J/A+A/708/A136 Effective supernova dust yield (Otaki+, 2026)
Effective supernova dust yields from rotating and non-rotating
stellar progenitors.
Otaki K., Schneider R., Graziani L., Bonella A., Marassi S., Limongi M.,
Bianchi S.
<Astron. Astrophys. 708, A136 (2026)>
=2026A&A...708A.136O 2026A&A...708A.136O (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Stars, masses ; Models
Keywords: supernovae: general - ISM: abundances - dust, extinction -
galaxies: high-redshift
Abstract:
Supernovae (SNe) are believed to be the dominant sources of dust
production at high redshift. However, the reverse shock generated by
the interaction of the SN forward shock and the interstellar medium
(ISM) can significantly reduce the mass of newly formed dust in SN
ejecta. This study quantifies the mass, composition, and grain size
distribution of surviving dust after the passage of the reverse shock
using the GRASHrev model. Our analysis covers a grid of SN models with
progenitor masses 13M☉≤mstar≤120M☉, metallicity
-3≤[Fe/H]=0, and explores, for the first time, the effect of stellar
rotation, considering two initial velocities v=0 and 300km/s. The SN
explosions are assumed to occur in a uniform ISM with densities
nISM=0.05, 0.5, and 5cm-3. We find that the larger grains (≥10nm)
are more resistant to destruction by the reverse shock, with amorphous
carbon dominating the surviving dust mass in most models. The
surviving dust mass decreases with increasing ISM density. For
non-rotating progenitors, the maximum mass of dust surviving the
passage of the reverse shock is ∼0.02M☉ released by SN
explosions of a 120 Msun progenitor with [Fe/H]=0 in the ISM density
0.5cm-3, corresponding to ∼4% of the initial dust mass before the
passage of the reverse shock. Similarly, among the rotating
progenitors, a maximum surviving mass fraction is ∼5% with a final
dust mass ∼0.03M☉ in [Fe/H]=-1 models. Although the reverse
shock has a strong destructive impact, our results indicate that, on
very short timescales of <30Myr since the onset of star formation,
SNe can enrich the ISM with carbonaceous grains ranging in size from
approximately 1nm to 100nm (up to ∼1um in non-rotating models).
This is especially notable given the recent detection of the 2175Å
UV extinction bump in galaxies at z>6, suggesting the early presence
of such dust.
Description:
We present the initial (before the passage of the reverse shock) and
effective (after the passage of the reverse shock) dust yields for all
grain species in each supernova model. All dust yields smaller than
1E-6 solMass are set to zero.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 97 28 Initial dust yields for non-rotating models
tablea2.dat 97 32 Initial dust yields for rotating models
tablea3.dat 103 27 Effective dust yields for non-rotating models
with [Fe/H] = 0
tablea4.dat 103 24 Effective dust yields for non-rotating models
with [Fe/H] = -1
tablea5.dat 103 18 Effective dust yields for non-rotating models
with [Fe/H] = -2
tablea6.dat 103 15 Effective dust yields for non-rotating models
with [Fe/H] = -3
tablea7.dat 103 27 Effective dust yields for rotating models
with [Fe/H] = 0
tablea8.dat 103 27 Effective dust yields for rotating models
with [Fe/H] = -1
tablea9.dat 103 21 Effective dust yields for rotating models
with [Fe/H] = -2
tablea10.dat 103 21 Effective dust yields for rotating models
with [Fe/H] = -3
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Byte-by-byte Description of file: tablea1.dat tablea2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- [Fe/H] [-3/0] Initial metallicity
5- 7 I3 Msun Mstar Progenitor mass (13/15/20/25/30/40/60/80/120)
10- 17 E8.2 Msun Mdust Total dust mass
20- 27 E8.2 Msun MAl2O3 Al2O3 mass
30- 37 E8.2 Msun MFe Fe mass
40- 47 E8.2 Msun MFe3O4 Fe3O4 mass
50- 57 E8.2 Msun MMgSiO3 MgSiO3 mass
60- 67 E8.2 Msun MMg2SiO4 Mg2SiO4 mass
70- 77 E8.2 Msun MAC AC mass
80- 87 E8.2 Msun MSiO2 SiO2 mass
90- 97 E8.2 --- mu Mean molecular weight
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Byte-by-byte Description of file: tablea[3456789].dat tablea10.dat
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Bytes Format Units Label Explanations
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1- 3 I3 Msun Mstar Progenitor mass (13/15/20/25/30/40/60/80/120)
6- 13 E8.2 Msun Mdust Total dust mass
16- 23 E8.2 Msun MAl2O3 Al2O3 mass
26- 33 E8.2 Msun MFe Fe mass
36- 43 E8.2 Msun MFe3O4 Fe3O4 mass
46- 53 E8.2 Msun MMgSiO3 MgSiO3 mass
56- 63 E8.2 Msun MMg2SiO4 Mg2SiO4 mass
66- 73 E8.2 Msun MAC AC mass
76- 83 E8.2 Msun MSiO2 SiO2 mass
86- 93 E8.2 % eta Surviving dust mass fraction
96-103 E8.2 cm-3 nISM Interstellar medium density
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Acknowledgements:
Koki Otaki, koki.otaki(at)uniroma1.it
(End) Patricia Vannier [CDS] 09-Feb-2026