J/ApJ/886/27 SNe IIP progenitors. I. LMC giant comparison sample (Wagle+, 2019)
Type IIP supernova progenitors and their explodability.
I. Convective overshoot, blue loops, and surface composition.
Wagle G.A., Ray A., Dev A., Raghu A.
<Astrophys. J., 886, 27 (2019)>
=2019ApJ...886...27W 2019ApJ...886...27W
ADC_Keywords: Supernovae; Stars, giant; Spectral types; Extinction; Colors;
Models; Photometry, UBV; Infrared sources
Keywords: Core-collapse supernovae ; Stellar evolutionary models ;
Computational methods ; Massive stars ; Stellar convective zones ;
Type II supernovae ; Blue loop ; Supergiant stars
Abstract:
We present the evolution of massive star progenitors of supernovae of
type IIP. We take the example of the nearby and well-studied SN2013ej.
We explore how convective overshoot affects the stellar structure,
surface abundances, and effective temperature of massive stars, using
the Modules for Experiments in Stellar Astrophysics. In particular,
models with moderate overshoot (f=0.02-0.031) show the presence of
blue loops in the Hertzsprung-Russell diagram with a red to blue
excursion (log10[Teff/K] from <3.6 to >4.0) and transition back to
red, during the core helium-burning phase. Models with overshoot
outside this range of f values kept the star in the red supergiant
state throughout the post-helium-ignition phases. The surface CNO
abundance shows enrichment post-main-sequence and again around the
time when helium is exhausted in the core. These evolutionary changes
in surface CNO abundance are indistinguishable in the currently
available observations due to large observational uncertainties.
However, these observations may distinguish between the ratio of
surface nitrogen to oxygen at different evolutionary stages of the
star. We also compare the effects of convective overshoot on various
parameters related to likelihood of explosion of a star as opposed to
collapse to a black hole. These parameters are the compactness
parameter, M4, and µ4. The combination µ4xM4, and
µ4 have similar variations with f and both peak at f=0.032. We
find that all of our 13M☉ models are likely to explode.
Description:
In Section 4, we outline the method of selection of observational data
of supergiants to compare with our model calculations in the
Hertzsprung-Russell diagram (HRD) and the evolution of surface
composition.
In brief, the stars plotted in Figure 1 include red supergiant (RSG)
and yellow supergiant (YSG) candidates selected from
Neugent+ (2012, J/ApJ/749/177) and blue supergiant (BSG) candidates
selected from Urbaneja+ (2017, J/AJ/154/102).
We selected 323 YSG+RSG candidates that belong to the Large Magellanic
Cloud (LMC; labeled Category 1) and had the spectral type reported in
Neugent+ (2012, J/ApJ/749/177). We then restricted the RSG candidates
within the luminosity range 4.2<log[L/L☉]<5.1, and the YSG
candidates to the luminosity range 4.42<log[L/L☉]<4.8. The
selection finally resulted in 117 YSGs and 46 RSG candidates.
Out of the 90 BSGs reported in Urbaneja+ (2017, J/AJ/154/102), we
selected 10 BSG candidates that were in the same luminosity range used
to restrict the YSG candidates and also had log10[Teff/K]<4.5.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 181 173 Observational data of LMC supergiants for the
Hertzsprung-Russell diagram (HRD)
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See also:
J/A+AS/96/269 : Stellar Models from 0.8 to 120 Msolar (Schaller+, 1992)
J/A+A/466/277 : VLT-FLAMES survey of massive stars (Hunter+, 2007)
J/A+A/496/841 : VLT-FLAMES survey of massive stars (Hunter+, 2009)
J/MNRAS/395/1409 : Type II-P SN progenitor constraints (Smartt+, 2009)
J/A+A/545/A43 : HII regions in NGC 628 and NGC 6946 (Cedres+, 2012)
J/ApJ/749/177 : Yellow and red supergiants in the LMC (Neugent+, 2012)
J/AJ/154/102 : LMC blue supergiants spectroscopic obs. (Urbaneja+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Star name if 2MASS empty
12- 28 A17 --- 2MASS 2MASS identifier (JHHMMSSss+DDMMSSs)
30- 38 F9.6 mag Vmag [11.34/14.81]? Visual magnitude (apparent)
40- 48 F9.6 mag U-B [-0.46/0.2]? U-B color index
50- 58 F9.6 mag B-V [-0.09/2.15]? B-V color index
60- 67 F8.6 mag V-R [0.04/1.26]? V-R color index
69- 75 A7 --- SpType Spectral type from Ref
77- 84 F8.6 [K] logTeff [3.5/4.4]? Log of effective temperature
86- 93 F8.6 [Lsun] logL [4.2/5.1]? Log of luminosity
95- 102 F8.6 [K] e_logTeff [1.6/2.8]? Lower uncertainty in logTeff
104- 111 F8.6 [K] E_logTeff [1.6/2.9]? Upper uncertainty in logTeff
113- 120 F8.6 [Lsun] e_logL [3.2/3.6]? Lower uncertainty in logL
122- 129 F8.6 [Lsun] E_logL [3.2/3.6]? Upper uncertainty in logL
131- 138 F8.6 mag Av [0.13/0.96]? Extinction coefficient
140- 147 F8.6 mag e_Av [0.03/0.04]? Upper uncertainty in Av
149- 156 F8.6 mag E_Av [0.03/0.05]? Lower uncertainty in Av
158- 166 F9.6 mag BC [-2.41/-0.01]? Bolometric correction
168- 175 F8.6 mag e_BC [0.01/0.04]? (Symmetrical) uncertainty
in bolometric correction
177- 179 A3 --- Class Classification of star (according to Ref) (1)
181 A1 --- Ref Source of data (2)
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Note (1): Classification of star as follows:
BSG = blue supergiant star (10 occurrences)
RSG = red supergiant star (46 occurrences)
YSG = yellow supergiant (117 occurrences)
Note (2): Reference code as follows:
a = Urbaneja+ 2017, J/AJ/154/102
b = Neugent+ 2012, J/ApJ/749/177
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History:
From electronic version of the journal
References:
Wagle et al. Paper I. 2019ApJ...886...27W 2019ApJ...886...27W This catalog
Wagle et al. Paper II. 2020ApJ...889...86W 2020ApJ...889...86W
Wagle et al. Paper III. 2020ApJ...894..118W 2020ApJ...894..118W
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 31-Mar-2021