Rapidly Evolving and Luminous Transients From Pan-Starrs1

Drout, M. R.; Chornock, R.; Söderberg, A. M.; Sanders, Nathan; McKinnon, R.; Rest, A.; Foley, R. J.; Milisavljević, D.; Margutti, R.; Berger, E.; Calkins, M.; Fong, W.; Gezari, Suvi; Huber, M. E.; Kankare, E.; Kirshner, R.; Leibler, C.; Lunnan, R.; Mattila, S.; Marion, G. H.; Narayan, Gautham; Riess, Adam G.; Roth, Kathy; Scolnic, Dan; Smartt, S. J.; Tonry, J.; Burgett, W. S.; Chambers, K.; Hodapp, Klaus W.; Jedicke, Robert; Kaiser, Nick; Magnier, E. A.; Metcalfe, N.; Morgan, J. S.; Price, P. A.; Waters, C.

doi:10.1088/0004-637x/794/1/23

Cited by 319 publications

(493 citation statements)

References 105 publications

(198 reference statements)

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“…For SN 2005ek, Mej ≈ 0.2-0.7 M⊙ and MNi ≈ 0.02-0.05 M⊙ are appropriate to fit its light curve. The event rate of these SNe is estimated as ∼ 1% of core-collapse SN rate (Drout et al 2013(Drout et al , 2014, which is also compatible with an NS merger rate estimation (Abadie et al 2010). We took a different approach from previous studies on ultra-stripped SNe (Tauris et al 2013;Tauris et al 2015).…”

Section: Summary and Discussionsupporting

confidence: 57%

“…To model these rapidly-evolving SNe with small ejecta mass, the progenitor stars are thought to be stripped much more than canonical stripped-envelope type Ib/c SNe, that is, ultra-stripped SNe coined by Tauris et al (2013); Tauris et al (2015). Besides SN 2005ek and other known SNe, ten rapidly-evolving transients were recently detected by Pan-STARRS1, which exhibit shorter decay-ing timescale (∼ 10 days) than canonical SNe with peak barometric luminosities ranging from ∼ 10 42 to 10 43 erg s −1 (Drout et al 2014). These ultra-stripped SNe are conjectured as products of close binary systems that experienced strong binary interactions, e.g.…”

Section: Introductionmentioning

confidence: 99%

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Neutrino-driven explosions of ultra-stripped Type Ic supernovae generating binary neutron stars

Suwa

Yoshida

Shibata

et al. 2015

Mon. Not. R. Astron. Soc.

102

116

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We study explosion characteristics of ultra-stripped supernovae (SNe), which are candidates of SNe generating binary neutron stars (NSs). As a first step, we perform stellar evolutionary simulations of bare carbon-oxygen cores of mass from 1.45 to 2.0 M ⊙ until the iron cores become unstable and start collapsing. We then perform axisymmetric hydrodynamics simulations with spectral neutrino transport using these stellar evolution outcomes as initial conditions. All models exhibit successful explosions driven by neutrino heating. The diagnostic explosion energy, ejecta mass, Ni mass, and NS mass are typically ∼ 10 50 erg, ∼ 0.1M ⊙ , ∼ 0.01M ⊙ , and ≈ 1.3M ⊙ , which are compatible with observations of rapidly-evolving and luminous transient such as SN 2005ek. We also find that the ultra-stripped SN is a candidate for producing the secondary low-mass NS in the observed compact binary NSs like PSR J0737-3039.

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Section: Summary and Discussionsupporting

confidence: 57%

Section: Introductionmentioning

confidence: 99%

Neutrino-driven explosions of ultra-stripped Type Ic supernovae generating binary neutron stars

Suwa

Yoshida

Shibata

et al. 2015

Mon. Not. R. Astron. Soc.

102

116

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“…The relatively recent advent of all-sky, high-cadence transient surveys has led to the discovery of many rapidly evolving, luminous transients (see Drout et al 2014, for details). Drout et al (2014) have estimated the rate of rapid transients (whose luminosity decreases by at least 50 per cent in 12 days) to be 4-8 per cent of the core-collapse rate (at a redshift z = 0.2).…”

Section: Expected Light Curve Propertiesmentioning

confidence: 99%

“…Drout et al (2014) have estimated the rate of rapid transients (whose luminosity decreases by at least 50 per cent in 12 days) to be 4-8 per cent of the core-collapse rate (at a redshift z = 0.2). Observationally, these newly discovered luminous transients form a heterogeneous group of objects, possibly suggesting a variety of explosion mechanisms.…”

Section: Expected Light Curve Propertiesmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

403

613

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The explosion of ultra-stripped stars in close binaries can lead to ejecta masses < 0.1 M ⊙ and may explain some of the recent discoveries of weak and fast optical transients. In Tau ris et al. (2013), it was demonstrated that helium star companions to neutron stars (NSs) may experience mass transfer and evolve into naked ∼ 1.5 M ⊙ metal cores, barely above the Chandrasekhar mass limit. Here we elaborate on this work and present a systematic investigation of the progenitor evolution leading to ultra-stripped supernovae (SNe). In particular, we examine the binary parameter space leading to electron-capture (EC SNe) and iron core-collapse SNe (Fe CCSNe), respectively, and determine the amount of helium ejected with applications to their observational classification as Type Ib or Type Ic. We mainly evolve systems where the SN progenitors are helium star donors of initial mass M He = 2.5 − 3.5 M ⊙ in tight binaries with orbital periods of P orb = 0.06 − 2.0 days, and hosting an accreting NS, but we also discuss the evolution of wider systems and of both more massive and lighter -as well as single -helium stars. In some cases we are able to follow the evolution until the onset of silicon burning, just a few days prior to the SN explosion. We find that ultra-stripped SNe are possible for both EC SNe and Fe CCSNe. EC SNe only occur for M He = 2.60 − 2.95 M ⊙ depending on P orb . The general outcome, however, is an Fe CCSN above this mass interval and an ONeMg or CO white dwarf for smaller masses. For the exploding stars, the amount of helium ejected is correlated with P orb -the tightest systems even having donors being stripped down to envelopes of less than 0.01 M ⊙ . We estimate the rise time of ultra-stripped SNe to be in the range 12 hr − 8 days, and light curve decay times between 1 and 50 days. A number of fitting formulae for our models are provided with applications to population synthesis. Ultrastripped SNe may produce NSs in the mass range 1.10 − 1.80 M ⊙ and are highly relevant for LIGO/VIRGO since most (possibly all) merging double NS systems have evolved through this phase. Finally, we discuss the low-velocity kicks which might be imparted on these resulting NSs at birth.

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“…While typical Type Ib/Ic SNe reach their peak luminosity in ∼ 20 days (e.g., Drout et al 2011;Prentice et al 2016), rapidly-evolving SN LCs rise in less than ∼ 10 days and decline quickly on a similar timescale (e.g., Poznanski et al 2010;Perets et al 2010;Kawabata et al 2010;Kasliwal et al 2010;Ofek et al 2010;Kasliwal et al 2012;Drout et al 2013Drout et al , 2014Inserra et al 2015). The simplest way to interpret the rapid LC evolution of some Type Ib/Ic SNe is that their ejecta mass is much smaller than in the more slowly evolving SNe (see also, e.g., Kleiser & Kasen 2014;Drout et al 2014;Tanaka et al 2016). LC evolution becomes faster with smaller ejecta mass because of the smaller diffusion timescale.…”

Section: Introductionmentioning

confidence: 99%

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Moriya

Mazzali

Tominaga

et al. 2016

Mon. Not. R. Astron. Soc.

105

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We investigate light-curve and spectral properties of ultra-stripped core-collapse supernovae. Ultra-stripped supernovae are the explosions of heavily stripped massive stars which lost their envelopes via binary interactions with a compact companion star. They eject only ∼ 0.1 M ⊙ and may be the main way to form double neutronstar systems which eventually merge emitting strong gravitational waves. We follow the evolution of an ultra-stripped supernova progenitor until iron core collapse and perform explosive nucleosynthesis calculations. We then synthesize light curves and spectra of ultra-stripped supernovae using the nucleosynthesis results and present their expected properties. Ultra-stripped supernovae synthesize ∼ 0.01 M ⊙ of radioactive 56 Ni, and their typical peak luminosity is around 10 42 erg s −1 or −16 mag. Their typical rise time is 5 − 10 days. Comparing synthesized and observed spectra, we find that SN 2005ek, some of the so-called calcium-rich gap transients, and SN 2010X may be related to ultra-stripped supernovae. If these supernovae are actually ultra-stripped supernovae, their event rate is expected to be about 1 per cent of core-collapse supernovae. Comparing the double neutron-star merger rate obtained by future gravitational-wave observations and the ultra-stripped supernova rate obtained by optical transient surveys identified with our synthesized light-curve and spectral models, we will be able to judge whether ultra-stripped supernovae are actually a major contributor to the binary neutron star population and provide constraints on binary stellar evolution.

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Rapidly Evolving and Luminous Transients From Pan-Starrs1

Cited by 319 publications

References 105 publications

Neutrino-driven explosions of ultra-stripped Type Ic supernovae generating binary neutron stars

Neutrino-driven explosions of ultra-stripped Type Ic supernovae generating binary neutron stars

Ultra-stripped supernovae: progenitors and fate

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

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