A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary

De, Kishalay; Kasliwal, M. M.; Ofek, E. O.; Moriya, Takashi J.; Burke, Jamie; Cao, Y.; Cenko, S. Bradley; Doran, Gary; Duggan, G.; Fender, R. P.; Fransson, Claes; Gal‐Yam, A.; Horesh, A.; Kulkarni, S. R.; Laher, Russ R.; Lunnan, R.; Manulis, I.; Masci, Frank J.; Mazzali, Paolo A.; Nugent, P.; Perley, D. A.; Petrushevska, T.; Piro, Anthony L.; Rumsey, C.; Sollerman, J.; Sullivan, M.; Taddia, F.

doi:10.1126/science.aas8693

Cited by 112 publications

(127 citation statements)

References 168 publications

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“…The mass of iron group ejecta falls between 0.01M and 0.04M . These values are compatible with the more modest explosion energies and nickel masses observed for hydrogen-rich low-mass progenitors (Pejcha & Prieto 2015) as well as for the ultra-stripped supernova candidates SN 2005ek (Drout et al 2013;Tauris et al 2013), SN 2010X (Kasliwal et al 2010;Moriya et al 2017) and iPTF 14gqr (De et al 2018). Thus, neutrino-driven explosion models do not appear to be underenergetic compared to observations in this mass range.…”

Section: Discussionsupporting

confidence: 81%

“…The existence of ultra-stripped supernovae was first suggested purely based on theoretical calculations of the final stages of mass transfer in close-orbit binaries (Tauris et al 2013) and it was realized that progenitors of neutron star gravitational wave mergers must have experienced such ultrastripped supernovae when the second-formed neutron star is born (Tauris et al 2013. A number of promising ultra-stripped supernova candidates have been identified based on observed properties of rapidly decaying supernova light curves (Drout et al 2013;Moriya et al 2017;De et al 2018).…”

Section: Introductionmentioning

confidence: 99%

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Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors

Müller

Tauris

Heger

et al. 2019

Monthly Notices of the Royal Astronomical Society

219

189

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We present a suite of seven 3D supernova simulations of non-rotating low-mass progenitors using multi-group neutrino transport. Our simulations cover single star progenitors with zeroage main sequence masses between 9.6M and 12.5M and (ultra)stripped-envelope progenitors with initial helium core masses between 2.8M and 3.5M . We find explosion energies between 0.1 Bethe and 0.4 Bethe, which are still rising by the end of the simulations. Although less energetic than typical events, our models are compatible with observations of less energetic explosions of low-mass progenitors. In six of our models, the mass outflow rate already exceeds the accretion rate onto the proto-neutron star, and the mass and angular momentum of the compact remnant have closely approached their final value, barring the possibility of later fallback. While the proto-neutron star is still accelerated by the gravitational tug of the asymmetric ejecta, the acceleration can be extrapolated to obtain estimates for the final kick velocity. We obtain gravitational neutron star masses between 1.22M and 1.44M , kick velocities between 11 km s −1 and 695 km s −1 , and spin periods from 20 ms to 2.7 s, which suggests that typical neutron star birth properties can be naturally obtained in the neutrino-driven paradigm. We find a loose correlation between the explosion energy and the kick velocity. There is no indication of spin-kick alignment, but a correlation between the kick velocity and the neutron star angular momentum, which needs to be investigated further as a potential point of tension between models and observations.

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Section: Discussionsupporting

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors

Müller

Tauris

Heger

et al. 2019

Monthly Notices of the Royal Astronomical Society

219

189

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“…USSNe are a proposed class linked to rapidly fading transients that are thought to be produced through the interaction of evolved massive stars, which have lost the majority of their envelopes via stripping by a neutron star in a close binary orbit (Tauris et al 2015). iPTF14gqr (De et al 2018), and perhaps SN 2010X (Moriya et al 2017), have been suggested to be members of this class. USSNe reach a V -band peak of approximately −16 mag, whilst LSQ13ddu is brighter by more than a factor of 100 at a peak of −19.7 mag.…”

Section: Light Curve Comparisonsmentioning

confidence: 99%

LSQ13ddu: a rapidly evolving stripped-envelope supernova with early circumstellar interaction signatures

Clark

Maguire

Inserra

et al. 2020

Monthly Notices of the Royal Astronomical Society

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This paper describes the rapidly evolving and unusual supernova LSQ13ddu, discovered by the La Silla-QUEST survey. LSQ13ddu displayed a rapid rise of just 4.8±0.9 d to reach a peak brightness of −19.70±0.02 mag in the LSQgr band. Early spectra of LSQ13ddu showed the presence of weak and narrow He i features arising from interaction with circumstellar material (CSM). These interaction signatures weakened quickly, with broad features consistent with those seen in stripped-envelope SNe becoming dominant around two weeks after maximum. The narrow He i velocities are consistent with the wind velocities of luminous blue variables but its spectra lack the typically seen hydrogen features. The fast and bright early light curve is inconsistent with radioactive 56 Ni powering but can be explained through a combination of CSM interaction and an underlying 56 Ni decay component that dominates the later time behaviour of LSQ13ddu. Based on the strength of the underlying broad features, LSQ13ddu appears deficient in He compared to standard SNe Ib.

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“…The He star is then expected to eventually undergo a SN explosion, which may either form a BNS that merges within a Hubble time, a BNS that is effectively stalled, an unbound BNS, or a NSBH system. The recent detection of a candidate ultra-stripped SN (De et al 2018) has provided additional strong evidence that HeNS binaries are the progenitors of BNSs (e.g., Dewi et al 2002;Ivanova et al 2003;Tauris et al 2013Tauris et al , 2015.…”

Section: Supernova Mass Loss Natal Kicks and Gravitational Radiationmentioning

confidence: 99%

Gravitational waves from supernova mass loss and natal kicks in close binaries

Holgado

Ricker

2019

Monthly Notices of the Royal Astronomical Society

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Some fraction of compact binaries that merge within a Hubble time may have formed from two massive stars in isolation. For this isolated-binary formation channel, binaries need to survive two supernova (SN) explosions in addition to surviving common-envelope evolution. For the SN explosions, both the mass loss and natal kicks change the orbital characteristics, producing either a bound or unbound binary. We show that gravitational waves (GWs) may be produced not only from the core-collapse SN process, but also from the SN mass loss and SN natal kick during the pre-SN to post-SN binary transition. We model the dynamical evolution of a binary at the time of the second SN explosion with an equation of motion that accounts for the finite timescales of the SN mass loss and the SN natal kick. From the dynamical evolution of the binary, we calculate the GW burst signals associated with the SN natal kicks. We find that such GW bursts may be of interest to future mid-band GW detectors like DECIGO. We also find that the energy radiated away from the GWs emitted due to the SN mass loss and natal kick may be a significant fraction, 10%, of the post-SN binary's orbital energy. For unbound post-SN binaries, the energy radiated away in GWs tends to be higher than that of bound binaries.

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A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary

Cited by 112 publications

References 168 publications

Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors

Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors

LSQ13ddu: a rapidly evolving stripped-envelope supernova with early circumstellar interaction signatures

Gravitational waves from supernova mass loss and natal kicks in close binaries

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