Recurrent Novae as a Progenitor System of Type Ia Supernovae. I. RS Ophiuchi Subclass: Systems with a Red Giant Companion

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.

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The effect of aspherical stellar wind of giant stars on the symbiotic channel of type Ia supernovae

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab676 ◽

2021 ◽

Author(s):

Chengyuan Wu ◽

Dongdong Liu ◽

Xiaofeng Wang ◽

Bo Wang

Keyword(s):

Mass Loss ◽

Stellar Wind ◽

Mass Loss Rate ◽

Binary Interaction ◽

Opening Angle ◽

Type Ia Supernovae ◽

Type Ia ◽

Binary Evolution ◽

Red Giant ◽

Ia Supernovae

Abstract The progenitor systems accounting for explosions of type Ia supernovae (SNe Ia) is still under debate. Symbiotic channel is one of the possible progenitor scenarios, in which the WDs in these systems increase in mass through wind accretion from their red giant companions. The mass-loss processes of the giants in the symbiotic systems could produce amount of circumstellar medium (CSM), and detections of interaction signals between SN ejecta and CSM can be used as an ideal way to distinguish different progenitor models. However, the density distribution and geometric structure of the CSM around the symbiotic systems remain highly uncertain. By assuming that the tidal torque from binary interaction can increase the mass-loss rate of the red giant and cause the stellar wind concentrate towards the equatorial plane, we provide a simplified method to estimate the density and the degree of deviation from spherical symmetry for the CSM. Based on the calculations of the binary evolutions of symbiotic systems using stellar evolution code MESA, we obtained the parameter space for producing SNe Ia. We found that SNe Ia could originate from symbiotic systems with massive carbon-oxygen white dwarfs (CO WDs), while the half-opening angle of the stellar wind from red giant towards the WD varies with the binary evolution, resulting in the formation of surrounding CSM with different geometric structures. The corresponding properties of ejecta-CSM interactions may be examined by spectropolarimetry observations in the future, from which one may find additional relationship between circumstellar environment of SNe Ia and their progenitor systems.

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Imprints of the ejecta–companion interaction in Type Ia supernovae: main-sequence, subgiant, and red giant companions

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stw2737 ◽

2016 ◽

Vol 465 (2) ◽

pp. 2060-2075 ◽

Cited By ~ 20

Author(s):

P. Boehner ◽

T. Plewa ◽

N. Langer

Keyword(s):

Main Sequence ◽

Type Ia Supernovae ◽

Type Ia ◽

Red Giant ◽

Ia Supernovae

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A new measurement of the Hubble constant using Type Ia supernovae calibrated with surface brightness fluctuations

Astronomy and Astrophysics ◽

10.1051/0004-6361/202039196 ◽

2021 ◽

Vol 647 ◽

pp. A72 ◽

Cited By ~ 3

Author(s):

Nandita Khetan ◽

Luca Izzo ◽

Marica Branchesi ◽

Radosław Wojtak ◽

Michele Cantiello ◽

...

Keyword(s):

Surface Brightness ◽

Hubble Constant ◽

Absolute Magnitude ◽

Host Galaxy ◽

Type Ia Supernovae ◽

Distance Measurements ◽

Surface Brightness Fluctuations ◽

Type Ia ◽

Red Giant ◽

Ia Supernovae

We present a new calibration of the peak absolute magnitude of Type Ia supernovae (SNe Ia) based on the surface brightness fluctuations (SBF) method, aimed at measuring the value of the Hubble constant. We build a sample of calibrating anchors consisting of 24 SNe hosted in galaxies that have SBF distance measurements. Applying a hierarchical Bayesian approach, we calibrate the SN Ia peak luminosity and extend the Hubble diagram into the Hubble flow by using a sample of 96 SNe Ia in the redshift range 0.02 < z < 0.075, which was extracted from the Combined Pantheon Sample. We estimate a value of H0 = 70.50 ± 2.37 (stat.) ± 3.38 (sys.) km s−1 Mpc−1 (i.e., 3.4% stat., 4.8% sys.), which is in agreement with the value obtained using the tip of the red giant branch calibration. It is also consistent, within errors, with the value obtained from SNe Ia calibrated with Cepheids or the value inferred from the analysis of the cosmic microwave background. We find that the SNe Ia distance moduli calibrated with SBF are on average larger by 0.07 mag than those calibrated with Cepheids. Our results point to possible differences among SNe in different types of galaxies, which could originate from different local environments and/or progenitor properties of SNe Ia. Sampling different host galaxy types, SBF offers a complementary approach to using Cepheids, which is important in addressing possible systematics. As the SBF method has the ability to reach larger distances than Cepheids, the impending entry of the Vera C. Rubin Observatory and JWST into operation will increase the number of SNe Ia hosted in galaxies where SBF distances can be measured, making SBF measurements attractive for improving the calibration of SNe Ia, as well as in the estimation of H0.

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Novae and Accreting White Dwarfs as Progenitors of Type Ia Supernovae

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312014949 ◽

2011 ◽

Vol 7 (S281) ◽

pp. 172-180

Author(s):

Mariko Kato

Keyword(s):

White Dwarfs ◽

Main Sequence ◽

Accretion Rate ◽

Type Ia Supernovae ◽

Light Curve Analysis ◽

X Ray ◽

Type Ia ◽

Recurrent Nova ◽

Red Giant ◽

Ia Supernovae

AbstractI review various phenomena associated with mass-accreting white dwarfs (WDs) in relation to progenitors of Type Ia supernovae (SNe Ia). The WD mass can be estimated from light curve analysis in multiwavelength bands based on the theory of optically thick winds. In the single degenerate scenario of SNe Ia, two main channels are known, i.e., WD + main sequence (MS) channel and WD + red giant (RG) channel. In each channel, a typical binary undergoes three evolutionary stages before explosion, i.e., the wind phase, supersoft X-ray source (SSS) phase, and recurrent nova phase, in this order because the accretion rate decreases with time as the companion mass decreases. For some accreting WDs we can identify the corresponding stage of evolution. Intermittent supersoft X-ray sources like RX J0513.9−6951 and V Sge correspond to wind phase objects. For the SSS phase, CAL 87-type objects correspond to the WD+MS channel. For the WD + RG channel, soft X-ray observations of early type galaxies give statistical evidence of SSS phase binaries. Recurrent novae of U Sco-type and RS Oph-type correspond to the WD + MS channel and WD + RG channel, respectively. The majority of recurrent novae host a very massive WD (≳ 1.35 M⊙) and often show a plateau phase in their optical light curves corresponding to the long-lasting supersoft X-ray phase. These properties are indications of increasing WD masses.

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The progenitors of type-Ia supernovae in semidetached binaries with red giant donors

Astronomy and Astrophysics ◽

10.1051/0004-6361/201833010 ◽

2019 ◽

Vol 622 ◽

pp. A35 ◽

Cited By ~ 2

Author(s):

D. Liu ◽

B. Wang ◽

H. Ge ◽

X. Chen ◽

Z. Han

Keyword(s):

Mass Transfer ◽

Parameter Space ◽

Delay Time ◽

Mass Transfer Rate ◽

Synthesis Method ◽

Mass Transfer Process ◽

Type Ia Supernovae ◽

Type Ia ◽

Red Giant ◽

Ia Supernovae

Context. The companions of the exploding carbon-oxygen white dwarfs (CO WDs) that produce type-Ia supernovae (SNe Ia) have still not been conclusively identified. A red-giant (RG) star can fill this role as the mass donor of the exploding WD − this channel for producing SNe Ia has been named the symbiotic channel. However, previous studies on this channel have given a relatively low rate of SNe Ia. Aims. We aim to systematically investigate the parameter space, Galactic rates, and delay time distributions of SNe Ia arising from the symbiotic channel under a revised mass-transfer prescription. Methods. We adopted an integrated mass-transfer prescription to calculate the mass-transfer process from a RG star onto the WD. In this prescription, the mass-transfer rate varies with the local material states. First, we obtain the parameter space that leads to SNe Ia by evolving a large number of semidetached WD+RG systems with the Eggleton stellar-evolution code. Second, we investigate the Galactic rates and delay-time distributions of SNe Ia using a binary population synthesis method. Results. The parameter space of WD+RG systems that can produce SNe Ia is enlarged significantly judging by our calculations. This channel could produce SNe Ia with intermediate and old ages, contributing up to 5% of all SNe Ia in the Galaxy. Our model increases the SN Ia rate from this channel by a factor of five. We suggest that the symbiotic systems RS Oph and T CrB are strong candidates for the progenitors of SNe Ia.

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Survey for the Binary Progenitor in SN1006 and Update on SN1572

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312015293 ◽

2011 ◽

Vol 7 (S281) ◽

pp. 322-325

Author(s):

Pilar Ruiz–Lapuente ◽

Jonay González Hernández ◽

Hugo Tabernero ◽

David Montes ◽

Ramon Canal ◽

...

Keyword(s):

Main Sequence ◽

The Other ◽

Type Ia Supernovae ◽

Main Sequence Stars ◽

Chemical Abundances ◽

Type Ia ◽

Red Giant ◽

Subgiant Stars ◽

Ia Supernovae ◽

Temperature Surface

AbstractWe have completed a survey down to R = 15 mag of the stars within a circle of 4 arcmin radius around the nominal center of the remnant of SN 1006, one of the three historical Type Ia supernovae (the other two being SN 1572 and SN 1604), in search of a possible surviving binary companion of the white dwarf whose explosion gave rise to the supernova. The stellar parameters (effective temperature, surface gravity, and metallicity), as well as the radial velocities of all the stars, have been measured from spectra obtained with the UVES spectrograph at the VLT, and from the former and the available photometry, distances have been determined. Chemical abundances of the Fe-peak elements Cr, Mn, Co, and Ni have also been measured to check for possible contamination of the stellar surface by the supernova ejecta. The limiting magnitude of the survey would allow us to find stellar companions of the red-giant type, subgiant stars, and main–sequence stars down to F5–6. Unlike in SN 1572, where a subgiant of type G0–1 has been proposed as the companion of SN 1572, for SN 1006 we can discard the possibility that SN 1006 had a red giant or subgiant companion.

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The delay time distribution of type Ia supernovae: theory and observation

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310002486 ◽

2009 ◽

Vol 5 (S262) ◽

pp. 31-35

Author(s):

Dany Vanbeveren ◽

Nicki Mennekens ◽

Jean-Pierre De Greve ◽

Erwin De Donder

Keyword(s):

Delay Time ◽

Time Distribution ◽

Theoretical Models ◽

Roche Lobe ◽

Type Ia Supernovae ◽

Population Number ◽

Common Envelope ◽

Type Ia ◽

Red Giant ◽

Ia Supernovae

AbstractUsing a population number synthesis code, the theoretical time distributions of type Ia supernovae in starburst galaxies are calculated, using competing models for the formation of such events: the single degenerate (a white dwarf accreting matter from a late main sequence or red giant companion) and double degenerate (the merger of two white dwarfs) scenario. The code includes the latest results in determining the progenitors for both models. Examples are the mass stripping effect in the case of the single degenerate scenario and the differentiation between the α- (based on the balance of energy) and γ- (based on the balance of angular momentum) description of energy conversion during common envelope evolution of binaries. The shape and extent of the obtained delay time distributions critically depends on which formation scenario is used. Comparing these results to the latest observed distributions allows to draw conclusions about the constraints put on the theoretical models by these observations. We also specifically investigate the influence of the degree of conservatism during Roche lobe overflow on the delay time distribution. We conclude that the single degenerate scenario alone cannot reproduce the observed delay time distributions, and that most double degenerate type Ia supernovae are formed through a quasi-conservative Roche lobe overflow phase followed by spiral-in, as opposed to a double common envelope evolution.

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Type Ia Progenitor Hunt in Ancient Remnants

Proceedings of the International Astronomical Union ◽

10.1017/s174392131201530x ◽

2011 ◽

Vol 7 (S281) ◽

pp. 326-330

Author(s):

Wolfgang E. Kerzendorf

Keyword(s):

Main Sequence ◽

High Resolution Spectroscopy ◽

Type Ia Supernovae ◽

Substantial Evidence ◽

Broad Agreement ◽

Accretion Process ◽

Close Proximity ◽

Type Ia ◽

Red Giant ◽

Ia Supernovae

AbstractThere is broad agreement that the stars which explode as Type Ia supernovae are white dwarfs. They have accreted material in a binary system until they are near the Chandrasekhar mass and detonate/deflagrate. The two main scenarios for this accretion process are merging with a companion white dwarf (double degenerate scenario), or accretion from a main-sequence to red giant donor (single degenerate scenario). The donor star survives post-explosion and would provide substantial evidence for the single degenerate scenario, if found. Our team is analyzing stars in close proximity to Galactic Type Ia remnants to find surviving donor stars. In my talk I will introduce the different progenitor systems and the expected state for a donor star today. I will outline our search using high resolution spectroscopy and will present updated results.

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