The properties of NI to CO to Fe decay

Nadyozhin, D. K.

doi:10.1086/192008

Cited by 158 publications

(128 citation statements)

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“…First, we derive a very rough estimate of what the required nickel masses would be if the SN peaks were completely powered by nickel. We use the relation a = L E (Nadyozhin 1994;Stritzinger & Leibundgut 2005), where τ Ni =8.8 days and τ Co =111.3 days, and assume no deviation from the Arnett rule (α=1, Arnett 1979). The time of explosion is quite uncertain in our sample, because the rise times are often not well-covered.…”

Section: Ni Massesmentioning

confidence: 99%

Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

Gal‐Yam

Rubin

et al. 2018

ApJ

135

126

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We investigate the light-curve properties of a sample of 26 spectroscopically confirmed hydrogen-poor superluminous supernovae (SLSNe-I) in the Palomar Transient Factory survey. These events are brighter than SNe Ib/c and SNe Ic-BL, on average, by about 4 and 2mag, respectively. The peak absolute magnitudes of SLSNe-I in rest-frame g band span −22M g −20 mag, and these peaks are not powered by radioactive 56 Ni, unless strong asymmetries are at play. The rise timescales are longer for SLSNe than for normal SNe Ib/c, by roughly 10 days, for events with similar decay times. Thus, SLSNe-I can be considered as a separate population based on photometric properties. After peak, SLSNe-I decay with a wide range of slopes, with no obvious gap between rapidly declining and slowly declining events. The latter events show more irregularities (bumps) in the light curves at all times. At late times, the SLSN-I light curves slow down and cluster around the 56 Co radioactive decay rate. Powering the late-time light curves with radioactive decay would require between 1 and 10 M e of Ni masses. Alternatively, a simple magnetar model can reasonably fit the majority of SLSNe-I light curves, with four exceptions, and can mimic the radioactive decay of 56 Co, up to ∼400 days from explosion. The resulting spin values do not correlate with the host-galaxy metallicities. Finally, the analysis of our sample cannot strengthen the case for using SLSNe-I for cosmology.

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Section: Ni Massesmentioning

confidence: 99%

Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

Gal‐Yam

Rubin

et al. 2018

ApJ

135

126

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“…For the mean lifetimes and decay energies of 56 Ni and 56 Co, we use (Nadyozhin 1994;Valenti et al 2008):…”

Section: Appendix D: Expression Of the Bolometric Luminositymentioning

confidence: 99%

Inferring supernova IIb/Ib/Ic ejecta properties from light curves and spectra: correlations from radiative-transfer models

Dessart¹,

Hillier²,

Woosley³

et al. 2016

Mon. Not. R. Astron. Soc.

139

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We present 1-D non-Local-Thermodynamic-Equilibrium time-dependent radiative-transfer simulations for a large grid of supernovae (SNe) IIb/Ib/Ic that result from the terminal explosion of the mass donor in a close-binary system. Our sample covers ejecta masses M e of 1.7-5.2 M d , kinetic energies E kin of 0.6-5.0ˆ10 51 erg, and 56 Ni masses of 0.05-0.30 M d . We find a strong correlation between the 56 Ni mass and the photometric properties at maximum, and between the rise time to bolometric maximum and the post-maximum decline rate. We confirm the small scatter in (V´R) at 10 d past R-band maximum. The quantity V m " a 2E kin {M e is comparable to the Doppler velocity measured from He I 5875Å at maximum in SNe IIb/Ib, although some scatter arises from the uncertain level of chemical mixing.The O I 7772Å line may be used for SNe Ic, but the correspondence deteriorates with higher ejecta mass/energy. We identify a temporal reversal of the Doppler velocity at maximum absorption in the " 1.05 µm feature in all models. The reversal is due to He I alone and could serve as a test for the presence of helium in SNe Ic. Because of variations in composition and ionisation, the ejecta opacity shows substantial variations with both velocity and time. This is in part the origin of the offset between our model light curves and the predictions from the Arnett model.

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“…The energy generation rates of 56 Ni and 56 Co are adopted from Nadyozhin (1994). We use the deposition factor of 56 Co as D Co = 0.968D(τ γ ) + 0.032D(355τ γ ), where τ γ is the optical depth of γ-rays, to take into account both the γ-rays energy release and the positron kinetic energy release (Nadyozhin 1994;Colgate et al 1997). We adopt κ = 0.1 cm 2 g −1 for the opacity of the SN ejecta.…”

Section: Light Curves Of Ultra-stripped Snementioning

confidence: 99%

Explosive nucleosynthesis of ultra-stripped Type Ic supernovae: application to light trans-iron elements

Yoshida¹,

Suwa²,

Umeda³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We investigate the explosive nucleosynthesis during two dimensional neutrino-driven explosion of ultra-stripped Type Ic supernovae evolved from 1.45 and 1.5 M ⊙ CO stars. These supernovae explode with the explosion energy of ∼ 10 50 erg and release ∼ 0.1 M ⊙ ejecta. The light trans-iron elements Ga-Zr are produced in the neutrinoirradiated ejecta. The abundance distribution of these elements has a large uncertainty because of the uncertainty of the electron fraction of the neutrino-irradiated ejecta. The yield of the elements will be less than 0.01 M ⊙ . Ultra-stripped supernova and core-collapse supernova evolved from a light CO core can be main sources of the light trans-iron elements. They could also produce neutron-rich nuclei 48 Ca. The ultrastripped supernovae eject 56 Ni of ∼ 0.006-0.01 M ⊙ . If most of neutrino-irradiated ejecta is proton-rich, 56 Ni will be produced more abundantly. The light curves of these supernovae indicate sub-luminous fast decaying explosion with the peak magnitude of about −15-−16. Future observations of ultra-stripped supernovae could give a constraint to the event rate of a class of neutron star mergers.

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The properties of NI to CO to Fe decay

Cited by 158 publications

References 0 publications

Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

Inferring supernova IIb/Ib/Ic ejecta properties from light curves and spectra: correlations from radiative-transfer models

Explosive nucleosynthesis of ultra-stripped Type Ic supernovae: application to light trans-iron elements

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