2017A&A...601A..29Z


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.06CEST01:16:19

2017A&A...601A..29Z - Astronomy and Astrophysics, volume 601A, 29-29 (2017/5-1)

Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction.

ZAPARTAS E., DE MINK S.E., IZZARD R.G., YOON S.-C., BADENES C., GOTBERG Y., DE KOTER A., NEIJSSEL C.J., RENZO M., SCHOOTEMEIJER A. and SHROTRIYA T.S.

Abstract (from CDS):

Most massive stars, the progenitors of core-collapse supernovae, are in close binary systems and may interact with their companion through mass transfer or merging. We undertake a population synthesis study to compute the delay-time distribution of core-collapse supernovae, that is, the supernova rate versus time following a starburst, taking into account binary interactions. We test the systematic robustness of our results by running various simulations to account for the uncertainties in our standard assumptions. We find that a significant fraction, 15+9–8%, of core-collapse supernovae are "late", that is, they occur 50-200Myr after birth, when all massive single stars have already exploded. These late events originate predominantly from binary systems with at least one, or, in most cases, with both stars initially being of intermediate mass (4-8M). The main evolutionary channels that contribute often involve either the merging of the initially more massive primary star with its companion or the engulfment of the remaining core of the primary by the expanding secondary that has accreted mass at an earlier evolutionary stage. Also, the total number of core-collapse supernovae increases by 14+15–14% because of binarity for the same initial stellar mass. The high rate implies that we should have already observed such late core-collapse supernovae, but have not recognized them as such. We argue that φ Persei is a likely progenitor and that eccentric neutron star - white dwarf systems are likely descendants. Late events can help explain the discrepancy in the delay-time distributions derived from supernova remnants in the Magellanic Clouds and extragalactic type Ia events, lowering the contribution of prompt Ia events. We discuss ways to test these predictions and speculate on the implications for supernova feedback in simulations of galaxy evolution.

Abstract Copyright: © ESO, 2017

Journal keyword(s): supernovae: general - binaries: close - stars: massive - stars: evolution - stars: evolution

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11298 1
2 SN 2002ic SN* 01 30 02.55 +21 53 06.9     18.5     SNIapec 215 1
3 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5289 1
4 * phi Per Be* 01 43 39.6379209 +50 41 19.432832 3.10 4.02 4.06 3.90 3.88 B1.5V:e-shell 541 0
5 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5921 1
6 Cl Melotte 20 OpC 03 26 42 +48 48.0           ~ 773 0
7 PSR J0537-6910 Psr 05 37 46.66 -69 10 17.1           ~ 239 1
8 NGC 2060 SNR 05 37 51.4470067818 -69 10 23.957283532   9.69 9.59     ~ 327 2
9 HD 58978 Be* 07 26 59.4826767357 -23 05 09.683936209 4.51 5.45 5.56 7.05   B0.5IVe 215 0
10 PSR J1141-6545 Psr 11 41 06.97000 -65 45 19.1600     25.08 24.38   ~ 158 1
11 SN 1994I SN* 13 29 54.072 +47 11 30.50     12.9     SNIc 584 1
12 * f01 Cyg Be* 20 59 49.5516391039 +47 31 15.378902421 3.77 4.71 4.75 4.62 4.63 B1.5Vnne 470 0
13 SN 2014C SN* 22 37 05.60 +34 24 31.9           SNIb 70 1
14 PSR J2305+4707 Psr 23 05 55.842 +47 07 45.32           ~ 211 1

    Equat.    Gal    SGal    Ecl

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2021.05.06-01:16:19

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