Max Planck Institute for Astrophysics
MPA Homepage CCSN Archive

Synthetic observables for electron-capture supernovae and low-mass core collapse supernovae (2021)

A. Kozyreva, P. Baklanov, S. Jones, G. Stockinger, H.-T. Janka

MNRAS 503, 797 (2021)
ADS, arXiv eprint 2102.02575

Stars in the mass range from 8 M⊙ to 10 M⊙ are expected to produce one of two types of supernovae (SNe), either electron-capture supernovae (ECSNe) or core-collapse supernovae (CCSNe), depending on their previous evolution. Either of the associated progenitors retain extended and massive hydrogen-rich envelopes and the observables of these SNe are, therefore, expected to be similar. In this study, we explore the differences in these two types of SNe. Specifically, we investigate three different progenitor models: a solar-metallicity ECSN progenitor with an initial mass of 8.8 M⊙, a zero-metallicity progenitor with 9.6 M⊙, and a solar-metallicity progenitor with 9 M⊙, carrying out radiative transfer simulations for these progenitors. We present the resulting light curves for these models. The models exhibit very low photospheric velocity variations of about 2000 km/s; therefore, this may serve as a convenient indicator of low-mass SNe. The ECSN has very unique light curves in broad-bands, especially the U band, and does not resemble any currently observed SN. This ECSN progenitor being part of a binary will lose its envelope for which reason the light curve becomes short and undetectable. The SN from the 9.6 M⊙ progenitor exhibits also quite an unusual light curve, explained by the absence of metals in the initial composition. The artificially iron-polluted 9.6 M⊙ model demonstrates light curves closer to normal SNe IIP. The SN from the 9 M⊙ progenitor remains the best candidate for so-called low-luminosity SNe IIP like SN 1999br and SN 2005cs.

The content of the files:

(1) time [days] (2) Tbb [K] (3) Rbb [cm] (4) Teff [K] (7) Mbol (8) U (9) B (10) V (11) I (12)R

The content of the lbol-files:

(1) time [days] (2) UBVRI-pseidobolometric [erg/s] (3) bolometric [erg/s] (4) X-ray-EUV <325Å (5) IR >890Å Luminosities are in log10-scale.

SN 2020pvb: a Type IIn-P supernova with a precursor outburst

Elias-Rosa, N. et. al.

ADS arXiv:2402.02924

In this paper, we used the model e8.8, i.e. exploded ECSN model, which we modified in the following way. The density profile was scaled with a factor of 10 to have the ejecta with the mass of 0.4 solar masses. The exploded ECSN model at day 10 after the explosion was surrounded with a circumstellar material.

The progenitor (evol7a in the plot) corresponds to an stellar evolution model with the envelope truncated to the radius of 400 solar radii and total mass of 1.7 solar masses (and ejecta mass of 0.4 solar masses), which was also published in the main paper on ECSN. We show the stellar evolution model artificially exploded (as a thermal bomb) with the energy of 0.02 foe to demonstrate the effect of interaction.

In this archive, we uploaded a few models, two of which - W1 and W2 (e88d10abW1 and e88d10abW2 in the plot) -- we published in the paper.

Models CSM parameters:
R [cm], M [M⊙], α
e88d10abW1lbol tt SED 1.5e15   2.2   2
e88d10abW2lbol tt SED 1.5e15   2.9   1
e88d10abW4lbol tt SED 1.24e15 5.3  0.5
e88d10abW4albol tt SED 1.24e15 3.9 0.75

Please contact Sasha Kozyreva via sasha.kozyreva gmail.com for any details, if needed.

In the case of making use of data from this website, please cite the Garching Core-Collapse Supernova Archive (by giving the link https://wwwmpa.mpa-garching.mpg.de/ccsnarchive/) as well as papers that are mentioned on this page. We made all possible efforts to ensure the correctness of the data in this archive. Errors, however, cannot be excluded. If any are found, we would appreciate being informed. — last update: