scholarly journals A Study of Magnetized White Dwarf + Helium Star Binary Evolution to Type Ia Supernovae

2021 ◽  
Author(s):  
Zhe Cui ◽  
Xiangdong Li
Keyword(s):  
White Dwarf ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Binary Evolution ◽  
Star Binary ◽  
Helium Star ◽  
Ia Supernovae

scholarly journals Circumstellar properties of Type Ia supernovae from the helium star donor channel

2019 ◽  
Vol 488 (3) ◽  
pp. 3949-3956
Author(s):  
Takashi J Moriya ◽  
Dongdong Liu ◽  
Bo Wang ◽  
Zheng-Wei Liu
Keyword(s):  
Radio Emission ◽  
Large Fraction ◽  
Supernova Explosion ◽  
Type Ia Supernovae ◽  
Companion Star ◽  
Type Ia Supernova ◽  
Type Ia ◽  
Binary Evolution ◽  
Helium Star ◽  
Ia Supernovae

ABSTRACT We investigate the predicted circumstellar properties of Type Ia supernova progenitor systems with non-degenerate helium star donors. It has been suggested that systems consisting of a carbon + oxygen white dwarf and a helium star can lead to Type Ia supernova explosions. Binary evolution calculations for the helium star donor channel predict that such a progenitor system is in either a stable helium-shell burning phase or a weak helium-shell flash phase at the time of the Type Ia supernova explosion. By using the binary evolution models from our previous study, we show that a large fraction of the progenitor systems with a helium star donor have a low enough density to explain the current non-detection of radio emission from Type Ia supernovae. Most of the progenitor systems in the weak helium-shell flash phase at the time of the Type Ia supernova explosion, which may dominate the prompt (short delay time) Type Ia supernova population, have both a low circumstellar density and a faint helium star donor, which could account for the non-detection of radio emission and a pre-explosion companion star in SN 2011fe and SN 2014J. We also find some progenitor systems that are consistent with the properties of the companion star candidate identified at the explosion location of the Type Iax SN 2012Z.

scholarly journals Two delays in white dwarf evolution revealed by Gaia

2019 ◽  
Vol 15 (S357) ◽  
pp. 175-178
Author(s):  
Sihao Cheng
Keyword(s):  
White Dwarf ◽  
White Dwarfs ◽  
The Other ◽  
High Mass ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Two Delays ◽  
Binary Evolution ◽  
Ia Supernovae

AbstractBy comparing two age indicators of high-mass white dwarfs (WDs) derived from Gaia data, two discoveries have been made recently: one is the existence of a cooling anomaly that produces the Q branch structure on the Hertzsprung–Russell diagram, and the other is the existence of high-mass WDs as double-WD merger products. The former poses a challenge for WD cooling models, and the latter has implications on binary evolution and type-Ia supernovae.

scholarly journals Helium double-detonation explosions for the progenitors of type Ia supernovae

2013 ◽  
Vol 9 (S298) ◽  
pp. 442-442
Author(s):  
B. Wang ◽  
D. Liu ◽  
S. Jia ◽  
Z. Han
Keyword(s):  
White Dwarf ◽  
Type Ia Supernovae ◽  
Mass Model ◽  
Type Ia ◽  
Helium Star ◽  
Ia Supernovae ◽  
Detonation Model

AbstractThermonuclear explosions from helium double-detonation sub-Chandrasekhar mass model have been considered as an alternative way for the production of type Ia supernovae (SNe Ia). In this work, we systematically studied the helium double-detonation model, in which a carbon–oxygen white dwarf (CO WD) accumulates a helium layer from a non-degenerate helium star.

scholarly journals Helium Star Donor Channel to Type Ia Supernovae and Their Surviving Companion Stars

2011 ◽  
Vol 7 (S281) ◽  
pp. 205-208
Author(s):  
Bo Wang ◽  
Zhanwen Han
Keyword(s):  
Main Sequence ◽  
Type Ia Supernovae ◽  
Population Synthesis ◽  
Short Delay ◽  
Delay Times ◽  
Spatial Velocity ◽  
Type Ia ◽  
Helium Star ◽  
Ia Supernovae ◽  
Synthesis Approach

AbstractEmploying Eggleton's stellar evolution code and assuming optically thick winds, we systematically studied the He star donor channel of Type Ia supernovae (SNe Ia), in which a carbon-oxygen white dwarf (WD) accretes material from a He main-sequence star or a He subgiant to increase its mass to the Chandrasekhar mass. We mapped out the initial parameters for producing SNe Ia in the orbital period–secondary mass plane for various WD masses from this channel. Based on a detailed binary population synthesis approach, we find that this channel can produce SNe Ia with short delay times (~100 Myr) implied by recent observations. We derived many properties of the surviving companions of this channel after SN explosion, which can be tested by future observations. We also find that the surviving companions from the SN explosion scenario have a high spatial velocity (>400 km/s), which could be an alternative origin for hypervelocity stars (HVSs), especially for HVSs such as US 708.

scholarly journals Are the Precursors of Type Ia Supernovae Double Degenerate Mergers?

2004 ◽  
Vol 194 ◽  
pp. 111-112
Author(s):  
Lilia Ferrario
Keyword(s):  
Neutron Stars ◽  
White Dwarf ◽  
White Dwarfs ◽  
Observational Evidence ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae

AbstractI argue that the observational evidence for white dwarf-white dwarf mergers supports the view that they give rise to ultra-massive white dwarfs or neutron stars through accretion induced collapse. The implications for the progenitors of Type Ia SNe are discussed.

scholarly journals Symbiotic Stars as Possible Progenitors of SNe Ia: Binary Parameters and Overall Outlook

2011 ◽  
Vol 7 (S281) ◽  
pp. 162-165 ◽  
Author(s):  
J. Mikołajewska
Keyword(s):  
White Dwarf ◽  
Physical Characteristics ◽  
Type Ia Supernovae ◽  
Symbiotic Stars ◽  
Type Ia ◽  
Red Giant ◽  
Ia Supernovae

AbstractSymbiotic stars are interacting binaries in which the first-formed white dwarf accretes and burns material from a red giant companion. This paper aims at presenting physical characteristics of these objects and discussing their possible link with progenitors of Type Ia supernovae.

scholarly journals Type IA Supernovae

1992 ◽  
Vol 151 ◽  
pp. 225-234
Author(s):  
J. Craig Wheeler
Keyword(s):  
White Dwarf ◽  
Cataclysmic Variables ◽  
Type Ia Supernovae ◽  
Low Velocity ◽  
Severe Problem ◽  
Transfer Rates ◽  
Secular Evolution ◽  
Thermonuclear Explosion ◽  
Type Ia ◽  
Ia Supernovae

Spectral calculations show that a model based on the thermonuclear explosion of a degenerate carbon/oxygen white dwarf provides excellent agreement with observations of Type Ia supernovae. Identification of suitable evolutionary progenitors remains a severe problem. General problems with estimation of supernova rates are outlined and the origin of Type Ia supernovae from double degenerate systems are discussed in the context of new rates of explosion per H band luminosity, the lack of observed candidates, and the likely presence of H in the vicinity of some SN Ia events. Re-examination of the problems of triggering Type Ia by accretion of hydrogen from a companion shows that there may be an avenue involving cataclysmic variables, especially if extreme hibernation occurs. Novae may channel accreting white dwarfs to a unique locus in accretion rate/mass space. Systems that undergo secular evolution to higher mass transfer rates could lead to just the conditions necessary for a Type Ia explosion. Tests involving fluorescence or absorption in a surrounding circumstellar medium and the detection of hydrogen stripped from a companion, which should appear at low velocity inside the white dwarf ejecta, are suggested. Possible observational confirmation of the former is described.

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