J/A+A/700/A253 Binary mass transfer model data. II. (Schneider+, 2025)
Supernovae from stellar mergers and accretors of binary mass transfer:
Implications for Type IIP, 1987A-like and interacting supernovae.
Schneider F.R.N., Laplace E., Podsiadlowski P.
<Astron. Astrophys. 700, A253 (2025)>
=2025A&A...700A.253S 2025A&A...700A.253S (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Supernovae
Keywords: binaries: general - stars: black holes - stars: massive -
stars: neutron - supernovae: general -
Abstract:
As most massive stars are born in binary and other multiple-star
systems, many are expected to exchange mass with a companion
star or merge with it during their lives. This means that most
supernovae (SNe) are from such binary products. Here, we focus on
hydrogen-rich Type II SNe from accretors of binary mass transfer and
stellar mergers, and contrast them to those from single stars. We
compute various SN properties such as the explosion energies, nickel
yields, and neutron star (NS) kick velocities, but also consider NS
masses. We find tight correlations between these parameters and
various summary variables of the pre-SN core structures of stars such
as the central specific entropy, core compactness, and iron core mass.
However, there is no obvious relation between these explosion
properties and the evolutionary history of the pre-SN stars (i.e.
single stars vs. binary mass accretors and stellar mergers). We find
linear relations between the nickel mass and the SN explosion energy
and the NS remnant mass, and motivate the reasons for such relations
in our models. These relations allow, in principle, for the
determination of SN explosion energies and NS masses from nickel
masses, e.g., inferred from the tail of SN light curves. We further
group our models into progenitors of SNe IIP, SN 1987A- like and
interacting SNe, predict their SN and SN-progenitor properties and
compare these to observations. Overall, there is good agreement, but
we also highlight some tension. Accretors of binary mass transfer and
stellar mergers naturally produce SNe IIP with long plateau durations
from progenitors with relatively small CO-cores but large envelope
masses that could explain SNe such as SN 2015ba. Our models give rise
to tight relations between the plateau luminosity and the nickel mass
as well as the SN ejecta velocity as inferred observationally for SNe
IIP. We speculate that cool/red supergiants at log L/L☉≥5.5
encounter enhanced mass loss due to envelope instabilities and that
some could retain a hydrogen envelope to then explode in interacting
SNe IIn. The rate of such SNe from our models seems compatible with
the observed SN IIn rate. Some of our binary models explode as 106
L☉ blue supergiants that may have encountered enhanced and/or
eruptive mass loss shortly before their SNe and could thus help
understand interacting SNe such as SN 1961V and SN 2005gl but also
superluminous Type II SNe such as SN 2010jl.
Description:
We have studied the SN outcomes (i.e. explosion energies, nickel
yields, NS kick velocities and NS masses) and likely SN types of
accretors of binary mass transfer and stellar mergers computed in
Paper I (Schneider et al., 2024A&A...686A..45S 2024A&A...686A..45S, Cat. J/A+A/686/A45) .
The SN types SN IIP, SN 1987A-like and interacting SN IIn were
assigned to the models based on their position in the HR diagram.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 110 485 Pre-SN and SN explosion properties of the
presented stellar models
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See also:
J/A+A/686/A45 : Binary mass transfer model data (Schneider+, 2024)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 F4.1 Msun Mini [11/75] Initial mass
6- 13 A8 --- Case Mass-transfer case
15- 19 F5.2 --- facc [0.1/2.0]? Accretion fraction in units
of initial mass of star
21- 25 F5.1 Myr tcc [3.7/24.9]? Time to core collapse
27- 32 F6.1 Msun Mcc [10.0/189.9]? Final stellar mass
34- 38 F5.1 Msun MCO [2.0/41.9]? CO core mass
40- 44 F5.2 --- sc/NA/kB [0.76/1.64]? Central specific entropy
46- 47 A2 --- SN Supernova type, BH or II
49- 55 F7.2 Msun Mrm [1.3/189.9]? Compact remnant mass
57- 61 F5.1 Msun Mej [0.0/97.6]? Supernova ejecta mass
63- 68 F6.1 Msun MHenv [0.0/159.7]? Mass of the hydrogen-rich
envelope
70 I1 --- Fallback [0/1]? Flag whether SN fallback occurred
72- 76 F5.2 [Lsun] logLcc [4.76/6.93]? Stellar luminosity
at core collapse
78- 82 F5.2 [K] logTeffcc [3.52/5.49]? Effective temperature
at core collapse
84- 87 I4 Rsun Rcc [0/1215]? Stellar radius at core collapse
89- 93 F5.1 10+4yr dtLBV [0.0/58.1]? Duration inside S Doradus
instability strip in HR diagram
95- 99 F5.2 10+44J Eexpl [0.00/3.24]? Explosion energy (in 1051erg)
101-105 F5.2 Msun MNi [0.00/0.25]? Nickel ejecta mass
107-110 I4 km/s vkick [0/1853]? Neutron star kick velocity
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Acknowledgements:
Fabian Schneider, fabian.schneider(at)h-its.org
References:
Schneider et al., Paper I 2024A&A...686A..45S 2024A&A...686A..45S, Cat. J/A+A/686/A45
(End) Patricia Vannier [CDS] 16-Jul-2025