Study of supernovae important for cosmology

Бакланов, П. В.; Блинников, С. И.; Potashov, M. Sh.; Dolgov, A. D.

doi:10.1134/s0021364013200034

Cited by 26 publications

(11 citation statements)

References 37 publications

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“…This leads us to suggest an alternative scenario. Moriya et al (2011, Figure 7) and Baklanov et al (2013, Figure 1) present models for a family of SNe IIn, i.e. SNe IIP with circumstellar material (CSM) interaction.…”

Section: Slopes Versus Effective Wavelengthmentioning

confidence: 99%

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The rise-time of Type II supernovae

González–Gaitán

Tominaga

Molina

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We investigate the early-time light-curves of a large sample of 223 type II supernovae (SNe) from the Sloan Digital Sky Survey and the Supernova Legacy Survey. Having a cadence of a few days and sufficient non-detections prior to explosion, we constrain rise-times, i.e. the durations from estimated first to maximum light, as a function of effective wavelength. At restframe g ′ -band (λ eff = 4722Å), we find a distribution of fast rise-times with median of (7.5 ± 0.3) days. Comparing these durations with analytical shock models of Rabinak & Waxman (2013);Nakar & Sari (2010) and hydrodynamical models of Tominaga et al. (2009), which are mostly sensitive to progenitor radius at these epochs, we find a median characteristic radius of less than 400 solar radii. The inferred radii are on average much smaller than the radii obtained for observed red supergiants (RSG). Investigating the post-maximum slopes as a function of effective wavelength in the light of theoretical models, we find that massive hydrogen envelopes are still needed to explain the plateaus of SNe II. We therefore argue that the SN II rise-times we observe are either a) the shock cooling resulting from the core collapse of RSG with small and dense envelopes, or b) the delayed and prolonged shock breakout of the collapse of a RSG with an extended atmosphere or embedded within pre-SN circumstellar material.

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Section: Slopes Versus Effective Wavelengthmentioning

confidence: 99%

“…A1). At these epochs the opacity was computed taking into account the non-equilibrium radiation (for details, see Baklanov et al 2013). The LTE and non-LTE opacities are shown in right Fig.…”

Section: Appendix A: Non-lte Effects On the Risementioning

confidence: 99%

The rise-time of Type II supernovae

González–Gaitán

Tominaga

Molina

et al. 2015

Monthly Notices of the Royal Astronomical Society

Self Cite

135

147

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“…The origin of the final luminosity increase observed so far (the 2012b event) has been largely debated. The peak luminosity which is comparable to those of SNe and the broad spectral lines led to the suggestion that the 2012b event is triggered by the final SN explosion of the progenitor (e.g., Mauerhan et al 2013;Smith et al 2014;Baklanov et al 2013;Ouyed et al 2013). The 2012a event, which is similar to the precursor of SN 2010mc (Ofek et al 2013b), is linked to the pre-SN mass ejection probably caused by the violent late-phase nuclear burning (e.g., Quataert & Shiode 2012, see also Moriya 2014a).…”

Section: Introductionmentioning

confidence: 97%

SN 2009ip: CONSTRAINING THE LATEST EXPLOSION PROPERTIES BY ITS LATE-PHASE LIGHT CURVE

Moriya

2015

ApJ

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We constrain the explosion and circumstellar properties at the 2012b event of SN 2009ip based on its late-phase bolometric light curve recently reported. The explosion energy and ejected mass at the 2012b event are estimated as 0.01 M ⊙ and 2 × 10 49 erg, respectively. The circumstellar medium is assumed to have two components: an inner shell and an outer wind. The inner shell which is likely created at the 2012a event has 0.2 M ⊙ . The outer wind is created by the wind mass loss before the 2012a mass ejection, and the progenitor is estimated to have had the mass-loss rate about 0.1 M ⊙ yr −1 with the wind velocity 550 km s −1 before the 2012a event. The estimated explosion energy and ejected mass indicate that the 2012b event is not caused by a regular supernova.

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“…Other techniques include the Spectral-fitting Expanding Atmosphere Method (e.g. Baron et al 2004) for SN IIP and the Dense Shell Method (Potashov et al 2013;Baklanov et al 2013) to measure distances to SN IIn supernovae.…”

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confidence: 99%

Strongly lensed SN Refsdal: refining time delays based on the supernova explosion models

Baklanov,

Lyskova,

Blinnikov

et al. 2020

Preprint

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We explore the unique supernova (SN) "Refsdal" -the first discovered gravitationally lensed SN with multiple images. A large magnification provided by the galactic-scale lens, augmented by the cluster lens, gave us the opportunity to perform a detailed modelling of a distant SN at z 1.5. We present results of radiation hydrodynamics modelling of SN Refsdal. According to our calculations, the SN Refsdal progenitor is likely to be a more massive and energetic version of SN 1987A, i.e. a blue supergiant star with a radius of R = 50R before an explosion and a total mass of M = 26M . The total energy release is E = 5 × 10 51 erg. Reconstruction of SN light curves allowed us to obtain time delays and magnifications for the images S2-S4 relative to S1 with higher accuracy than previous estimates of Rodney et al. We estimate the Hubble constant H 0 = 68.6 +13.6 −9.7 km s −1 Mpc −1 via rescaling the time delays predicted by different lens models to match the values obtained in this work. With more photometric data on the fifth image SX, we will be able to further refine the time delay and magnification estimates for SX and obtain competitive constraints on H 0 .

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Study of supernovae important for cosmology

Cited by 26 publications

References 37 publications

The rise-time of Type II supernovae

The rise-time of Type II supernovae

SN 2009ip: CONSTRAINING THE LATEST EXPLOSION PROPERTIES BY ITS LATE-PHASE LIGHT CURVE

Strongly lensed SN Refsdal: refining time delays based on the supernova explosion models

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