2021A&A...656A..61D


Query : 2021A&A...656A..61D

2021A&A...656A..61D - Astronomy and Astrophysics, volume 656A, 61-61 (2021/12-1)

Nebular phase properties of supernova Ibc from He-star explosions.

DESSART L., HILLIER D.J., SUKHBOLD T., WOOSLEY S.E. and JANKA H.-T.

Abstract (from CDS):

Following our recent work on TypeII supernovae (SNe), we present a set of 1D nonlocal thermodynamic equilibrium radiative transfer calculations for nebular-phase TypeIbc SNe starting from state-of-the-art explosion models with detailed nucleosynthesis. Our grid of progenitor models is derived from He stars that were subsequently evolved under the influence of wind mass loss. These He stars, which most likely form through binary mass exchange, synthesize less oxygen than their single-star counterparts with the same zero-age main sequence (ZAMS) mass. This reduction is greater in He-star models evolved with an enhanced mass loss rate. We obtain a wide range of spectral properties at 200 d.In models from He stars with an initial mass > 6 M, the [OI] λλ 6300, 6364 is of a comparable or greater strength than [CaII] λλ 7291, 7323 - the strength of [OI] λλ 6300, 6364 increases with the He-star initial mass.In contrast, models from lower mass He stars exhibit a weak [OI] λλ 6300, 6364, strong [CaII] λλ 7291, 7323, and also strong NII lines and FeII emission below 5500 Å. The ejecta density, which is modulated by the ejecta mass, the explosion energy, and clumping, has a critical impact on gas ionization, line cooling, and spectral properties. We note that FeII dominates the emission below 5500 Å and is stronger at earlier nebular epochs.It ebbs as the SN ages, while the fractional flux in [OI] λλ 6300, 6364 and [CaII] λλ 7291, 7323 increases with a similar rate as the ejecta recombine. Although the results depend on the adopted wind mass loss rate and pre-SN mass, we find that He-stars of 6-8 M initially (ZAMS mass of 23-28 M) match the properties of standard SNeIbc adequately. This finding agrees with the offset in progenitor masses inferred from the environments of SNeIbc relative to SNeII. Our results for less massive He stars are more perplexing since the predicted spectra are not seen in nature. They may be missed by current surveys or associated with TypeIbn SNe in which interaction power dominates over decay power.

Abstract Copyright: © L. Dessart et al. 2021

Journal keyword(s): radiative transfer - stars: evolution - supernovae: general - binaries: general

VizieR on-line data: <Available at CDS (J/A+A/656/A61): tablea.dat tablea3.dat-tablea23.dat>

Simbad objects: 16

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Number of rows : 16
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 SN 2016gkg SN* 01 34 14.46 -29 26 25.0           SNIIb 75 0
2 SN 2002ap SN* 01 36 23.85 +15 45 13.2   13.11 14.54     SNIc-BL 547 1
3 SN 2007gr SN* 02 43 27.98 +37 20 44.7       12.77   SNIc 217 1
4 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5102 0
5 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4781 2
6 SN 2006jc SN* 09 17 20.78 +41 54 32.7     13.8     SNIbn 319 1
7 SN 1993J SN* 09 55 24.77476 +69 01 13.7026   10.8 12.0     SNIIb 1362 1
8 SN 2013ge SN* 10 34 48.46 +21 39 41.9           SNIc 43 1
9 SN 2004aw SN* 11 57 50.24 +25 15 55.1   18.06       SNIc 188 1
10 SN 2020oi SN* 12 22 54.930 +15 49 24.96           SNIc 33 0
11 SN 2008ax SN* 12 30 40.80 +41 38 16.1   23.6 23.5 14.1 22.6 SNIIb 244 1
12 SN 2012au SN* 12 54 52.18 -10 14 50.2           SNIb 56 2
13 SN 2007C SN* 13 08 49.30 -06 47 01.0 18.1 17.1 15.9     SNIb 50 1
14 SN 2011dh SN* 13 30 05.10555 +47 10 10.9227           SNIIb 351 1
15 SN 2009jf SN* 23 04 52.98 +12 19 59.5           SNIb 99 1
16 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2668 1

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2023.01.30-23:05:35

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