx.doi.org/10.1017/s1743921313009319.
Full textAbstract:
AbstractType IIP SNe constitute a major fraction of all core-collapse supernovae and arise from massive stars that end their lives close to Red Supergiants. The blastwave from the SN interacting with the progenitor's circumstellar matter produces a hot region bounded by a forward and a reverse shock from which most of the X-ray emission originates. Analysis of archival Chandra observations of SN 2004dj, one of the nearest supernovae since SN 1987A, together with published data from radio and optical bands determines the pre-explosion mass-loss rate, blastwave speed, electron acceleration and magnetic field amplification efficiencies. X-ray emission arises from both inverse Compton scattering by non-thermal electrons accelerated in the forward shock and from thermal emission from the supernova ejecta hit by the reverse shock. Determination of the properties of the radiating plasma based on the separation of thermal and non-thermal radiation differentiates different types of supernovae and their environments.
13
Langer, Norbert, and Alexander Heger. "Evolution and explosion of Wolf-Rayet stars." Symposium - International Astronomical Union 193 (1999): 187–95. http://dx.doi.org/10.1017/s0074180900205299.
Full textAbstract:
We investigate the pre-supernova evolution of Wolf-Rayet stars. We discuss whether the separation of hydrogen-free, core collapse supernovae into Type Ic and Type Ib supernovae is related to the occurrence of ‘Case BB mass transfer’ in massive close binaries, especially since the new, smaller WR mass loss rates do not favor helium-poor progenitor models from massive single stars. We also discuss the influence of rotation on the formation, evolution and explosion of WR stars using new models for rotating massive stars that have been computed from zero age to core collapse. We compute the spin-down of (non-magnetic) WR stars due to their strong mass loss, and compare pulsar spin rates with our predictions. Finally, we discuss implications of our results for the rotation rate of Type Ib/c supernova progenitors in general, and for SN 1998bw and the ‘collapsar’ model for γ-ray bursts in particular.
14
Vieyro, F. L., V. Bosch-Ramon, and N. Torres-Albà. "Non-thermal emission resulting from a supernova explosion inside an extragalactic jet." Astronomy & Astrophysics 622 (February 2019): A175. http://dx.doi.org/10.1051/0004-6361/201833319.
Full textAbstract:
Context. Core-collapse supernovae are found in galaxies with ongoing star-formation. In a starburst galaxy hosting an active galactic nucleus with a relativistic jet, supernovae can take place inside the jet. The collision of the supernova ejecta with the jet flow is expected to lead to the formation of an interaction region, in which particles can be accelerated and produce high-energy emission. Aims. We study the non-thermal radiation produced by electrons accelerated as a result of a supernova explosion inside the jet of an active galactic nucleus within a star-forming galaxy. Methods. We first analyzed the dynamical evolution of the supernova ejecta impacted by the jet. Then, we explored the parameter space using simple prescriptions for the observed gamma-ray lightcurve. Finally, the synchrotron and the inverse Compton spectral energy distributions for two types of sources, a radio galaxy and a powerful blazar, are computed. Results. For a radio galaxy, the interaction between a supernova and a jet of power ∼1043 − 1044 erg s−1 can produce apparent gamma-ray luminosities of ∼1042 − 1043 erg s−1, with an event duty cycle of supernova remnant interacting with the jet close to one for one galaxy. For a blazar with a powerful jet of ∼1046 erg s−1, the jet-supernova ejecta interaction could produce apparent gamma-ray luminosities of ∼1043 − 1044 erg s−1, but with a much lower duty cycle. Conclusions. The interaction of supernovae with misaligned jets of moderate power can be relatively frequent, and can result in steady gamma-ray emission potentially detectable for sources in the local universe. For powerful blazars much farther away, the emission would be steady as well, and it might be detectable under very efficient acceleration, but the events would be rather infrequent.
15
Nazaryan, T. A., A. R. Petrosian, A. A. Hakobyan, et al. "Supernovae in paired galaxies." Proceedings of the International Astronomical Union 9, S304 (2013): 351–52. http://dx.doi.org/10.1017/s1743921314004281.
Full textAbstract:
AbstractWe investigate the influence of close neighbor galaxies on the properties of supernovae (SNe) and their host galaxies using 56 SNe located in pairs of galaxies with different levels of star formation (SF) and nuclear activity. The mean distance of type II SNe from nuclei of hosts is greater by about a factor of 2 than that of type Ibc SNe. The distributions and mean distances of SNe are consistent with previous results compiled with the larger sample. For the first time it is shown that SNe Ibc are located in pairs with significantly smaller difference of radial velocities between components than pairs containing SNe Ia and II. We consider this as a result of higher star formation rate (SFR) of these closer systems of galaxies.
16
Poelarends, Arend J. T., Scott Wurtz, James Tarka, L. Cole Adams, and Spencer T. Hills. "Electron Capture Supernovae from Close Binary Systems." Astrophysical Journal 850, no. 2 (2017): 197. http://dx.doi.org/10.3847/1538-4357/aa988a.
Full text
17
Smith, Nathan. "Episodic Mass Loss and Pre-SN Circumstellar Envelopes." Proceedings of the International Astronomical Union 3, S250 (2007): 193–200. http://dx.doi.org/10.1017/s1743921308020498.
Full textAbstract:
AbstractI discuss observational clues concerning episodic mass-loss properties of massive stars in the time before the final supernova explosion. In particular, I will focus on the mounting evidence that LBVs and related stars are candidates for supernova progenitors, even though current paradigms place them at the end of core-H burning. Namely, conditions in the immediate circumstellar environment within a few 102 AU of Type IIn supernovae require very high progenitor mass-loss rates. Those rates are so high that the only known stars that come close are LBVs during rare giant eruptions. I will highlight evidence from observations of some recent extraordinary supernovae suggesting that explosive or episodic mass loss (a.k.a. LBV eruptions like the 19th century eruption of Eta Car) occur in the 5-10 years immediately preceding the SN. Finally, I will discuss some implications for stellar evolution from these SNe, the most important of which is the observational fact that the most massive stars can indeed make it to the ends of their lives with substantial H envelopes intact, even at Solar metallicity.
18
Filippenko, Alexei V., Thomas Matheson, and Luis C. Ho. "The ``Type IIb'' Supernova 1993J in M81: A Close Relative of Type Ib Supernovae." Astrophysical Journal 415 (October 1993): L103. http://dx.doi.org/10.1086/187043.
Full text
19
Lopez, R., J. Isern, J. Labay, and R. Canal. "Explosion of White Dwarfs." International Astronomical Union Colloquium 93 (1987): 413–17. http://dx.doi.org/10.1017/s0252921100105147.
Full textAbstract:
AbstractWe present models for Type I supernova light curves based on the explosion of partially solid white dwarfs in close binary systems. Studies of such explosions show that they leave bound remnants of different size. Our results reproduce quite well the maximun luminosities, the expansion velocities and the shape of the light curve. As the two basic papameters that govern the light curve, the ejected mass and the mass of 56Ni produced, are variable our models reproduce the slow and fast subclasses of “classical” Type I supernovae.
20
Cheng, Qiao-Bin, Chao-Jun Feng, Xiang-Hua Zhai, and Xin-Zhou Li. "Artificial neural network spectral light curve template for type Ia supernovae and its cosmological constraints." Modern Physics Letters A 36, no. 21 (2021): 2150149. http://dx.doi.org/10.1142/s0217732321501492.
Full textAbstract:
The spectral energy distribution (SED) sequence for type Ia supernovae (SN Ia) is modeled by an artificial neural network. The SN Ia luminosity is characterized as a function of phase, wavelength, a color parameter and a decline rate parameter. After training and testing the neural network, the SED sequence could give both the spectrum with wavelength range from 3000 Åto 8000 Åand the light curve with phase from 20 days before to 50 days after the maximum luminosity for the supernovae with different colors and decline rates. Therefore, we call this the Artificial Neural Network Spectral Light Curve Template (ANNSLCT) model. We retrain the Joint Light-curve Analysis (JLA) supernova sample by using the ANNSLCT model and obtain the parameters for each supernova to make a constraint on the cosmological [Formula: see text]CDM model. We find that the best fitting values of these parameters are very close to those from the JLA sample trained with the Spectral Adaptive Lightcurve Template 2 (SALT2) model. It is expectable that the ANNSLCT model has potential to analyze more SN Ia multi-color light curves measured in future observation projects.
21
Marchant, Pablo, Mathieu Renzo, Robert Farmer, et al. "Pulsational Pair-instability Supernovae in Very Close Binaries." Astrophysical Journal 882, no. 1 (2019): 36. http://dx.doi.org/10.3847/1538-4357/ab3426.
Full text
22
Grant, Andrew. "Iron isotope reveals Earth’s close encounters with supernovae." Physics Today 69, no. 6 (2016): 23. http://dx.doi.org/10.1063/pt.3.3192.
Full text
23
Nomoto, K. "Explosions of Helium Stars and Type IB/IC/IIB Supernovae." Symposium - International Astronomical Union 143 (1991): 515–28. http://dx.doi.org/10.1017/s0074180900045691.
Full textAbstract:
Theoretical models of supernova explosions of helium stars with various masses are reviewed to examine possible connections between Wolf-Rayet stars and Type Ib/Ic/IIb supernovae. Nucleosynthesis, Rayleigh-Taylor instabilities, and light curves are compared with observations. Maximum brightness and the fast decline of the light curves of typical SNe Ib/Ic can be well accounted for by the helium star models if the helium star mass is as low as 3-5 M⊙. These low mass helium stars can form from stars of 12-18 M⊙ after Roche-lobe overflow in close binary systems. Probably progenitors of typical SNe Ib/Ic are not classified as Wolf-Rayet stars.
24
Liljegren, S., A. Jerkstrand, and J. Grumer. "Carbon monoxide formation and cooling in supernovae." Astronomy & Astrophysics 642 (October 2020): A135. http://dx.doi.org/10.1051/0004-6361/202038116.
Full textAbstract:
Context. The inclusion of molecular physics is an important piece that tends to be missing from the puzzle when modeling the spectra of supernovae (SNe). Molecules have both a direct impact on the spectra, particularly in the infrared, and an indirect one as a result of their influence on certain physical conditions, such as temperature. Aims. In this paper, we aim to investigate molecular formation and non-local thermodynamic equilibrium (NLTE) cooling, with a particular focus on CO, the most commonly detected molecule in supernovae. We also aim to determine the dependency of supernova chemistry on physical parameters and the relative sensitivity to rate uncertainties. Methods. We implemented a chemical kinetic description of the destruction and formation of molecules into the SN spectral synthesis code SUMO. In addition, selected molecules were coupled into the full NLTE level population framework and, thus, we incorporated molecular NLTE cooling into the temperature equation. We produced a test model of the CO formation in SN 1987A between 150 and 600 days and investigated the sensitivity of the resulting molecular masses to the input parameters. Results. We find that there is a close inter-dependency between the thermal evolution and the amount of CO formed, mainly through an important temperature-sensitive CO destruction process with O+. After a few hundred days, CO completely dominates the cooling of the oxygen-carbon zone of the supernova which, therefore, contributes little optical emission. The uncertainty of the calculated CO mass scales approximately linearly with the typical uncertainty factor for individual rates. We demonstrate how molecular masses can potentially be used to constrain various physical parameters of the supernova.
25
van den Bergh, Sidney. "Centenary of S Andromedae (SN 1885a)." Highlights of Astronomy 7 (1986): 573–77. http://dx.doi.org/10.1017/s153929960000695x.
Full textAbstract:
AbstractObservations by Hartwig, Wolf, Dunér and Bigourdan are used to show that SN 1885a reached MV(max) = −18.8 ± 0.5 on 17 or 18 August 1885. The lightcurve of S And is found to have declined more rapidly after maximum than that of any other well-observed supernova. The existence of S And and the relatively young age of the supernova remnant Sgr A East appear to indicate that the supernova frequencies near the nucleus of M31 and the Galactic centre are respectively ∽102and ∽103times higher than expected. It is spectulated that S And may belong to a population of supernovae (“type 0”) that only occur near the nuclei of giant galaxies. Beyond the Local Group such objects might perhaps have been missed because of their fast decline and close proximity to luminous nuclei.
26
BARKOV, MAXIM V. "CLOSE BINARY PROGENITORS OF HYPERNOVAE." International Journal of Modern Physics: Conference Series 08 (January 2012): 209–19. http://dx.doi.org/10.1142/s2010194512004618.
Full textAbstract:
In this paper we propose a new plausible mechanism of supernova explosions specific to close binary systems. The starting point is the common envelope phase in the evolution of a binary consisting of a red super giant and a neutron star. As the neutron star spirals towards the center of its companion it spins up via disk accretion. Depending on the specific angular momentum of gas captured by the neutron star via the Bondi-Hoyle mechanism, it may reach millisecond periods either when it is still inside the common envelope or after it has merged with the companion core. The high accretion rate may result in strong differential rotation of the neutron star and generation of a magnetar-strength magnetic field. The magnetar wind can blow away the common envelope if its magnetic field is as strong as 1015 G, and can destroy the entire companion if it is as strong as 1016 G. The total explosion energy can be comparable to the rotational energy of a millisecond pulsar and reach 1052 erg. The result is an unusual type-II supernova with very high luminosity during the plateau phase, followed by a sharp drop in brightness and a steep light-curve tail. The remnant is either a solitary magnetar or a close binary involving a Wolf-Rayet star and a magnetar. When this Wolf-Rayet star explodes this will be a third supernovae explosion in the same binary. A particularly interesting version of the binary progenitor involves merger of a red super giant star with an ultra-compact companion, neutron star or black hole. In the case if a strong magnetic field is not generated on the surface of a neutron star then it will collapse to a black hole. After that we expect the formation of a very long-lived accretion disk around the black hole. The Blandford-Znajek driven jet from this black hole may drive not only hypernovae explosion but produce a bright X-ray transient event on a time scale of 104 s.
27
Geier, Stephan, Thomas Kupfer, Veronika Schaffenroth, and Ulrich Heber. "Hot subdwarf stars in the Galactic halo Tracers of prominent events in late stellar evolution." Proceedings of the International Astronomical Union 11, S317 (2015): 302–3. http://dx.doi.org/10.1017/s174392131500681x.
Full textAbstract:
AbstractHot subdwarf stars (sdO/Bs) are the stripped cores of red giants located at the bluest extension of the horizontal branch. They constitute the dominant population of UV-bright stars in old stellar environments and are most likely formed by binary interactions. We perform the first systematic, spectroscopic analysis of a sample of those stars in the Galactic halo based on data from SDSS. In the course of this project we discovered 177 close binary candidates. A significant fraction of the sdB binaries turned out to have close substellar companions, which shows that brown dwarfs and planets can significantly influence late stellar evolution. Close hot subdwarf binaries with massive white dwarf companions on the other hand are good candidates for the progenitors of type Ia supernovae. We discovered a hypervelocity star, which not only turned out to be the fastest unbound star known in our Galaxy, but also the surviving companion of such a supernova explosion.
28
Tauris, T. M., N. Langer, T. J. Moriya, Ph Podsiadlowski, S. C. Yoon, and S. I. Blinnikov. "ULTRA-STRIPPED TYPE Ic SUPERNOVAE FROM CLOSE BINARY EVOLUTION." Astrophysical Journal 778, no. 2 (2013): L23. http://dx.doi.org/10.1088/2041-8205/778/2/l23.
Full text
29
Di Stefano, R. "Mass from a third star: transformations of close compact-object binaries within hierarchical triples." Monthly Notices of the Royal Astronomical Society 493, no. 2 (2020): 1855–73. http://dx.doi.org/10.1093/mnras/staa220.
Full textAbstract:
ABSTRACT Close-orbit binaries consisting of two compact objects are a centre of attention because of the detection of gravitational-radiation-induced mergers. The creation of close, compact-object binaries involves physical processes that are not yet well understood; there are open questions about the manner in which two compact objects come to be close enough to merge within a Hubble time. Here, we explore an important, and likely common physical process: mass transfer from a third star in a wider, hierarchical orbit. Mass added to the close binary’s components can reduce the time to merger and can even change the nature of an accretor, transforming a white dwarf to a neutron star and/or a neutron star to a black hole. Some accreting WDs in close binaries may even explode as Type Ia supernovae. Given the ubiquity of higher order multiples, the evolutionary channels we lay out may be important pathways to gravitational mergers, including Type Ia supernovae. Fortunately, these pathways also lead to testable predictions.
30
Janka, H. Th, R. Buras, K. Kifonidis, A. Marek, and M. Rampp. "Core-Collapse Supernovae at the Threshold." International Astronomical Union Colloquium 192 (2005): 253–62. http://dx.doi.org/10.1017/s025292110000926x.
Full textAbstract:
SummaryRecent progress in modeling core-collapse supernovae is summarized and set in perspective. Two-dimensional simulations with state-of-the-art treatment of neutrino transport still fail to produce powerful explosions, but evidence is presented that they are very close to a success.
31
Janka, H. Th, and E. M. Müller. "Dynamics of Type-II Supernovae." International Astronomical Union Colloquium 145 (1996): 109–17. http://dx.doi.org/10.1017/s0252921100007971.
Full textAbstract:
Hydrodynamical simulations of type-II supernovae in one and two dimensions are performed for the revival phase of the delayed shock by neutrino energy deposition. Starting with a post-collapse model of the 1.31 Mʘ iron core of a 15 Mʘ star immediately after the stagnation of the prompt shock about 10 ms after core bounce, the models are followed for several hundred milliseconds with varied neutrino fluxes from the neutrino sphere. The variation of the neutrino luminosities is motivated by the considerable increase of the neutrino emission due to convective processes inside and close to the neutrino sphere (see Janka 1993), which are driven by negative gradients of entropy and electron concentration left behind by the prompt shock (Burrows & Fryxell 1992, Janka & Müller 1992). The size of this luminosity increase remains to be quantitatively analyzed yet and may require multi-dimensional neutrino transport. However, in the presented simulations the region below the neutrino sphere is cut out and replaced by an inner boundary condition, so that the convective zone is only partially included and the neutrino flows are treated as a freely changeable energy source.For small neutrino luminosities the energy transfer to the matter is insufficient to revive the stalled shock. However, there is a sharp transition to successful explosions, when the neutrino luminosities lie above some ‘threshold value’. Once the shock is driven out and the density and temperature of the matter between neutrino sphere and shock start to decrease during the expansion, suitable conditions for further neutrino energy deposition are maintained, and an explosion results. With the neutrino energy deposition the entropy per nucleon in the region between neutrino sphere and shock grows, and convective overturn will set in. Multi-dimensional simulations show that due to the large pressure scale height a large-scale pattern of up-flows and down-flows with velocities close to the local speed of sound develops. Consequently, cold, postshock material is advected down into the neutrino heating layer close to the neutrino sphere and hot material is transported outwards, thus reducing energy losses by re-emission of neutrinos and increasing the pressure behind the shock. Therefore these convective processes are found to be a very important aid to the delayed supernova explosion. In fact, two-dimensional models explode even in cases where spherically symmetrical computations fail.
32
Meng, Xiangcun, Xuefei Chen, and Zhanwen Han. "The single degenerate channel for the progenitors of Type Ia supernovae." Proceedings of the International Astronomical Union 4, S252 (2008): 379–82. http://dx.doi.org/10.1017/s1743921308023259.
Full textAbstract:
AbstractWe have carried out a detailed study of the single-degenerate channel for the progenitors of type Ia supernovae (SNe Ia). In the model, a carbon-oxygen white dwarf (CO WD) accretes hydrogen-rich material from an unevolved or a slightly evolved non-degenerate companion to increase its mass to Chandrasekhar mass limit. Incorporating the prescription of Hachisuet al. (1999a) for the accretion efficiency into Eggleton's stellar evolution code and assuming that the prescription is valid for all metallicities, we performed binary stellar evolution calculations for more than 25,000 close WD binary systems with various metallicities. The initial parameter spaces for SNe Ia are presented in an orbital period-secondary mass (logPi,M2i) plane for eachZ.Adopting the results above, we studied the birth rate of SNe Ia for variousZvia binary population synthesis. From the study, we see that for a highZ, SNe Ia occur systemically earlier and the peak value of the birth rate is larger if a single starburst is assumed. The Galactic birth rate from the channel is lower than (but comparable to) that inferred from observations.We also showed the distributions of the parameters of the binary systems at the moment of supernova explosion and the distributions of the properties of companions after supernova explosion. The former provides physics input to simulate the interaction between supernova ejecta and its companion, and the latter is helpful for searching the companions in supernova remnants.
33
Filippenko, Alexei V. "Are Wolf-Rayet Stars the Progenitors of Type IB/IC Supernovae?" Symposium - International Astronomical Union 143 (1991): 529–36. http://dx.doi.org/10.1017/s0074180900045708.
Full textAbstract:
I discuss evidence for and against the hypothesis that Type Ib and Type Ic supernovae (SNe) are produced by core collapse in massive, evolved progenitors. A key object is SN 1987K, whose spectroscopic classification changed from Type II to Type Ib/Ic as it aged. The progenitor of SN 1987K may well have been a massive star which experienced incomplete mass loss, leaving a thin outer envelope of hydrogen. However, several arguments are used to conclude that in most SNe Ib/Ic, the pre-supernova mass loss cannot be caused entirely by strong winds as in Wolf-Rayet stars. Mass transfer in close binary systems is probably important, but in such cases the supernova progenitor is not necessarily a Wolf-Rayet star; instead, it may be a relatively quiescent, hot, low-mass helium star that explodes via core collapse. For example, the rapid decline of the light curve of the Type Ic SN 1987M, and its seemingly low ejected mass, are consistent with this idea. It is also possible that some, but not all, SNe Ib/Ic arise from deflagrations or detonations of white dwarfs.
34
Bond, Howard E., Robin Ciardullo, and Michael G. Meakes. "Close-Binary Nuclei of Planetary Nebulae." Symposium - International Astronomical Union 151 (1992): 517–21. http://dx.doi.org/10.1017/s0074180900122855.
Full textAbstract:
Close-binary planetary-nebula nuclei (PNNs) provide direct evidence for occurrence of a common-envelope phase in binary-star evolution. Their descendants are V471 Tauri-type detached binaries, cataclysmic binaries, and possibly Type I supernovae. Thirteen close-binary PNNs are now known from periodic photometric or radial-velocity variations, or from composite optical/UV spectra. At least 10% of PNNs are close binaries, a fraction more than sufficient to account for the formation of all of the cataclysmic variables in the solar neighborhood. The Abell 35-type binary PNNs, a class with three known members, contain rapidly rotating, chromospherically active late-type primary stars along with extremely hot companions detected with the IUE satellite.
35
Dewi, Jasinta D. M., and Onno R. Pols. "The evolution of close helium star to neutron star binaries." Symposium - International Astronomical Union 212 (2003): 410–11. http://dx.doi.org/10.1017/s0074180900212527.
Full textAbstract:
We present the evolution of helium stars in binary systems with a 1.4 M⊙ neutron-star companion which will produce double neutron-star binaries, i.e., systems with helium stars more massive than 2.5 M⊙. We found that mass transfer from helium star less massive than ~ 3.3 M⊙ will end up in a common-envelope phase. If the neutron star has enough time to complete the spiral-in before the core of the helium star collapses, the system will become a very tight double neutron-star binary (P ≈ 0d.01). More massive helium stars do not go through a dynamically-unstable mass transfer. The outcome of binaries with helium star in this range of mass is double-neutron star systems with period of 0d.1-1d, suggesting them to be the progenitor of the observed Galactic double neutron-star pulsars B 1913+16 and B 15344+12. Wide DNS pulsars like J 1518+4904 are produced from helium star-neutron star binaries which avoid Roche-lobe overflow. We are also able to distinguish the progenitors of Type Ib supernovae (as the high-mass helium stars or systems in wide orbits) from those of Type Ic supernovae (as the lower-mass helium stars or systems in close orbits).
36
Chandra, Vedant, Hsiang-Chih Hwang, Nadia L. Zakamska, et al. "The SN Ia runaway LP 398-9: detection of circumstellar material and surface rotation." Monthly Notices of the Royal Astronomical Society 512, no. 4 (2022): 6122–33. http://dx.doi.org/10.1093/mnras/stac883.
Full textAbstract:
ABSTRACT A promising progenitor scenario for Type Ia supernovae (SNeIa) is the thermonuclear detonation of a white dwarf in a close binary system with another white dwarf. After the primary star explodes, the surviving donor can be spontaneously released as a hypervelocity runaway. One such runaway donor candidate is LP 398-9, whose orbital trajectory traces back ≈105 yr to a known supernova remnant. Here, we report the discovery of carbon-rich circumstellar material around LP 398-9, revealed by a strong infrared excess and analysed with follow-up spectroscopy. The circumstellar material is most plausibly composed of inflated layers from the star itself, mechanically and radioactively heated by the past companion’s supernova. We also detect a 15.4 h periodic signal in the UV and optical light curves of LP 398-9, which we interpret as surface rotation. The rotation rate is consistent with theoretical predictions from this supernova mechanism, and the brightness variations could originate from surface inhomogeneity deposited by the supernova itself. Our observations strengthen the case for this double-degenerate SNIa progenitor channel, and motivate the search for more runaway SNIa donors.
37
Han, Z., and X. Chen. "White dwarf accretion and type Ia supernovae." Proceedings of the International Astronomical Union 8, S290 (2012): 117–20. http://dx.doi.org/10.1017/s1743921312019333.
Full textAbstract:
AbstractType Ia supernovae (SNe Ia) are believed to be thermonuclear explosions of carbon-oxygen white dwarfs at a mass close to the Chandrasekhar limit. However, a white dwarf at birth has a significantly lower mass and needs to accrete mass to grow to the limit for the explosion. Various progenitor models have been proposed and those models play an important role in our understanding of SNe Ia and cosmology.
38
Fuller, Jim, and Wenbin Lu. "The spins of compact objects born from helium stars in binary systems." Monthly Notices of the Royal Astronomical Society 511, no. 3 (2022): 3951–64. http://dx.doi.org/10.1093/mnras/stac317.
Full textAbstract:
ABSTRACT The angular momentum (AM) content of massive stellar cores helps us to determine the natal spin rates of neutron stars and black holes. Asteroseismic measurements of low-mass stars have proven that stellar cores rotate slower than predicted by most prior work, so revised models are necessary. In this work, we apply an updated AM transport model based on the Tayler instability to massive helium stars in close binaries, in which tidal spin-up can greatly increase the star’s AM. Consistent with prior work, these stars can produce highly spinning black holes upon core-collapse if the orbital period is less than $P_{\rm orb} \lesssim \! 1 \, {\rm d}$. For neutron stars, we predict a strong correlation between the pre-explosion mass and the neutron star rotation rate, with millisecond periods ($P_{\rm NS} \lesssim 5 \, {\rm ms}$) only achievable for massive ($M \gtrsim 10 \, M_\odot$) helium stars in tight ($P_{\rm orb} \lesssim 1 \, {\rm d}$) binaries. Finally, we discuss our models in relation to type Ib/c supernovae, superluminous supernove, gamma-ray bursts, and LIGO/Virgo measurements of black hole spins. Our models are roughly consistent with the rates and energetics of these phenomena, with the exception of broad-lined Ic supernovae, whose high rates and ejecta energies are difficult to explain.
39
Das, Kaustav K., Christoffer Fremling, Mansi M. Kasliwal, et al. "SN 2023zaw: An Ultrastripped, Nickel-poor Supernova from a Low-mass Progenitor." Astrophysical Journal Letters 969, no. 1 (2024): L11. http://dx.doi.org/10.3847/2041-8213/ad527a.
Full textAbstract:
Abstract We present SN 2023zaw—a subluminous (M r = −16.7 mag) and rapidly evolving supernova (t 1/2,r = 4.9 days), with the lowest nickel mass (≈0.002 M ⊙) measured among all stripped-envelope supernovae discovered to date. The photospheric spectra are dominated by broad He i and Ca near-infrared emission lines with velocities of ∼10,000−12,000 km s−1. The late-time spectra show prominent narrow He i emission lines at ∼1000 km s−1, indicative of interaction with He-rich circumstellar material. SN 2023zaw is located in the spiral arm of a star-forming galaxy. We perform radiation-hydrodynamical and analytical modeling of the lightcurve by fitting with a combination of shock-cooling emission and nickel decay. The progenitor has a best-fit envelope mass of ≈0.2 M ☉ and an envelope radius of ≈50 R ⊙. The extremely low nickel mass and low ejecta mass (≈0.5 M ⊙) suggest an ultrastripped SN, which originates from a mass-losing low-mass He-star (zero-age main-sequence mass < 10 M ⊙) in a close binary system. This is a channel to form double neutron star systems, whose merger is detectable with LIGO. SN 2023zaw underscores the existence of a previously undiscovered population of extremely low nickel mass (<0.005 M ☉) stripped-envelope supernovae, which can be explored with deep and high-cadence transient surveys.
40
Priestley, F. D., H. Chawner, M. Matsuura, I. De Looze, M. J. Barlow, and H. L. Gomez. "Revisiting the dust destruction efficiency of supernovae." Monthly Notices of the Royal Astronomical Society 500, no. 2 (2020): 2543–53. http://dx.doi.org/10.1093/mnras/staa3445.
Full textAbstract:
ABSTRACT Dust destruction by supernovae is one of the main processes removing dust from the interstellar medium (ISM). Estimates of the efficiency of this process, both theoretical and observational, typically assume a shock propagating into a homogeneous medium, whereas the ISM possesses significant substructure in reality. We self-consistently model the dust and gas properties of the shocked ISM in three supernova remnants (SNRs), using X-ray and infrared (IR) data combined with corresponding emission models. Collisional heating by gas with properties derived from X-ray observations produces dust temperatures too high to fit the far-IR fluxes from each SNR. An additional colder dust component is required, which has a minimum mass several orders of magnitude larger than that of the warm dust heated by the X-ray emitting gas. Dust-to-gas mass ratios indicate that the majority of the dust in the X-ray emitting material has been destroyed, while the fraction of surviving dust in the cold component is plausibly close to unity. As the cold component makes up virtually all the total dust mass, destruction time-scales based on homogeneous models, which cannot account for multiple phases of shocked gas and dust, may be significantly overestimating actual dust destruction efficiencies, and subsequently underestimating grain lifetimes.
41
Tsuna, Daichi, Yuki Takei, and Toshikazu Shigeyama. "Precursors of Supernovae from Mass Eruption: Prospects for Early Warning of Nearby Core-collapse Supernovae." Astrophysical Journal 945, no. 2 (2023): 104. http://dx.doi.org/10.3847/1538-4357/acbbc6.
Full textAbstract:
Abstract Recent observations of a large fraction of Type II supernovae (SNe) show traces of dense circumstellar medium (CSM) very close to the progenitor star. If this CSM is created by eruptive mass loss several months before core collapse, the eruption itself may be visible as a precursor, helpful as an early warning of a near-future SN. Using radiation hydrodynamical simulations based on the open-source code CHIPS, we theoretically model the emission from the mass eruption of a red supergiant star. We find that for a modest mass eruption the luminosity is typically on the order of 1039 erg s−1, can last as long as hundreds of days until the star explodes, and is mainly bright in the infrared (from −9 to −11 mag around peak). We discuss observational strategies to find these signatures from Galactic and local Type II SNe.
42
Ludwig, Peter, Shawn Bishop, Ramon Egli, et al. "Time-resolved 2-million-year-old supernova activity discovered in Earth’s microfossil record." Proceedings of the National Academy of Sciences 113, no. 33 (2016): 9232–37. http://dx.doi.org/10.1073/pnas.1601040113.
Full textAbstract:
Massive stars (M≳10 M⊙), which terminate their evolution as core-collapse supernovae, are theoretically predicted to eject >10−5M⊙ of the radioisotope 60Fe (half-life 2.61 Ma). If such an event occurs sufficiently close to our solar system, traces of the supernova debris could be deposited on Earth. Herein, we report a time-resolved 60Fe signal residing, at least partially, in a biogenic reservoir. Using accelerator mass spectrometry, this signal was found through the direct detection of live 60Fe atoms contained within secondary iron oxides, among which are magnetofossils, the fossilized chains of magnetite crystals produced by magnetotactic bacteria. The magnetofossils were chemically extracted from two Pacific Ocean sediment drill cores. Our results show that the 60Fe signal onset occurs around 2.6 Ma to 2.8 Ma, near the lower Pleistocene boundary, terminates around 1.7 Ma, and peaks at about 2.2 Ma.
43
Davenport, James R. A., Sofia Z. Sheikh, Wael Farah, et al. "Real-time Technosignature Strategies with SN 2023ixf." Research Notes of the AAS 7, no. 6 (2023): 120. http://dx.doi.org/10.3847/2515-5172/acdc24.
Full textAbstract:
Abstract Several technosignature techniques focus on historic events such as SN 1987A as the basis to search for coordinated signal broadcasts from extraterrestrial agents. The recently discovered SN 2023ixf in the spiral galaxy M101 is the nearest Type II supernova in over a decade, and will serve as an important benchmark event. Here we review the potential for SN 2023ixf to advance ongoing techonsignature searches, particularly signal-synchronization techniques such as the “SETI Ellipsoid” that identifies over time stars that could transmit signals after observing a supernovae event. We find that more than 100 stars within 100 pc are already close to intersecting this SETI Ellipsoid, providing numerous targets for real-time monitoring within ∼3° of SN 2023ixf. We are commencing a radio technosignature monitoring campaign of these targets with the Allen Telescope Array and the Green Bank Telescope.
44
Langer, N. "Open questions in massive star research." Proceedings of the International Astronomical Union 18, S361 (2022): 1–11. http://dx.doi.org/10.1017/s1743921322003088.
Full textAbstract:
AbstractIn discussing open question in the field of massive stars, I consider their evolution from birth to death. After touching upon massive star formation, which may be bi-modal and not lead to a zero-age main sequence at the highest masses, I consider the consequences of massive stars being close to their Eddington limit. Then, when discussing the effects of a binary companion, I highlight the importance of massive Algols and contact binaries for understanding the consequences of mass transfer, and the role of binaries in forming Wolf-Rayet stars. Finally, a discussion on pair instability supernovae and of superluminous supernovae is provided.
45
Kochanek, C. S., K. Auchettl, and K. Belczynski. "Stellar binaries that survive supernovae." Monthly Notices of the Royal Astronomical Society 485, no. 4 (2019): 5394–410. http://dx.doi.org/10.1093/mnras/stz717.
Full textAbstract:
Abstract The number of binaries containing black holes (BH) or neutron stars (NS) depends critically on the fraction of binaries that survive supernova (SN) explosions. We searched for surviving star plus remnant binaries in a sample of 49 supernova remnants (SNR) containing 23 previously identified compact remnants and three high-mass X-ray binaries (HMXB), finding no new interacting or non-interacting binaries. The upper limits on any main-sequence stellar companion are typically $\lesssim 0.2\, \mathrm{M}_\odot$ and are at worst $\lesssim 3\, \mathrm{M}_\odot$. This implies that f &lt; 0.1 of core-collapse SNRs contain a non-interacting binary, and f = 0.083 (0.032 &lt; f &lt; 0.17) contain an interacting binary at 90 per cent confidence. We also find that the transverse velocities of HMXBs are low, with a median of only 12 km s−1 for field HMXBs, so surviving binaries will generally be found very close to the explosion centre. We compare the results to a ‘standard’ StarTrack binary population synthesis (BPS) model, finding reasonable agreement with the observations. In particular, the BPS models predict that 6 per cent of initial binaries leave a star plus remnant binary, or 5 per cent of SNRs assuming an 84 per cent binary fraction.
46
Ramos, Angelu, Jessica Schonhut-Stasik, Anna Payne, and Keivan Stassun. "Identifying Habitable-zone Planet Systems Susceptible to Nearby Supernovae." Research Notes of the AAS 7, no. 2 (2023): 21. http://dx.doi.org/10.3847/2515-5172/acbaf9.
Full textAbstract:
Abstract We investigate whether any known candidate habitable-zone exoplanet systems could be imperiled by being sufficiently close to a future supernova. Using existing exoplanet databases, we identify 24 stars possessing at least one planet in the star’s habitable zone. We search the Gaia EDR3 catalog for possible core-collapse supernova progenitors within 150 lt-yr of each of these systems, using Pan-STARRS and Gaia EDR3/DR2 colors to identify neighboring stars that are likely to have masses ≥8M ⊙ (i.e., potential supernova Type II progenitors). Within, our sample, we find one instance of a habitable-zone planetary system within 150 lt-yr of a possible Type II supernova progenitor.
47
Sawada, Ryo, Kazumi Kashiyama, and Yudai Suwa. "On the Energy Source of Ultrastripped Supernovae." Astrophysical Journal 927, no. 2 (2022): 223. http://dx.doi.org/10.3847/1538-4357/ac53ae.
Full textAbstract:
Abstract Ultrastripped supernovae (USSNe) with a relatively low ejecta mass of ∼0.1 M ⊙ (e.g., iPTF 14gqr and SN 2019dge) are considered to originate from ultrastripped carbon–oxygen cores in close binary systems and are likely to be progenitors of binary neutron stars. Here we conduct the explosion simulations of ultrastripped progenitors with various masses (1.45 M ⊙ ≤ M CO ≤ 2.0 M ⊙) based on results of neutrino-radiation hydrodynamics simulations, and consistently calculate the nucleosynthesis and the supernova light curves. We find that a USSN from a more massive progenitor has a larger ejecta mass but a smaller 56Ni mass mainly due to the fallback that leads to the light curve being dimmer and slower. By comparing the synthetic light curves with the observed ones, we show that SN 2019dge can be solely powered by 56Ni synthesized during the explosion of a progenitor with M CO ≲ 1.6 M ⊙ while iPTF 14gqr cannot be explained by the 56Ni-powered model; ∼0.05 M ⊙ of 56Ni inferred from the light-curve fitting is argued to be difficult to synthesize for ultrastripped progenitors. We consider fallback accretion onto and rotation-powered relativistic wind from the newborn neutron star (NS) as alternative energy sources and show that iPTF 14gqr could be powered by a newborn NS with a magnetic field of B p ∼ 1015 G and an initial rotation period of P i ∼ 0.1 s.
48
Fryer, Christopher L., Eric Burns, Anna Y. Q. Ho, et al. "Explaining Nonmerger Gamma-Ray Bursts and Broad-lined Supernovae with Close Binary Progenitors with Black Hole Central Engines." Astrophysical Journal 986, no. 2 (2025): 185. https://doi.org/10.3847/1538-4357/add474.
Full textAbstract:
Abstract For over 25 yr, the origin of long-duration gamma-ray bursts (lGRBs) has been linked to the collapse of rotating massive stars. However, we have yet to pinpoint the stellar progenitor powering these transients. Moreover, the dominant engine powering the explosions remains open to debate. Observations of both lGRBs, supernovae associated with these GRBs, such as broad-line (BL) stripped-envelope (type Ic) supernovae (hereafter, Ic-BL), supernovae (SNe), and perhaps superluminous SNe, fast blue optical transients, and fast x-ray transients, may provide clues to both engines and progenitors. In this paper, we conduct a detailed study of the tight-binary formation scenario for lGRBs, comparing this scenario to other leading progenitor models. Combining this progenitor scenario with different lGRB engines, we can compare to existing data and make predictions for future observational tests. We find that the combination of the tight-binary progenitor scenario with the black hole accretion disk engine can explain lGRBs, low-luminosity GRBs, ultra-long GRBs, and Ic-BL. We discuss the various progenitor properties required for these different subclasses and note such systems would be future gravitational-wave merger sources. We show that the current literature on other progenitor-engine scenarios cannot explain all of these transient classes with a single origin, motivating additional work. We find that the tight-binary progenitor with a magnetar engine is excluded by existing observations. The observations can be used to constrain the properties of stellar evolution, the nature of the GRB, and the associated SN engines in lGRBs and Ic-BL. We discuss the future observations needed to constrain our understanding of these rare, but powerful, explosions.
49
Mera Evans, T. B., P. Hoeflich, and R. Diehl. "Galactic Positrons from Thermonuclear Supernovae." Astrophysical Journal 930, no. 2 (2022): 107. http://dx.doi.org/10.3847/1538-4357/ac5253.
Full textAbstract:
Abstract Type Ia supernovae (SNe Ia) may originate from a wide variety of explosion scenarios and progenitor channels. They exhibit a factor of ≈10 difference in brightness and thus a differentiation in the mass of 56Ni → 56Co → 56Fe. We present a study on the fate of positrons within SNe Ia in order to evaluate their escape fractions and energy spectra. Our detailed Monte Carlo transport simulations for positrons and γ-rays include both β + decay of 56Co and pair production. We simulate a wide variety of explosion scenarios, including the explosion of white dwarfs (WDs) close to the Chandrasekhar mass (M Ch), He-triggered explosions of sub-M Ch WDs, and dynamical mergers of two WDs. For each model, we study the influence of the size and morphology of the progenitor magnetic field between 1 and 1013 G. Population synthesis based on the observed brightness distribution of SNe Ia was used to estimate the overall contributions to Galactic positrons due to escape from SNe Ia. We find that this is dominated by SNe Ia of normal brightness, where variations in the distribution of emitted positrons are small. We estimate a total SNe Ia contribution to Galactic positrons of <2% and, depending on the magnetic field morphology, <6–20% for M Ch and sub-M Ch, respectively.
50
Iben, Jr., Icko, and Alexander V. Tutukov. "On the Evolution of Close Triple Stars That Produce Type Ia Supernovae." Astrophysical Journal 511, no. 1 (1999): 324–34. http://dx.doi.org/10.1086/306672.
Full text