THE ROLE OF VARIATIONS OF CENTRAL DENSITY OF WHITE DWARF PROGENITORS UPON TYPE <font>IA</font> SUPERNOVAE

Fisher, Robert; Falta, David; Jordan, G. C.; Lamb, D. Q.

doi:10.1142/9789814307673_0033

Cited by 4 publications

(3 citation statements)

References 18 publications

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“…In the case of both an electron-capture SN and an accretion-induced white dwarf (WD) collapse, the NS forms when the degenerate Oxygen-Neon (ONe) core collapses as a consequence of electron-capture reactions, inducing a thermonuclear runaway. In MOBSE, we assume that if a growing degenerate ONe core reaches the mass M ECSN = 1.38 M it collapses due to the electron-capture on 24 Mg and on 20 Ne (Miyaji et al 1980;Nomoto 1984Nomoto , 1987Nomoto & Kondo 1991;Kitaura et al 2006;Fisher et al 2010;Jones et al 2013;Takahashi et al 2013;Schwab et al 2015;Jones et al 2016), otherwise it forms a ONe WD, which can still collapse to a NS if it will accrete sufficient mass.…”

Section: Single Star Evolution and Snementioning

confidence: 99%

The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks

Giacobbo

Mapelli

2018

Monthly Notices of the Royal Astronomical Society

310

193

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Six gravitational wave events have been reported by the LIGO-Virgo collaboration (LVC), five of them associated with black hole binary (BHB) mergers and one with a double neutron star (DNS) merger, while the coalescence of a black hole-neutron star (BHNS) binary is still missing. We investigate the progenitors of double compact object binaries with our population-synthesis code MOBSE. MOBSE includes advanced prescriptions for mass loss by stellar winds (depending on metallicity and on the Eddington ratio) and a formalism for core-collapse, electron-capture and (pulsational) pair instability supernovae. We investigate the impact of progenitor's metallicity, of the common-envelope parameter α and of the natal kicks on the properties of DNSs, BHNSs and BHBs. We find that neutron-star (NS) masses in DNSs span from 1.1 to 2.0 M , with a preference for light NSs, while NSs in merging BHNSs have mostly large masses (1.3 − 2.0 M ). BHs in merging BHNSs are preferentially low mass (5 − 15 M ). BH masses in merging BHBs strongly depend on the progenitor's metallicity and span from ∼ 5 to ∼ 45 M . The local merger rate density of both BHNSs and BHBs derived from our simulations is consistent with the values reported by the LVC in all our simulations. In contrast, the local merger rate density of DNSs matches the value inferred from the LVC only if low natal kicks are assumed. This result adds another piece to the intricate puzzle of natal kicks and DNS formation.

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Section: Single Star Evolution and Snementioning

confidence: 99%

The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks

Giacobbo

Mapelli

2018

Monthly Notices of the Royal Astronomical Society

310

193

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“…In the case of both an ECSN and an accretioninduced WD collapse, the NS forms when the degenerate Oxygen-Neon (ONe) core collapses as a consequence of electron-capture reactions, inducing a thermonuclear runaway (Miyaji et al 1980;Nomoto 1984Nomoto , 1987Nomoto & Kondo 1991;Kitaura et al 2006;Fisher et al 2010;Jones et al 2013;Takahashi et al 2013;Schwab et al 2015;Jones et al 2016).…”

Section: Electron-capture Sne (Ecsne)mentioning

confidence: 99%

The impact of electron-capture supernovae on merging double neutron stars

Giacobbo

Mapelli

2018

Monthly Notices of the Royal Astronomical Society

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Natal kicks are one of the most debated issues about double neutron star (DNS) formation. Several observational and theoretical results suggest that some DNSs have formed with low natal kicks ( 50 km s −1 ), which might be attributed to electroncapture supernovae (ECSNe). We investigate the impact of ECSNe on the formation of DNSs by means of population synthesis simulations. In particular, we assume a Maxwellian velocity distribution for the natal kick induced by ECSNe with one dimensional root-mean-square σ ECSN = 0, 7, 15, 26, 265 km s −1 . The total number of DNSs scales inversely with σ ECSN and the number of DNS mergers is higher for relatively low kicks. This effect is particularly strong if we assume low efficiency of common-envelope ejection (described by the parameter α = 1), while it is only mild for high efficiency of common-envelope ejection (α = 5). In most simulations, more than 50 per cent of the progenitors of merging DNSs undergo at least one ECSN and the ECSN is almost always the first SN occurring in the binary system. Finally, we have considered the extreme case in which all neutron stars receive a low natal kick ( 50 km s −1 ). In this case, the number of DNSs increases by a factor of ten and the percentage of merging DNSs which went through an ECSN is significantly suppressed (< 40 per cent).

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“…Our results from variations of the central density of the progenitor provide a theoretical explanation of the observed trend that type Ia supernovae from older host galaxies are systematically dimmer. Previous work [64,65,66,67,68] addressed the question of the impact of central density on brightness, with different studies reaching different conclusions. We found a strong trend of decreasing brightness with increasing central density due to increased rates of weak interactions that drive the burning toward more neutron rich products.…”

Section: Discussionmentioning

confidence: 99%

On Simulating Type Ia Supernovae

Calder

Krueger

Jackson

et al. 2012

J. Phys.: Conf. Ser.

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Type Ia supernovae are bright stellar explosions distinguished by standardizable light curves that allow for their use as distance indicators for cosmological studies. Despite their highly successful use in this capacity, the progenitors of these events are incompletely understood. We describe simulating type Ia supernovae in the paradigm of a thermonuclear runaway occurring in a massive white dwarf star. We describe the multi-scale physical processes that realistic models must incorporate and the numerical models for these that we employ. In particular, we describe a flame-capturing scheme that addresses the problem of turbulent thermonuclear combustion on unresolved scales. We present the results of our study of the systematics of type Ia supernovae including trends in brightness following from properties of the host galaxy that agree with observations. We also present performance results from simulations on leadership-class architectures.

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THE ROLE OF VARIATIONS OF CENTRAL DENSITY OF WHITE DWARF PROGENITORS UPON TYPE IA SUPERNOVAE

Cited by 4 publications

References 18 publications

The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks

The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks

The impact of electron-capture supernovae on merging double neutron stars

On Simulating Type Ia Supernovae

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