scholarly journals Type Ia Progenitor Hunt in Ancient Remnants

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.

scholarly journals Novae and Accreting White Dwarfs as Progenitors of Type Ia Supernovae

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.

scholarly journals Survey for the Binary Progenitor in SN1006 and Update on SN1572

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.

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

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.

scholarly journals HD 74438: A tight spectroscopic quadruple as possible progenitor of sub-Chandrasekhar Type Ia supernovae

2021 ◽  
Author(s):  
Thibault Merle ◽  
Adrian Hamers ◽  
Sophie Van Eck ◽  
Alain Jorissen ◽  
Mathieu Van der Swaelmen ◽  
...  
Keyword(s):  
Open Cluster ◽  
High Resolution Spectroscopy ◽  
Type Ia Supernovae ◽  
Multiple Systems ◽  
Future Evolution ◽  
Excellent Candidate ◽  
The Galaxy ◽  
Type Ia ◽  
Ia Supernovae

Abstract Stars often form in multiple systems and may follow a complex evolution involving mass transfer and collisions, leading to mergers that are possible progenitors of Type Ia supernovae (SNe) [1, 2]. The progenitors of such explosions are still highly debated [3]. While binaries have received much attention so far, higher-order stellar systems show a wide variety of interactions especially in tight systems, like long-term gravitational effects playing a key role in triple (where they are called von Zeipel-Lidov-Kozai , [4, 5], hereafter ZLK, oscillations) and quadruple systems. Here we report on the properties of the first spectroscopic quadruple (SB4) found within a star cluster: the 2+2 hierarchical system HD 74438 [6]. Its membership in the open cluster IC 2391 makes it the youngest (43 My) SB4 discovered so far. The eccentricity of the 6 y outer period is 0.46 and the two inner orbits, with periods of 20.5 d and 4.4 d, and eccentricities of 0.36 and 0.15, are not coplanar. Using an innovative combination of ground-based high resolution spectroscopy [7, 8, 9, 10] and Gaia/Hipparcos astrometry [11, 12, 13, 14], we show that this system is undergoing secular interaction that likely pumped the eccentricity of one of the inner orbit higher than expected for the spectral types of its components. We compute the future evolution of HD 74438 by considering gravitational dynamics, stellar evolution, and binary interactions [15], and show that this system is an excellent candidate progenitor of sub-Chandrasekhar Type Ia supernova through white dwarf (WD) mergers. This specific type of SNIa better accounts for the chemical evolution of iron-peak elements in the Galaxy [16].

scholarly journals The Changing Nature of QU Carinae: SN Ia Progenitor or a Hoax?

2011 ◽  
Vol 7 (S281) ◽  
pp. 149-153
Author(s):  
Stella Kafka
Keyword(s):  
Supernova Explosion ◽  
High Resolution Spectroscopy ◽  
High Mass ◽  
Type Ia Supernovae ◽  
Variable Nature ◽  
Type Ia ◽  
Chandrasekhar Limit ◽  
Ia Supernovae ◽  
Mass Accumulation

AbstractThe race to the elusive Type Ia supernovae (SNe Ia) progenitors is at its zenith, with numerous clues from SNe Ia ejecta and a dearth of observational candidates. Still, the single degenerate channel is a viable route of mass accumulation onto a white dwarf to the Chandrasekhar limit. I present long-term high resolution spectroscopy of QU Carinae, one of the most promising single degenerate SNe Ia progenitors. I discuss its highly variable nature and compare it to current scenarios for mass accumulation onto high-mass white dwarfs, eventually leading to WD detonation and to a supernova explosion.

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