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Supernova 1987A's Keyhole:A Long-lived Jet-pair in the Final Explosion Phase of Core-collapse Supernovae
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作者 Noam Soker 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2024年第7期89-94,共6页
I further study the manner by which a pair of opposite jets shape the“keyhole”morphological structure of the core-collapse supernova(CCSN)SN 1997A,now the CCSN remnant(CCSNR)1987A.By doing so,I strengthen the claim ... I further study the manner by which a pair of opposite jets shape the“keyhole”morphological structure of the core-collapse supernova(CCSN)SN 1997A,now the CCSN remnant(CCSNR)1987A.By doing so,I strengthen the claim that the jittering-jet explosion mechanism accounts for most,likely all,CCSNe.The“keyhole”structure comprises a northern low-intensity zone closed with a bright rim on its front and an elongated low-intensity nozzle in the south.This rim-nozzle asymmetry is observed in some cooling flow clusters and planetary nebulae that are observed to be shaped by jets.I build a toy model that uses the planar jittering jets pattern,where consecutive pairs of jets tend to jitter in a common plane,implying that the accreted gas onto the newly born neutron star at the late explosion phase flows perpendicular to that plane.This allows for a long-lived jet-launching episode.This long-lasting jet-launching episode launches more mass into the jets that can inflate larger pairs of ears or bubbles,forming the main jets'axis of the CCSNR that is not necessarily related to a possible pre-collapse core rotation.I discuss the relation of the main jets'axis to the neutron star's natal kick velocity. 展开更多
关键词 STARS massive-(stars)supernovae general-(stars)supernovae individual(SN 1987A)-ISM supernova remnants-stars jets
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Energy Conservation in the Thin Layer Approximation: I. The Spherical Classic Case for Supernovae Remnants 被引量:2
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作者 Lorenzo Zaninetti 《International Journal of Astronomy and Astrophysics》 2020年第2期71-88,共18页
The thin layer approximation applied to the expansion of a supernova remnant assumes that all the swept mass resides in a thin shell. The law of motion in the thin layer approximation is therefore found using the cons... The thin layer approximation applied to the expansion of a supernova remnant assumes that all the swept mass resides in a thin shell. The law of motion in the thin layer approximation is therefore found using the conservation of momentum. Here we instead introduce the conservation of energy in the framework of the thin layer approximation. The first case to be analysed is that of an interstellar medium with constant density and the second case is that of 7 profiles of decreasing density with respect to the centre of the explosion. The analytical and numerical results are applied to 4 supernova remnants: Tycho, Cas A, Cygnus loop, and SN 1006. The back reaction due to the radiative losses for the law of motion is evaluated in the case of constant density of the interstellar medium. 展开更多
关键词 supernovae: General supernovae: Individual (SN Tycho) supernovae: Individual (SN Cas A) supernovae: Individual (SN Cygnus Loop) supernovae: Individual (SN 1006)
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Prospects of the Multi-channel Photometric Survey Telescope in the Cosmological Application of Type Ia Supernovae
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作者 Zhenyu Wang Jujia Zhang +1 位作者 Xinzhong Er Jinming Bai 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2024年第4期183-191,共9页
The Multi-channel Photometric Survey Telescope(Mephisto)is a real-time,three-color photometric system designed to capture the color evolution of stars and transients accurately.This telescope system can be crucial in ... The Multi-channel Photometric Survey Telescope(Mephisto)is a real-time,three-color photometric system designed to capture the color evolution of stars and transients accurately.This telescope system can be crucial in cosmological distance measurements of low-redshift(low-z,z■0.1)Type Ia supernovae(SNe Ia).To optimize the capabilities of this instrument,we perform a comprehensive simulation study before its official operation is scheduled to start.By considering the impact of atmospheric extinction,weather conditions,and the lunar phase at the observing site involving the instrumental features,we simulate light curves of SNe Ia obtained by Mephisto.The best strategy in the case of SN Ia cosmology is to take the image at an exposure time of 130 s with a cadence of 3 days.In this condition,Mephisto can obtain hundreds of high-quality SNe Ia to achieve a distance measurement better than 4.5%.Given the on-time spectral classification and monitoring of the Lijiang 2.4 m Telescope at the same observatory,Mephisto,in the whole operation,can significantly enrich the well-calibrated sample of supernovae at low-z and improve the calibration accuracy of high-z SNe Ia. 展开更多
关键词 (stars:)supernovae:general (cosmology:)cosmological parameters telescopes
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Energy Conservation in the Thin Layer Approximation: II. The Asymmetric Classic Case for Supernovae Remnant
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作者 Lorenzo Zaninetti 《International Journal of Astronomy and Astrophysics》 2020年第2期165-189,共25页
Here we extend the conservation of energy in the framework of the thin layer approximation to the asymmetrical case. Four types of interstellar mediums are analysed, in which the density follows an inverse square prof... Here we extend the conservation of energy in the framework of the thin layer approximation to the asymmetrical case. Four types of interstellar mediums are analysed, in which the density follows an inverse square profile, a power law profile, an exponential profile and a toroidal profile. An analytical solution for the radius as a function of time and the polar angle in spherical coordinates is derived in the case of the inverse square profile. The analytical and numerical results are applied to two supernova remnants: SN 1987A and SN 1006. The back reaction due to the radiative losses is evaluated in the case of the inverse square profile for the surrounding medium. Two models for the image formation are presented, which explain the triple ring visible in SN 1987A and the jet feature of SN 1006. 展开更多
关键词 supernovae General ISM Supernova Remnants supernovae Individual (SN 1987A) supernovae Individual (SN 1006)
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The Tension Cosmology, Largest Cosmic Structures and Explosions of Supernovae from SST
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作者 Sylwester Kornowski 《Journal of High Energy Physics, Gravitation and Cosmology》 CAS 2024年第3期1029-1044,共16页
Here, using the Scale-Symmetric Theory (SST) we explain the cosmological tension and the origin of the largest cosmic structures. We show that a change in value of strong coupling constant for cold baryonic matter lea... Here, using the Scale-Symmetric Theory (SST) we explain the cosmological tension and the origin of the largest cosmic structures. We show that a change in value of strong coupling constant for cold baryonic matter leads to the disagreement in the galaxy clustering amplitude, quantified by the parameter S8. Within the same model we described the Hubble tension. We described also the mechanism that transforms the gravitational collapse into an explosion—it concerns the dynamics of virtual fields that lead to dark energy. Our calculations concern the Type Ia supernovae and the core-collapse supernovae. We calculated the quantized masses of the progenitors of supernovae, emitted total energy during explosion, and we calculated how much of the released energy was transferred to neutrinos. Value of the speed of sound in the strongly interacting matter measured at the LHC confirms that presented here model is correct. Our calculations show that the Universe is cyclic. 展开更多
关键词 Scale-Symmetric Theory Tension Cosmology Coupling Constants Parameters σ8 and S8 Largest Cosmic Structures Dark Energy Supernova Explosion Cyclic Universe
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Energy Conservation in the Thin Layer Approximation: IV. The Light Curve for Supernovae 被引量:1
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作者 Lorenzo Zaninetti 《International Journal of Astronomy and Astrophysics》 2021年第1期37-58,共22页
The light curves (LC) for Supernova (SN) can be modeled adopting the conversion of the flux of kinetic energy into radiation. This conversion requires an analytical or a numerical law of motion for the expanding radiu... The light curves (LC) for Supernova (SN) can be modeled adopting the conversion of the flux of kinetic energy into radiation. This conversion requires an analytical or a numerical law of motion for the expanding radius of the SN. In the framework of conservation of energy for the thin layer approximation, we present a classical trajectory based on a power law profile for the density, a relativistic trajectory based on the Navarro-Frenk-White profile for the density, and a relativistic trajectory based on a power law behaviour for the swept mass. A detailed simulation of the LC requires the evaluation of the optical depth as a function of time. We modeled the LC of SN 1993J in different astronomical bands, the LC of GRB 050814 and the LC GRB 060729 in the keV region. The time dependence of the magnetic field of equipartition is derived from the theoretical formula for the luminosity. 展开更多
关键词 supernovae: General supernovae: (Individual: SN1993j) Gamma-Ray Burst: (Individual: GRB 050814) Gamma-Ray Burst: (Individual: GRB 060729)
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Energy Conservation in the Thin Layer Approximation: III. The Spherical Relativistic Case for Supernovae 被引量:1
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作者 Lorenzo Zaninetti 《International Journal of Astronomy and Astrophysics》 2020年第4期285-301,共17页
The theory of the conservation of energy in the thin layer approximation has been extended to special relativity. Four models for the density of the circumstellar medium are analyzed, which are represented by constant... The theory of the conservation of energy in the thin layer approximation has been extended to special relativity. Four models for the density of the circumstellar medium are analyzed, which are represented by constant, power law, exponential and Emden (<em>n</em> = 5) profile for density. The astrophysical results are presented in a numerical way, except for a Taylor expansion of the four trajectories in the surrounding of the origin. The free parameters of the models are particularized for SN1993j, for which the radius versus time is known. Some evaluations on the time dilation are presented. 展开更多
关键词 supernovae: General supernovae: Individual (SN1993j) ISM: Supernova Remnants
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A Brief Review of Historical Supernovae
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作者 Shawqi Al Dallal Walid J. Azzam 《International Journal of Astronomy and Astrophysics》 2021年第1期73-86,共14页
Supernovae are powerful explosions of massive stars that have reached a terminal stage in their evolution. A huge amount of energy is released during the explosion in a wide range of wavelengths. The supernova explosi... Supernovae are powerful explosions of massive stars that have reached a terminal stage in their evolution. A huge amount of energy is released during the explosion in a wide range of wavelengths. The supernova explosion causes a sudden rise in the dead star’s luminosity which may outshine momentarily the entire galaxy in which it resides. The explosion is produced by a catastrophic collapse of the iron core of a massive star or the collapse of a white dwarf after accreting enough mass from its companion to reach the Chandrasekhar limit. The first record of a supernova occurrence goes back to 185 CE. Subsequently, humans have witnessed across the centuries a series of such violent events that appear suddenly in the sky and illuminate the darkness of the night for several weeks or months. In the first part of this paper, we briefly describe the processes that lead to a supernova explosion. In the second part, we discuss historical supernovae as appearing in the records of human civilizations. In the third part, we highlight ancient records relating the sudden appearance of a supernova or a comet to the spread of epidemics in certain regions of the world. 展开更多
关键词 supernovae Formation Historical supernovae Epidemic Correlations
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Do Near-Solar-System Supernovae Enhance Volcanic Activities on Earth and Neighbouring Planets on Their Paths through the Spiral Arms of the Milky Way, and What Might Be the Consequences for Estimations of Earth’s History and Predictions for Its Future? 被引量:3
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作者 Heinz-Juergen Brink 《International Journal of Geosciences》 2019年第5期563-575,共13页
Recent observations of young volcanism on the near-Earth terrestrial planets require a new understanding. Magmatic/volcanic episodes on Venus, Mars and Mercury, as well as on Earth’s Moon, are apparently contemporane... Recent observations of young volcanism on the near-Earth terrestrial planets require a new understanding. Magmatic/volcanic episodes on Venus, Mars and Mercury, as well as on Earth’s Moon, are apparently contemporaneous thermal events that accompanied increased magmatic/volcanic activity on Earth, following a 300-Myr cycle. A collateral galactic thermal source in the Milky Way appears to be needed that would predominantly affect the interior of the planets and, perhaps indirectly, Earth’s biosphere, compared to other galactic sources, such as intense cosmic rays or large, rocky bolides. The search for such a source leads to near-Earth supernovae, with their neutrino output, and to the question of whether those neutrinos could act as energy transmitters to heat up the body of Earth, and also enhance its short-term magmatic processes;for example, Cenozoic anorogenic volcanism. This observation challenges present assumptions and paradigms about Earth’s history, and requires the following reconsiderations: 1) the real origin of the end-Cretaceous mass extinction;2) the general radioactive age determinations of rocks;and 3) geodynamic modelling using additional, external heat sources. 展开更多
关键词 Synchronous Planetary MAGMATISM Galactic Heat Source supernovae and White DWARFS NEUTRINOS Mass EXTINCTIONS
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A Check on the Cardassian Expansion Model with Type-la Supernovae Data 被引量:1
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作者 Li CaoNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 《Chinese Journal of Astronomy and Astrophysics》 CSCD 北大核心 2003年第4期341-346,共6页
We use the magnitude-redshift relation for the type Ia supernova datacompiled by Riess et al. to analyze the Cardassian expansion scenario. This scenario assumes theuniverse to be flat, matter dominated, and accelerat... We use the magnitude-redshift relation for the type Ia supernova datacompiled by Riess et al. to analyze the Cardassian expansion scenario. This scenario assumes theuniverse to be flat, matter dominated, and accelerating, but contains no vacuum contribution. Thebest fitting model parameters are H_0 = 65.3 km s^(-1) Mpc^(-1), n = 0.35 and Ω_m = 0.05. When thehighest redshift supernova, SN 1997ck, is excluded, H_0 remains the same, but n becomes 0.20 andΩ_m, 0.15, and the matter density remains unreasonably low. Our result shows that this particularscenario is strongly disfavoured by the SNeIa data. 展开更多
关键词 supernovae: general cosmology: theory distances and redshifts
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Distribution of ^(56)Ni Yields of Type Ia Supernovae and its Implication for Progenitors 被引量:1
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作者 Bo Wang Xiang-Cun Meng +1 位作者 Xiao-Feng Wang Zhan-Wen Han 《Chinese Journal of Astronomy and Astrophysics》 CSCD 2008年第1期71-80,共10页
The amount of 56↑Ni produced in Type Ia supernova (SN Ia) explosion is probably the most important physical parameter underlying the observed correlation of SN Ia luminosities with their light curves. Based on an e... The amount of 56↑Ni produced in Type Ia supernova (SN Ia) explosion is probably the most important physical parameter underlying the observed correlation of SN Ia luminosities with their light curves. Based on an empirical relation between the 56↑Ni mass and the light curve parameter △m15, we obtained rough estimates of the 56↑Ni mass for a large sample of nearby SNe Ia with the aim of exploring the diversity in SN Ia. We found that the derived 56↑Ni masses for different SNe Ia could vary by a factor of ten (e.g., MNi = 0.1 - 1.3 M⊙), which cannot be explained in terms of the standard Chandrasekhar-mass model (with a 56↑Ni mass production of 0.4 - 0.8 M⊙). Different explosion and/or progenitor models are clearly required for various SNe Ia, in particular, for those extremely nickel-poor and nickel-rich producers. The nickel-rich (with MNi 〉 0.8 M⊙) SNe Ia are very luminous and may have massive progenitors exceeding the Chandrasekhar-mass limit since extra progenitor fuel is required to produce more 56↑Ni to power the light curve. This is also consistent with the finding that the intrinsically bright SNe Ia prefer to occur in stellar environments of young and massive stars. For example, 75% SNe Ia in spirals have △ml5 〈 1.2 while this ratio is only 18% in E/S0 galaxies. The nickel-poor SNe Ia (with MNi 〈 0.2 M⊙) may invoke the sub- Chandrasekhar model, as most of them were found in early-type E/S0 galaxies dominated by the older and low-mass stellar populations. This indicates that SNe Ia in spiral and E/S0 galaxies have progenitors of different properties. 展开更多
关键词 STARS evolution - supernovae general - white dwarfs
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Modelling and Analysis of the Hubble Diagram of 280 Type SNIa Supernovae and Gamma Ray Bursts Redshifts with Analytical and Empirical Redshift/Magnitude Functions 被引量:2
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作者 Laszlo A. Marosi 《International Journal of Astronomy and Astrophysics》 2016年第3期272-275,共5页
Based on an analysis of 280 Type SNIa supernovae and gamma-ray bursts redshifts in the range of z = 0.0104 - 8.1 the Hubble diagram is shown to follow a strictly exponential slope predicting an exponentially expanding... Based on an analysis of 280 Type SNIa supernovae and gamma-ray bursts redshifts in the range of z = 0.0104 - 8.1 the Hubble diagram is shown to follow a strictly exponential slope predicting an exponentially expanding or static universe. At redshifts > 2 - 3 ΛCDM models show a poor agreement with the observed data. Based on the results presented in this paper, the Hubble diagram test does not necessarily support the idea of expansion according to the big-bang concordance model. 展开更多
关键词 MAGNITUDE Redshift Data Fitting supernovae Gamma Ray Bursts Hubble Diagram ΛCDM Cosmological Model
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Predicting Gravitational Waves from Jittering-jets-driven Core Collapse Supernovae
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作者 Noam Soker 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2023年第12期1-6,共6页
I estimate the frequencies of gravitational waves from jittering jets that explode core collapse supernovae(CCSNe)to crudely be 5–30 Hz,and with strains that might allow detection of Galactic CCSNe.The jittering jets... I estimate the frequencies of gravitational waves from jittering jets that explode core collapse supernovae(CCSNe)to crudely be 5–30 Hz,and with strains that might allow detection of Galactic CCSNe.The jittering jets explosion mechanism(JJEM)asserts that most CCSNe are exploded by jittering jets that the newly born neutron star(NS)launches within a few seconds.According to the JJEM,instabilities in the accreted gas lead to the formation of intermittent accretion disks that launch the jittering jets.Earlier studies that did not include jets calculated the gravitational frequencies that instabilities around the NS emit to have a peak in the crude frequency range of 100–2000Hz.Based on a recent study,I take the source of the gravitational waves of jittering jets to be the turbulent bubbles(cocoons)that the jets inflate as they interact with the outer layers of the core of the star at thousands of kilometers from the NS.The lower frequencies and larger strains than those of gravitational waves from instabilities in CCSNe allow future,and maybe present,detectors to identify the gravitational wave signals of jittering jets.Detection of gravitational waves from local CCSNe might distinguish between the neutrino-driven explosion mechanism and the JJEM. 展开更多
关键词 gravitational waves-stars NEUTRON-STARS black holes-(stars )supernovae general-stars jets
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The cooling time of white dwarfs produced from type Iasupernovae
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作者 Xiang-Cun Meng Wu-Ming Yang Zhong-Mu Li 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2010年第9期927-934,共8页
Type Ia supernovae (SNe Ia) play a key role in measuring cosmological parameters, in which the Phillips relation is adopted. However, the origin of the relation is still unclear. Several parameters are suggested, e.... Type Ia supernovae (SNe Ia) play a key role in measuring cosmological parameters, in which the Phillips relation is adopted. However, the origin of the relation is still unclear. Several parameters are suggested, e.g. the relative content of carbon to oxygen (C/O) and the central density of the white dwarf (WD) at ignition. These parameters are mainly determined by the WD's initial mass and its cooling time, respectively. Using the progenitor model developed by Meng & Yang, we present the distributions of the initial WD mass and the cooling time. We do not find any correlation between these parameters. However, we notice that as the range of the WD's mass decreases, its average value increases with the cooling time. These results could provide a constraint when simulating the SN Ia explosion, i.e. the WDs with a high C/O ratio usually have a lower central density at ignition, while those having the highest central density at ignition generally have a lower C/O ratio. The cooling time is mainly determined by the evolutionary age of secondaries, and the scatter of the cooling time decreases with the evolutionary age. Our results may indicate that WDs with a long cooling time have more uniform properties than those with a short cooling time, which may be helpful to explain why SNe Ia in elliptical galaxies have a more uniform maximum luminosity than those in spiral galaxies. 展开更多
关键词 STARS white dwarfs -- stars supernovae GENERAL
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The Role of Jets in Exploding Supernovae and in Shaping their Remnants
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作者 Noam Soker 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2022年第12期28-52,共25页
I review studies of core collapse supernovae(CCSNe) and similar transient events that attribute major roles to jets in powering most CCSNe and in shaping their ejecta. I start with reviewing the jittering jets explosi... I review studies of core collapse supernovae(CCSNe) and similar transient events that attribute major roles to jets in powering most CCSNe and in shaping their ejecta. I start with reviewing the jittering jets explosion mechanism that I take to power most CCSN explosions. Neutrino heating does play a role in boosting the jets. I compare the morphologies of some CCSN remnants to planetary nebulae to conclude that jets and instabilities are behind the shaping of their ejecta. I then discuss CCSNe that are descendants of rapidly rotating collapsing cores that result in fixed-axis jets(with small jittering) that shape bipolar ejecta. A large fraction of the bipolar CCSNe are superluminous supernovae(SLSNe). I conclude that modeling of SLSN light curves and bumps in the light curves must include jets, even when considering energetic magnetars and/or ejecta interaction with the circumstellar matter(CSM). I connect the properties of bipolar CCSNe to common envelope jets supernovae(CEJSNe) where an old neutron star or a black hole spirals-in inside the envelope and then inside the core of a red supergiant. I discuss how jets can shape the pre-explosion CSM, as in Supernova 1987A, and can power pre-explosion outbursts(precursors)in binary system progenitors of CCSNe and CEJSNe. Binary interaction also facilitates the launching of postexplosion jets. 展开更多
关键词 (stars:)supernovae:general ISM:supernova remnants stars:jets ISM:jets and outflows (stars:)binaries:general
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Mass-accreting white dwarfs and type Ia supernovae
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作者 Bo Wang 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2018年第5期1-28,共28页
Type Ia supernovae(SNe Ia) play a prominent role in understanding the evolution of the Universe. They are thought to be thermonuclear explosions of mass-accreting carbon-oxygen white dwarfs(CO WDs) in binaries, al... Type Ia supernovae(SNe Ia) play a prominent role in understanding the evolution of the Universe. They are thought to be thermonuclear explosions of mass-accreting carbon-oxygen white dwarfs(CO WDs) in binaries, although the mass donors of the accreting WDs are still not well determined. In this article, I review recent studies on mass-accreting WDs, including H-and He-accreting WDs. I also review currently most studied progenitor models of SNe Ia, i.e., the single-degenerate model(including the WD+MS channel, the WD+RG channel and the WD+He star channel), the doubledegenerate model(including the violent merger scenario) and the sub-Chandrasekhar mass model.Recent progress on these progenitor models is discussed, including the initial parameter space for producing SNe Ia, the binary evolutionary paths to SNe Ia, the progenitor candidates for SNe Ia, the possible surviving companion stars of SNe Ia, some observational constraints, etc. Some other potential progenitor models of SNe Ia are also summarized, including the hybrid CONe WD model, the core-degenerate model, the double WD collision model, the spin-up/spin-down model and the model of WDs near black holes. To date, it seems that two or more progenitor models are needed to explain the observed diversity among SNe Ia. 展开更多
关键词 supernovae general - binaries close - stars evolution - white dwarfs
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Common Envelope to Explosion Delay time Distribution(CEEDTD)of Type Ia Supernovae
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作者 Noam Soker 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2022年第3期263-270,共8页
I use recent observations of circumstellar matter(CSM)around type Ia supernovae(SNe Ia)to estimate the fraction of SNe Ia that explode into a planetary nebula(PN)and to suggest a new delay time distribution from the c... I use recent observations of circumstellar matter(CSM)around type Ia supernovae(SNe Ia)to estimate the fraction of SNe Ia that explode into a planetary nebula(PN)and to suggest a new delay time distribution from the common envelope evolution(CEE)to the SN Ia explosion for SNe Ia that occur shortly after the CEE.Under the assumption that the CSM results from a CEE,I crudely estimate that about 50%of all SNe Ia are SNe Ia inside PNe(SNIPs),and that the explosions of most SNIPs occur within a CEE to explosion delay(CEED)time of less than about ten thousand years.I also estimate that the explosion rate of SNIPs,i.e.,the CEED time distribution,is roughly constant within this timescale of ten thousand years.The short CEED time suggests that a fraction of SNIPs come from the core-degenerate(CD)scenario where the merger of the core with the white dwarf takes place at the end of the CEE.I present my view that the majority of SNIPs come from the CD scenario.I list some further observations that might support or reject my claims,and describe the challenge to theoretical studies to find a process to explain a merger to explosion delay(MED)time of up to ten thousand years or so.A long MED will apply also to the double degenerate scenario. 展开更多
关键词 (stars:)binaries(including multiple):close (stars:)white dwarfs (stars:)supernovae:general ISM:supernova remnants
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The Study of the Physical Properties and Energy Sources of Five Luminous Type Ibc Supernovae
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作者 白松瑶 王涛 +3 位作者 王善钦 甘文沛 王浏毅 梁恩维 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2023年第12期34-56,共23页
In this paper,we study five luminous supernovae(LSNe)Ibc(SN 2009ca,ASASSN-15mj,SN 2019omd,SN 2002ued,and SN 2021bmf)whose peak absolute magnitudes M_(peakare)≈-19.5 to-21 mag by fitting their multi-band light curves(... In this paper,we study five luminous supernovae(LSNe)Ibc(SN 2009ca,ASASSN-15mj,SN 2019omd,SN 2002ued,and SN 2021bmf)whose peak absolute magnitudes M_(peakare)≈-19.5 to-21 mag by fitting their multi-band light curves(LCs)with different energy source models.We find that SN 2009ca might be powered by the^(56)Ni model since the required^(56)Ni mass(0.56 M_(⊙))is comparable to those of energetic SNe Ic,while the rest four SNe cannot be accounted for the^(56)Ni model since their derived^(56)Ni masses are(?)1 M_(⊙)or the ratios of the^(56)Ni mass to the ejecta mass are larger than 0.2.This indicates that some LSNe might be powered by^(56)Ni decay,while most of them need additional energy sources.We then use the magnetar plus^(56)Ni model and the fallback plus^(56)Ni model to fit the LCs of the four LSNe that cannot be explained by the^(56)Ni model,finding that the two models can account for the four SNe,and the derived parameters are comparable to those of LSNe or superluminous SNe in the literature,if they were(mainly)powered by magnetars or fallback.We suggest that the magnetar plus^(56)Ni model is more reasonable than the fallback plus^(56)Ni model,since the validity of the fallback plus^(56)Ni model depends on the value of accretion efficiency(η)and favors a largeηvalue,and the magnetar plus^(56)Ni model yields smallerχ^(2)/dof values.It should be pointed out that,however,the fallback plus^(56)Ni model is still a promising model that can account for the four SNe in our sample as well as other LSNe. 展开更多
关键词 Stars-(stars:)supernovae general-stars MAGNETARS
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Boosting Jittering Jets by Neutrino Heating in Core Collapse Supernovae
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作者 Noam Soker 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2022年第9期77-87,共11页
I estimate the energy that neutrino heating adds to the outflow that jets induce in the collapsing core material in core collapse supernovae(CCSNe), and find that this energy crudely doubles the energy that the jets d... I estimate the energy that neutrino heating adds to the outflow that jets induce in the collapsing core material in core collapse supernovae(CCSNe), and find that this energy crudely doubles the energy that the jets deposit into the outer core. I consider the jittering jets explosion mechanism where there are several stochastic jet-launching episodes, each lasting for about 0.01–0.1 s. The collapsing core material passes through the stalled shock at about100 km and then slowly flows onto the proto-neutron star(NS). I assume that the proto-NS launches jittering jets,and that the jets break out from the stalled shock. I examine the boosting process by which the high-pressure gas inside the stalled shock, the gain region material, expands alongside the jets and does work on the material that the jets shock, the cocoon. This work is crudely equal to the energy that the original jets carry. I argue that the coupling between instabilities, stochastic rotation, magnetic fields, and jittering jets leads to most CCSN explosions. In other cases, the pre-collapse core is rapidly rotating and therefore ordered rotation replaces stochastic rotation and fixed jets replace jittering jets. 展开更多
关键词 stars:supernovae:general stars:jets ISM:supernova remnants
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Model-Synthesized Rate of Type Ia Supernovae and its Influence on the Chemical Enrichment of the ISM
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作者 Wen Guo Feng-Hui Zhang +2 位作者 Xiang-Cun Meng Zhong-Mu Li Zhan-Wen Han 《Chinese Journal of Astronomy and Astrophysics》 CSCD 2008年第1期63-70,共8页
Using Hurley's rapid binary stellar evolution code, we have studied the model-synthesized rate of Type Ia Supernovae (SNe Ia) and its influence on the chemical enrichment of the interstellar medium ejected by stell... Using Hurley's rapid binary stellar evolution code, we have studied the model-synthesized rate of Type Ia Supernovae (SNe Ia) and its influence on the chemical enrichment of the interstellar medium ejected by stellar populations. We adopt two popular scenarios, i.e., single degenerate scenario (SD) and double degenerate scenario (DD), for the progenitors of SNe Ia to calculate the rates of SNe Ia. Rates calculated in this work agree with that of Hachisu et al. and Han & Podsiadlowski, but are different from that usually adopted in chemical evolution models of galaxies. We apply the rates of SNe Ia to the chemical enrichment (especially Fe enrichment), then compare the results with previous studies. As known SNe Ia slightly affect the enrichment of C, N, O and Mg elements, while significantly affect the enrichment of Fe. We find that the occurrence and the value of the Fe enrichment in our models are earlier and smaller than that commonly adopted in chemical evolution models. We also study the evolution of [Mg/Fe] ratios, which are almost reciprocals of the Fe enrichment. The study may provide constraints on the free parameters of chemical evolution models of galaxies and evolutionary population synthesis. 展开更多
关键词 GALAXIES abundances - supernovae general-galaxies stellar content-white dwarfs
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