Observational signatures of SNIa progenitors, as predicted by models

Hillman, Yael; Prialnik, Dina; Kovetz, A.; Shara, Michael M.

doi:10.1093/mnras/stu2235

Cited by 51 publications

(63 citation statements)

References 37 publications

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“…Several explanations have been proposed to explain the existence of single low-mass WDs: merger events either during common-envelope evolution or of two very low-mass WDs (Nelemans, 2010;Brown et al, 2011); sub-stellar companions that help to eject the envelope and get evaporated or suffer a merge (Nelemans & Tauris, 1998); strong mass loss in metal-rich stars close to the tip of the first giant branch (Kilic et al, 2007;Brown et al, 2011;Han et al, 1994;Meng et al, 2008); remnants of the companion stars in type Ia Supernovae (Justham et al, 2009;Wang & Han, 2009). However, none of this channels has been able to convincingly reproduce the observed fraction so far (see Zorotovic & Schreiber, 2017, for a review).…”

Section: Single Low-mass Wdsmentioning

confidence: 99%

Cataclysmic variable evolution and the white dwarf mass problem: A Review

Zorotovic

Schreiber

2020

Advances in Space Research

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Although the theory of cataclysmic variable (CV) evolution is able to explain several observational aspects, strong discrepancies have existed for decades between observations and theoretical predictions of the orbital period distribution, the location of the minimum period, and the space density of CVs. Moreover, it has been shown in the last decade that the average white dwarf (WD) mass observed in CVs is significantly higher than the average mass in single WDs or in detached progenitors of CVs, and that there is an absence of helium-core WDs in CVs which is not observed in their immediate detached progenitors. This highly motivated us to revise the theory of CV formation and evolution. A new empirical model for angular momentum loss in CVs was developed in order to explain the high average WD mass observed and the absence of systems with helium-core WDs. This model seems to help, at the same time, with all of the above mentioned disagreements between theory and observations. Moreover, it also provides us with a very likely explanation for the existence of low-mass WDs without a companion. Here we will review the standard model for CV evolution and the disagreements that have existed for decades between simulations and observations with their possible solutions and/or improvements. We will also summarize the recently confirmed disagreement related to the average WD mass and the fraction of helium-core WDs among CVs, as well as the development of an empirical model that allows us to solve all the disagreements, discussing the physics that could be involved.

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Section: Single Low-mass Wdsmentioning

confidence: 99%

Cataclysmic variable evolution and the white dwarf mass problem: A Review

Zorotovic

Schreiber

2020

Advances in Space Research

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“…Observed intervals between eruptions range from ∼1 year (Darnley et al 2014b(Darnley et al , for M31N 2008 up to 98 years (Schaefer 2010, with the shortest predicted recurrence period-albeit derived from incomplete observational data-being just six months ). The theoretical limits on the recurrence period of all novae may be as short as 50 days (Hillman et al 2015) or even 25 days 45 and as long as mega-years (see, for example, Starrfield et al 1985;Kovetz & Prialnik 1994;Yaron et al 2005). The shorter recurrence periods are driven by a combination of a high-mass WD and a high mass accretion rate.…”

Section: Introductionmentioning

confidence: 99%

M31N 2008-12a—THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION

Darnley

Henze

Bode

et al. 2016

ApJ

Self Cite

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The Andromeda Galaxy recurrent nova M31N 2008-12a had been observed in eruption 10 times, including yearly eruptions from 2008 to 2014. With a measured recurrence period of =  P 351 13 rec days (we believe the true value to be half of this) and a white dwarf very close to the Chandrasekhar limit, M31N 2008-12a has become the leading pre-explosion supernova type Ia progenitor candidate. Following multi-wavelength follow-up observations of the 2013 and 2014 eruptions, we initiated a campaign to ensure early detection of the predicted 2015 eruption, which triggered ambitious ground-and space-based follow-up programs. In this paper we present the 2015 detection, visible to near-infrared photometry and visible spectroscopy, and ultraviolet and X-ray observations from the Swiftobservatory. The LCOGT 2 m (Hawaii) discovered the 2015 eruption, estimated to have commenced at August 28.28±0.12 UT. The 2013-2015 eruptions are remarkably similar at all wavelengths. New early spectroscopic observations reveal short-lived emission from material with velocities ∼13,000 km s −1 ,

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“…However, the main aspects of this picture have been contested by several authors. First, the existence of the stability strip has been questioned (e.g., Idan et al 2013;Starrfield 2014;Hillman et al 2015). In fact, no stable burning is reported in the Yaron et al (2005) tables either, although the ejected mass becomes zero at the highest mass-accretion rates.…”

Section: Discussionmentioning

confidence: 99%

“…As can be seen, our baseline model (Ṁ = 10 −7 M yr −1 ) predicts the maximal SN Ia rate of ≈5.0 × 10 −4 yr −1 . For the mass-accretion rate ofṀ = 5 × 10 −7 M yr −1 considered by Hillman et al (2015), the maximal SN Ia rate becomes ≈1.1 × 10 −4 yr −1 . Interestingly, for lower mass-accretion rates, observed population of novae could in principle explain a larger fraction of SNe Ia, and for very low rates,Ṁ < ∼ 10 −9 M yr −1 , and low WD temperature, the predicted rate is compatible with the observed value.…”

Section: E-09mentioning

confidence: 99%

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Constraining the role of novae as progenitors of type Ia supernovae

Soraisam

Gilfanov

2015

A&A

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Context. With the progenitors of type Ia supernovae (SNe Ia) still eluding direct detections, various types of accreting white dwarfs (WDs) have been proposed as prospective candidates. One of the possibilities are WDs undergoing unstable nuclear burning on their surfaces. Although observations and theoretical modeling of classical novae generally suggest that more material is ejected during the explosion than is accreted, there is growing evidence that in certain accretion regimes of novae, appreciable mass accumulation by the WD in the course of unstable nuclear burning may be possible. Aims. We propose that statistics of novae in nearby galaxies may be a powerful tool to determine the role these systems play in producing SNe Ia. Methods. We used multicycle nova evolutionary models to compute the number and temporal distribution of novae that would be produced by a typical SN Ia progenitor before it reached the Chandrasekhar mass limit (M ch ) and exploded, assuming that it experienced unstable nuclear burning during its entire accretion history. We then used the observed nova rate in M 31 to constrain the maximal contribution of the nova channel to the SN Ia rate in this galaxy. Results. The M 31 nova rate measured by the POINT-AGAPE survey is ≈65 yr −1 . Assuming that all these novae will reach M ch , we estimate the maximal SN Ia rate novae may produce, which is < ∼ 0.1-0.5 × 10 −3 yr −1 . This constrains the overall contribution of the nova channel to the SN Ia rate at < ∼ 2-7%. However, if all POINT-AGAPE novae do eventually reach M ch , a significant population of fast novae (t 2 < ∼ 10 days) originating from the most massive WDs is expected, with a rate of ∼200−300 yr −1 , which is significantly higher than currently observed. We point out that statistics of such fast novae can provide powerful diagnostics of the contribution of the nova channel to the final stage of mass accumulation by the single-degenerate (SD) SN Ia progenitors. To explore the prospects of their use, we investigated the efficiency of detecting fast novae as a function of the limiting magnitude and temporal sampling of a nova survey of M 31 by a PTF class telescope. We find that a survey with the limiting magnitude of m R ≈ 22 observing at least every second night will catch ≈90% of fast novae expected in the SD scenario. Such surveys should be detecting fast novae in M 31 at a rate on the order of > ∼ 10 3 × f per year, where f is the fraction of SNe Ia that accreted in the unstable nuclear burning regime while accumulating the final ΔM ≈ 0.1 M before the supernova explosion.

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Observational signatures of SNIa progenitors, as predicted by models

Cited by 51 publications

References 37 publications

Cataclysmic variable evolution and the white dwarf mass problem: A Review

Cataclysmic variable evolution and the white dwarf mass problem: A Review

M31N 2008-12a—THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION

Constraining the role of novae as progenitors of type Ia supernovae

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