Type I supernovae. I - Analytic solutions for the early part of the light curve

Arnett, W. David

doi:10.1086/159681

Cited by 1,245 publications

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“…The peak brightness can be estimated according to Arnett's rule (Arnett 1982), which results in absolute magnitudes of M = −11.8, −13.4, −15.0, and −16.6 for nickel masses of 0.001, 0.005, 0.01, and 0.05 M⊙, respectively, where we gauged the relation with the models of Paper I. As the diffusion time is shorter than the radioactive decay timescale, the light curves should follow the radioactive decay law immediately after the light curve peak, until the SN becomes optically thin to gamma-rays at time τ d , when the decay of the optical light curve should accelerate.…”

Section: Expected Light Curve Propertiesmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

406

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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Section: Expected Light Curve Propertiesmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

406

613

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“…It is known that the peak luminosity of SNIa is directly linked to the amount of radioactive 56 Ni produced in the explosion [3,5]. Hence SNIa, having different magnitudes at maximum, are probably the result of the synthesis of different amounts of radioactive 56 Ni.…”

Section: Type Ia Supernovaementioning

confidence: 99%

Classification of Supernovae

Turatto

2003

Supernovae and Gamma-Ray Bursters

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Abstract. The current classification scheme for supernovae is presented. The main observational features of the supernova types are described and the physical implications briefly addressed. Differences between the homogeneous thermonuclear type Ia and similarities among the heterogeneous core collapse type Ib, Ic and II are highlighted. Transforming type IIb, narrow line type IIn, supernovae associated with GRBs and few peculiar objects are also discussed.

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“…Although we have limited information on the spectroscopic and photometric evolution of OGLE-2012-SN-006, we attempt to constrain SN parameters using the quasibolometric light curve computed before, with the initial assumption that the SN luminosity peak is mostly powered by the radioactive decays. To this aim, we fit the SN data using a toy light-curve model elaborated by Valenti et al (2008), 7 which has been shown to successfully reproduce the early-7 This model is obtained using the code of Valenti et al (2008), which is based on Arnett (1982), but accounting for the typo correction reported in Arnett (1996) -(see Wheeler et al 2014). …”

Section: Discussion and Summarymentioning

confidence: 99%

“…The model of Valenti et al (2008) is based on simple analytical approximations (Arnett 1982;Cappellaro et al 1997;Clocchiatti & Wheeler 1997), and on a division of the light curve into two periods. In the first period, the supernova is optically thick (photospheric phase); later on, it gets optically thin (nebular phase).…”

Section: Discussion and Summarymentioning

confidence: 99%

Massive stars exploding in a He-rich circumstellar medium – V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006

Pastorello

Wyrzykowski

Valenti

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present optical observations of the peculiar Type Ibn supernova (SN Ibn) OGLE-2012-SN-006, discovered and monitored by the OGLE − IV survey, and spectroscopically followed by P ESST O at late phases. Stringent pre-discovery limits constrain the explosion epoch with fair precision to JD = 2456203.8 ± 4.0. The rise time to the I-band light curve maximum is about two weeks. The object reaches the peak absolute magnitude M I = −19.65 ± 0.19 on JD = 2456218.1 ± 1.8. After maximum, the light curve declines for about 25 days with a rate of 4 mag 100d −1 . The symmetric I-band peak resembles that of canonical Type Ib/c supernovae (SNe), whereas SNe Ibn usually exhibit asymmetric and narrower early-time light curves. Since 25 days past maximum, the light curve flattens with a decline rate slower than that of the 56 Co to 56 Fe decay, although at very late phases it steepens to approach that rate. However, other observables suggest that the match with the 56 Co decay rate is a mere coincidence, and the radioactive decay is not the main mechanism powering the light curve of OGLE-2012-SN-006. An early-time spectrum is dominated by a blue continuum, with only a marginal evidence for the presence of He I lines marking this SN Type. This spectrum shows broad absorptions bluewards than 5000Å, likely O II lines, which are similar to spectral features observed in super-luminous SNe at early epochs. The object has been spectroscopically monitored by P ESST O from 90 to 180 days after peak, and these spectra show the typical features observed in a number of SN 2006jc-like events, including a blue spectral energy distribution and prominent and narrow (v F W HM ≈ 1900 km s −1 ) He I emission lines. This suggests that the ejecta are interacting with He-rich circumstellar material. The detection of broad (10 4 km s −1 ) O I and Ca II features likely produced in the SN ejecta (including the [O I] λλ6300,6364 doublet in the latest spectra) lends support to the interpretation of OGLE-2012-SN-006 as a core-collapse event.

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Type I supernovae. I - Analytic solutions for the early part of the light curve

Cited by 1,245 publications

References 0 publications

Ultra-stripped supernovae: progenitors and fate

Ultra-stripped supernovae: progenitors and fate

Classification of Supernovae

Massive stars exploding in a He-rich circumstellar medium – V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006

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