Numerical Modeling of the Early Light Curves of Type Iip Supernovae

Morozova, Viktoriya; Piro, Anthony L.; Renzo, M.; Ott, Christian D.

doi:10.3847/0004-637x/829/2/109

Cited by 56 publications

(98 citation statements)

References 73 publications

(151 reference statements)

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“…The dispersion could arise from intrinsic progenitor properties like the mass of the H envelope, the metallicity, the radius, or the characteristics of circumstellar material (CSM) around the progenitor. For example, in the last few years, several studies have shown that the majority of SNe II at early epochs present evidence of CSM interactions (e.g., Khazov et al 2016;Morozova et al 2016;Yaron et al 2017;Moriya et al 2017;Dessart et al 2017;Morozova et al 2017;Forster et al 2018). Moreover, some SNe II with strong CSM interaction have proven to be poor standard candles (de Jaeger et al 2018a).…”

Section: Introductionmentioning

confidence: 99%

The Berkeley sample of Type II supernovae: BVRI light curves and spectroscopy of 55 SNe II

Jaeger

Zheng

Stahl

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In this work, BV RI light curves of 55 Type II supernovae (SNe II) from the Lick Observatory Supernova Search program obtained with the Katzman Automatic Imaging Telescope and the 1 m Nickel telescope from 2006 to 2018 are presented. Additionally, more than 150 spectra gathered with the 3 m Shane telescope are published. We conduct an analyse of the peak absolute magnitudes, decline rates, and time durations of different phases of the light and colour curves. Typically, our light curves are sampled with a median cadence of 5.5 days for a total of 5093 photometric points. In average V-band plateau declines with a rate of 1.29 mag (100 days) −1 , which is consistent with previously published samples. For each band, the plateau slope correlates with the plateau length and the absolute peak magnitude: SNe II with steeper decline have shorter plateau duration and are brighter. A time-evolution analysis of spectral lines in term of velocities and pseudoequivalent widths is also presented in this paper. Our spectroscopic sample ranges between 1 and 200 days post-explosion and has a median ejecta expansion velocity at 50 days post-explosion of 6500 km s −1 (Hα line) and a standard dispersion of 2000 km s −1 . Nebular spectra are in good agreement with theoretical models using a progenitor star having a mass < 16 M . All the data are available to the community and will help to understand SN II diversity better, and therefore to improve their utility as cosmological distance indicators.

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Section: Introductionmentioning

confidence: 99%

The Berkeley sample of Type II supernovae: BVRI light curves and spectroscopy of 55 SNe II

Jaeger

Zheng

Stahl

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…We trace the ionization fractions of hydrogen and helium solving the Saha equations in the non-degenerate approximation as proposed in Zaghloul et al (2000). The numerical grid consists of 1000 cells and is identical to the one used in Morozova et al (2015Morozova et al ( , 2016.…”

Section: Numerical Setupmentioning

confidence: 99%

Unifying Type II Supernova Light Curves with Dense Circumstellar Material

Morozova

Piro

Valenti

2017

ApJ

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190

247

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A longstanding problem in the study of supernovae (SNe) has been the relationship between the TypeIIP and TypeIIL subclasses. Whether they come from distinct progenitors or they are from similar stars with some property that smoothly transitions from one class to another has been the subject of much debate. Here,using onedimensional radiation-hydrodynamic SN models, we showthat the multi-band light curves of SNe IIL are well fit by ordinary red supergiants surrounded by dense circumstellar material (CSM). The inferred extent of this material, coupled with a typical wind velocity of 10 100 km s 1 --, suggests enhanced activity by these stars during the last months to ∼years of their lives, which may be connected with advanced stages of nuclear burning. Furthermore, we find that,even for more plateau-like SNe,dense CSM provides a better fit to the first 20 days of their light curves, indicating that the presence of such material may be more widespread than previously appreciated. Here we choose to model the CSM with a wind-like density profile, but it is unclear whether this just generally represents some other mass distribution, such as a recent mass ejection, thick disk, or even inflated envelope material. Better understanding the exact geometry and density distribution of this material will be an important question for future studies.

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“…Such stars have extended envelopes that typically contain several solar masses of hydrogen. Analytical calculations and numerical simulations of the light curves and spectra that would result from the successful explosion of such progenitor stars are able to reproduce the main features reasonably well, including the characteristic plateau in the light curve that is the defining signature of Type II-P SNe (Popov 1993;Filippenko 1997;Bersten et al 2011;Dessart et al 2013;Morozova et al 2016). Furthermore, searches for progenitors in pre-explosion images of Type II-P SNe indeed show the presence of presumably single red supergiants at the explosion site in several cases (Van Dyk et al 2003;Smartt et al 2009).…”

Section: Introductionmentioning

confidence: 90%

The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: the role of binary interaction

Zapartas

Mink

Justham

et al. 2019

A&A

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Hydrogen-rich supernovae, known as Type II (SNe II), are the most common class of explosions observed following the collapse of the core of massive stars. We use analytical estimates and population synthesis simulations to assess the fraction of SNe II progenitors that are expected to have exchanged mass with a companion prior to explosion. We estimate that 1/3 to 1/2 of SN II progenitors have a history of mass exchange with a binary companion before exploding. The dominant binary channels leading to SN II progenitors involve the merger of binary stars. Mergers are expected to produce a diversity of SN II progenitor characteristics, depending on the evolutionary timing and properties of the merger. Alternatively, SN II progenitors from interacting binaries may have accreted mass from their companion, and subsequently been ejected from the binary system after their companion exploded. We show that the overall fraction of SN II progenitors that are predicted to have experienced binary interaction is robust against the main physical uncertainties in our models. However, the relative importance of different binary evolutionary channels is affected by changing physical assumptions. We further discuss ways in which binarity might contribute to the observed diversity of SNe II by considering potential observational signatures arising from each binary channel. For supernovae which have a substantial H-rich envelope at explosion (i.e., excluding Type IIb SNe), a surviving non-compact companion would typically indicate that the supernova progenitor star was in a wide, non-interacting binary. We argue that a significant fraction of even Type II-P SNe are expected to have gained mass from a companion prior to explosion.

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Numerical Modeling of the Early Light Curves of Type Iip Supernovae

Cited by 56 publications

References 73 publications

The Berkeley sample of Type II supernovae: BVRI light curves and spectroscopy of 55 SNe II

The Berkeley sample of Type II supernovae: BVRI light curves and spectroscopy of 55 SNe II

Unifying Type II Supernova Light Curves with Dense Circumstellar Material

The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: the role of binary interaction

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