J/A+A/686/A45 Binary mass transfer model data (Schneider+, 2024)
Pre-supernova evolution and final fate of stellar mergers and accretors of
binary mass transfer.
Schneider F.R.N., Podsiadlowski P., Laplace E.
<Astron. Astrophys. 686, A45 (2024)>
=2024A&A...686A..45S 2024A&A...686A..45S (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Supernovae
Keywords: binaries: general - stars: black holes - stars: evolution -
stars: massive - stars: neutron - supernovae: general
Abstract:
The majority of massive stars are expected to exchange mass or merge
with a companion during their lives. This immediately implies that
most supernovae (SNe) are from such post-mass-exchange objects. Here,
we explore how mass accretion and merging affect the pre-SN structures
of stars and their final fates. To this end, we modelled these complex
processes by rapid mass accretion onto stars of different evolutionary
stages and followed their evolution up to iron core collapse. We used
the stellar evolution code MESA and inferred the outcome of
core-collapse using a neutrino-driven SN model. Our models cover
initial masses from 11 to 70M☉ and the accreted mass ranges from
10-200% of the initial mass. All models are non-rotating and for solar
metallicity. The rapid accretion model offers a systematic way to
approach the landscape of mass accretion and stellar mergers. It is
naturally limited in scope and serves as a clean zeroth order baseline
for these processes. We find that mass accretion, in particular onto
post-main-sequence (post-MS) stars, can lead to a long-lived blue
supergiant (BSG) phase during which stars burn helium in their cores.
In comparison to genuine single stars, post-MS accretors have small
core-to-total mass ratios, regardless of whether they end their lives
as BSGs or cool supergiants (CSGs), and they can have genuinely
different pre-SN core structures. As in single and binary-stripped
stars, we find black-hole (BH) formation for the same characteristic
CO core masses MCO of ∼7M☉ and ≳13M☉. In models with
the largest mass accretion, the BH formation landscape as a function
of MCO is shifted by about 0.5M☉ to lower masses, that is,
such accretors are more difficult to explode. We find a tight relation
between our neutron-star (NS) masses and the central entropy of the
pre-SN models in all accretors and single stars, suggesting a
universal relation that is independent of the evolutionary history of
stars. Post-MS accretors explode both as BSGs and CSGs, and we show
how to understand their pre-SN locations in the Hertzsprung-Russell
(HR) diagram. Accretors exploding as CSGs can have much higher
envelope masses than single stars. Some BSGs that avoid the
luminous-blue-variable (LBV) regime in the HR diagram are predicted to
collapse into BHs of up to 50M☉, while others explode in SNe and
eject up to 40M☉, greatly exceeding ejecta masses from single
stars. Both the BH and SN ejecta masses increase to about 80M☉
in our models when allowing for multiple mergers, for example, in
initial triple-star systems, and they can be even higher at lower
metallicities. Such high BH masses may fall into the
pair-instability-SN mass gap and could help explain binary BH mergers
involving very massive BHs as observed in GW190521. We further find
that some of the BSG models explode as LBVs, which may lead to
interacting SNe and possibly even superluminous SNe.
Description:
The stellar models were computed with revision 10398 of the
Modules-for-Experiments-in-Stellar-Astrophysics (MESA) software
package (Paxton et al., 2011ApJS..192....3P 2011ApJS..192....3P, 2013ApJS..208....4P 2013ApJS..208....4P,
2015ApJS..220...15P 2015ApJS..220...15P, 2018ApJS..234...34P 2018ApJS..234...34P, 2019ApJS..243...10P 2019ApJS..243...10P). We
used the same basic MESA setup as in Schneider et al.
(2021A&A...645A...5S 2021A&A...645A...5S) and briefly summarise it in Sect. 2.1. In Sect.
2.2, we explain how we model binary-star accretion. For comparison of
these accretion models with genuine single stars, we employ the
single-star models of Schneider et al. (2021A&A...645A...5S 2021A&A...645A...5S). In Sect.
2.3, we briefly describe how we coupled our models to a SN code to
study their final fates and possible SN explosions. An overview of all
models and key properties discussed in this work are provided in Table
A.1. MESA inlists and other settings required to reproduce our models
are published online on Zenodo
(https://zenodo.org/doi/10.5281/zenodo.10731998).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 130 485 Stellar model data
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
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]? 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 Mfinal [10.0/189.9]? Final stellar mass
34- 38 F5.1 Msun MHe [2.4/41.1]? Helium core mass
40- 44 F5.1 Msun MCO [2.0/41.9]? CO core mass
46- 50 F5.2 Msun MFe [1.46/6.18]? Iron core mass
52- 56 F5.2 --- compact [0.01/0.95]? Compactness parameter
58- 62 F5.2 --- mu4 [0.02/0.6]? Dimensionless dm/dr at s=4
64- 68 F5.2 --- M4 [1.5/2.85]? Dimensionless m at s=4
70- 74 F5.2 --- sc/NA/kB [0.76/1.64]? Central specific entropy
76- 77 A2 --- SN Supernova type, BH or II
79- 85 F7.2 Msun Mrm [1.3/189.9]? Compact remnant mass
87- 91 F5.1 Msun Mej ? SN ejecta mass
93 I1 --- Fallback [0/1]? Flag whether SN fallback occurred
95- 99 F5.2 [Lsun] logLcc [4.76/6.93]? Stellar luminosity
at core collapse
101-105 F5.2 [K] logTeffcc [3.52/5.49]? Effective temperature
at core collapse
107-110 I4 Rsun Rstar ? Stellar radius at core collapse
112-118 F7.2 --- <Xenv>cc ? Average H mass fraction in envelope
at core collapse
120-124 F5.1 yr dtCHeB-BSG/1e5 ? Duration of core helium burning as
blue supergiant
126-130 F5.1 yr dtLBV/1e4 ? Duration inside S Doradus instability
strip in HR diagram
--------------------------------------------------------------------------------
Acknowledgements:
Fabian Schneider, fabian.schneider(at)h-its.org
(End) Patricia Vannier [CDS] 07-Mar-2024