Type Ia supernovae from non-accreting progenitors

Antoniadis, John; Chanlaridis, S.; Gräfener, G.; Langer, N.

doi:10.1051/0004-6361/201936991

Cited by 16 publications

(14 citation statements)

References 74 publications

(101 reference statements)

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“…However, for the metallicity and mass range considered here, the assumption that the ensuing strong stellar wind blows off any remaining hydrogen within a short time remains a good approximation (Laplace et al 2020). Notably, we did not consider the lowest mass helium stars that could still produce SNe despite their low mass, and that may (Yoon et al 2010) or may not (Antoniadis et al 2020) retain their hydrogen. Whereas for the lower mass He stars considered here, a single star origin appears unlikely, it cannot be excluded that single stars with initial masses near 30 M may lose their envelope quickly after core hydrogen exhaustion (Smith & Owocki 2006;Petrov et al 2016).…”

Section: Modelmentioning

confidence: 99%

Supernovae Ib and Ic from the explosion of helium stars

Dessart

Yoon

Aguilera-Dena

et al. 2020

A&A

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Much difficulty has so far prevented the emergence of a consistent scenario for the origin of Type Ib and Ic supernovae (SNe). Either the SN rates or the ejecta masses and composition were in tension with inferred properties from observations. Here, we follow a heuristic approach by examining the fate of helium stars in the mass range from 4 to 12 M⊙, which presumably form in interacting binaries. The helium stars were evolved using stellar wind mass loss rates that agree with observations and which reproduce the observed luminosity range of galactic Wolf-Rayet stars, leading to stellar masses at core collapse in the range from 3 to 5.5 M⊙. We then exploded these models adopting an explosion energy proportional to the ejecta mass, which is roughly consistent with theoretical predictions. We imposed a fixed 56Ni mass and strong mixing. The SN radiation from 3 to 100 d was computed self-consistently, starting from the input stellar models using the time-dependent nonlocal thermodynamic equilibrium radiative-transfer code CMFGEN. By design, our fiducial models yield very similar light curves, with a rise time of about 20 d and a peak luminosity of ~1042.2 erg s−1, which is in line with representative SNe Ibc. The less massive progenitors retain a He-rich envelope and reproduce the color, line widths, and line strengths of a representative sample of SNe Ib, while stellar winds remove most of the helium in the more massive progenitors, whose spectra match typical SNe Ic in detail. The transition between the predicted Ib-like and Ic-like spectra is continuous, but it is sharp, such that the resulting models essentially form a dichotomy. Further models computed with varying explosion energy, 56Ni mass, and long-term power injection from the remnant show that a moderate variation of these parameters can reproduce much of the diversity of SNe Ibc. We conclude that massive stars stripped by a binary companion can account for the vast majority of ordinary Type Ib and Ic SNe and that stellar wind mass loss is the key to removing the helium envelope in the progenitors of SNe Ic.

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Section: Modelmentioning

confidence: 99%

Supernovae Ib and Ic from the explosion of helium stars

Dessart

Yoon

Aguilera-Dena

et al. 2020

A&A

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“…As a final remark we note that fallback SNe leading to the formation of NSs or LMG objects in symmetric explosions, may also carry broader implications for compact-object populations. For instance, they might contribute to the observed pulsar population in globular clusters, thereby serving as a substitute for L6, page 5 of 10 A&A 657, L6 (2022) NSs that formed via electron-capture SNe, which may be rarer than previously thought (Antoniadis et al 2020).…”

Section: Discussionmentioning

confidence: 99%

Explodability fluctuations of massive stellar cores enable asymmetric compact object mergers such as GW190814

Antoniadis

Aguilera-Dena

Vigna-Gómez

et al. 2022

A&A

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The first three observing runs with Advanced LIGO and Virgo have resulted in the detection of binary black hole (BBH) mergers with highly unequal mass components, which are difficult to reconcile with standard formation paradigms. The most representative of these is GW190814, a highly asymmetric merger between a 23 M⊙ black hole (BH) and a 2.6 M⊙ compact object. Here, we explore recent results, suggesting that a sizable fraction of stars with pre-collapse carbon-oxygen core masses above 10 M⊙, and extending up to at least 30 M⊙, may produce objects inside the so-called lower mass gap that bridges the division between massive pulsars and BHs in Galactic X-ray binaries. We demonstrate that such an explosion landscape would naturally cause a fraction of massive binaries to produce GW190814-like systems instead of symmetric-mass BBHs. We present examples of specific evolutionary channels leading to the formation of GW190814 and GW200210, a 24 + 2.8 M⊙ merger discovered during the O3b observing run. We estimate the merger-rate density of these events in our scenario to be 𝒪(5%) of the total BBH merger rate. Finally, we discuss the broader implications of this formation channel for compact object populations, and its possible relevance to less asymmetric merger events such as GW200105 and GW200115.

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“…to be O(200 Myr), although it might be possible to form similar ONe cores via WD mergers (Schwab et al 2016). Antoniadis et al (2020), argued that the frequency of ONe SNe Ia can be comparable to the observed SN Ib/c rates. Considering the results presented here, we update the relative ratio between ONe SNe Ia and SNe Ib/c to be 0.17-0.30 at Z = 0.02 and 0.03-0.13 at Z = 10 −4 (assuming a Chabrier 2005, initial mass function).…”

Section: Shell Burning and Envelope Ejection Prior To Collapse Near-mentioning

confidence: 99%

“…For our models that feature residual carbon in their cores, the close succession of those two reactions-forced by the forbidden transition-could have a non-negligible effect on the overall outcome by reducing the carbon ignition density. Antoniadis et al (2020) presented a case study of two heliumstar models that develop a degenerate (C)ONe core and subsequently experience a thermal runaway when their central density is 9.2 log 10 (ρ c /g cm −3 ) 9.8. These stars likely avoid e-captures on 20 Ne, and produce a (C)ONe SN Ia.…”

Section: Other Sources Of Uncertaintymentioning

confidence: 99%

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Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Chanlaridis¹,

Antoniadis²,

Aguilera-Dena³

et al. 2022

Preprint

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Context. When stripped from their hydrogen-rich envelopes, stars with initial masses between ∼7 and 11 M develop massive degenerate cores and collapse. Depending on the final structure and composition, the outcome can range from a thermonuclear explosion, to the formation of a neutron star in an electron-capture supernova (ECSN). It has been recently demonstrated that stars in this mass range may be more prone to disruption than previously thought: they may initiate explosive oxygen burning when their central densities are still below ρ c 10 9.6 g cm −3 . At the same time, their envelopes expand significantly, leading to the complete depletion of helium. This combination makes them interesting candidates for Type Ia Supernovae-which we call (C)ONe SNe Ia-and might have broader implications for the formation of neutron stars via ECSNe. Aims. To constrain the observational counterparts of (C)ONe SNe Ia and the key properties that enable them, it is crucial to constrain the evolution, composition, and pre-collapse structure of their progenitors, as well as the evolution of these quantities with cosmic time. In turn, this requires a detailed investigation of the final evolutionary stages preceding the collapse, and their sensitivity to input physics.Methods. Here, we model the evolution of 252 single, non-rotating helium-stars covering the initial mass range 0.8-3.5 M , metallicities between Z = 10 −4 and 0.02, and overshoot efficiency factors from f OV = 0.0 to 0.016 across all convective boundaries. We use these models to constrain several properties of these stars, including their central densities, compositions and envelope masses at the time of explosive oxygen ignition, and the final outcome as a function of initial helium-star mass. We further investigate the sensitivity of these properties to mass-loss rate assumptions using an additional grid of 110 models with varying wind efficiencies. Results. We find that helium-star models with masses between ∼1.8 and 2.7 M are able to evolve onto 1.35-1.37 M (C)ONe cores that initiate explosive burning at central densities between log 10 (ρ c /g cm −3 ) ∼ 9.3 and 9.6. We constrain the amount of residual carbon retained after core carbon burning as a function of initial conditions, and conclude that it plays a critical role in determining the final outcome: Chandrasekhar-mass cores with residual carbon mass fractions of X min ( 12 C) 0.004 result in (C)ONe SNe Ia, while those with lower carbon mass fractions become ECSNe. We find that (C)ONe SNe Ia are more likely to occur at high metallicities, whereas at low metallicities ECSNe dominate. We constrain the relative ratio between (C)ONe SNe Ia and SNe Ib/c to be 0.17-0.30 at Z = 0.02, and 0.03-0.13 at Z ≤ 10 −3 . Conclusions. We conclude with a discussion on potential observational properties of (C)ONe SNe Ia and their progenitors. In the few thousand years leading to the explosion, at least some progenitors should be identifiable as luminous metal-rich supergiants, embedded in hydrogen-free circumstellar nebulae.

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Type Ia supernovae from non-accreting progenitors

Cited by 16 publications

References 74 publications

Supernovae Ib and Ic from the explosion of helium stars

Supernovae Ib and Ic from the explosion of helium stars

Explodability fluctuations of massive stellar cores enable asymmetric compact object mergers such as GW190814

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

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