Issues on the evolution and properties of stripped ...
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FOE 2019 Raleigh, May 20, 2019 Issues on the evolution and properties of stripped-envelope supernova progenitors Sung-Chul yoon (SNU) With thanks to: W. Chun, Y. Jeong, H. Jin, SH Park, H.-J. Kim, L. Dessart, A. Tolstov, S. Blinnikov, A. Clocchiatti
Transcript of Issues on the evolution and properties of stripped ...
FOE�2019�������������������������������������������������������������������������������������������������������������Raleigh,�May 20,�2019
Issues on the evolution and properties of stripped-envelope supernova
progenitors
Sung-Chul yoon (SNU)
With thanks to: W. Chun, Y. Jeong, H. Jin, SH Park, H.-J. Kim, L. Dessart, A. Tolstov, S. Blinnikov, A. Clocchiatti
Ø This talk focuses on ordinary IIb, Ib and Ic supernova progenitors (ESN~ 1.0 foe; i.e., no GRB, no superluminous SNe)
Ø Most IIb, Ib and Ic SNe have an ejecta mass of 1 – 5 Msun: a binary origin? (e.g., Drout et al. 11; Taddia et al. 15, Lyman et al. 16)
Ø SN IIb progenitors:
§ Diversity in terms of the hydrogen envelope masses and radii
§ M_Henv = 0.01 ~ 0.5 Msun, R = 10 ~ 500 Rsun (e.g., Aldering et al. 94, Mound et al. 11, Folatelli et al. 15, Van Dyk et al. 11, Bersten et al. 12, Van Dyk et al. 14, Kilpartricket al. 16, Tartaglia et al. 16)
§ e.g., 2008ax (BSG) , 2011dh (YSG), 1993J (RSG)
§ Can this diversity be explained by binary systems?
Ø SN Ib and Ic progenitors:
§ What distinguishes SN Ib progenitors from SN Ic progenitors?
§ He-envelope mass?
Introduction : stripped-envelope SNe (IIb, Ib & Ic)
Massive Star Evolution: The Standard ScenarioThe dominant channel
for single stars
Mass loss plays the key role: single star models usually predict too high final masses (M > 10 Msun) of stripped-envelope SN progenitors. (e.g., Eldridge & Vink06, Georgy et al. 13)
SN IIb/Ib/Ic
SN IIb/IbUltra-stripped SN IcSuperluminous SN
neutron star
naked He core
naked He core
common envelope
NS merger,kilonova
Common envelope ejectionRed Nova
Binary StarsSingle Star
supernova (mostly type IIP)
Focus of This Talk
Primary Star Evolution in Stable Case B system
Figure from Yoon 15
Example of Binary Star Evolution of Stable Case B System
Yoon 2015
quais-WR starlike HD45166
Helium Giant like upsilon Sgr.
Stable mass transfer channel: Effects of initial orbit
Stablemasstransferifq≈1.0
Theprimarystarfills
theRoche-lobeduring
thepost-main
sequencephase.
Pinit =~100-- ~1000d
SNIb/Ic
SNIIb (e.g.,2008ax)Compactprogenitor
highZorhighM
lowZorlowM
SNIIb (e.g.,2011dh)YSGprogenitor
SNIIb (e.g.,1993J)RSGprogenitor
Hecore
COcore
Theprimarylosealargefraction
ofthehydrogenenvelope,and
becomesblue.
InitialseparationofthebinaryorbitH-envelope mass increases.
Yoon+17
effe
ct o
f mas
s lo
ss b
y w
inds
effect of initial period
Merger1989A-like SN
or SN IIn
For mass ratio of 0.9.
see also Podsiadlowski 92, Stancliffe & Eldirdige 09, Claeys 11, Benvenuto et al. 13
SN IIb progenitors on the HR diagram
Yoon+17
Blue Yellow Red
SN IIb progenitors – mass of H-rich envelope
Yoon+17
Blue
Yellow
Red
It seems that stellar evolution models can explain SN IIb diversity. But....
IIP progenitorH-env ~ 8 Msun
IIb progenitorH-env ~ 0.2 Msun:
Binding energy is positive for the most part of the H envelope:very loosely bound!
Red supergiant progenitors of different hydrogen envelope masses
What distinguishes SN Ic progenitors from SN Ib progenitors?
Classical Scenario
CO
He
CO Ib
Ic
Effect of Nickel mixing
He
CO
He
CO
IbNi
mixing into He envelope: He line formation by
non-thermal processes
IcNi
no/very weak mixing:
e.g. Dessart et al. 2012
No /very weak He lines
Ø Do SN Ib and SN Ic form a continuous sequence in terms of He contents?
Ø Can we constrain He content from SN observations?
Questions
SN Model – He-rich progenitor
SN Model – He-deficient progenitor
Light Curve
Light Curve
Light Curve
Light Curve
Light Curve
Color Evolution
Cooling by expansion Delayed effect of
nickel heating
Color Evolution
Color Evolution
Color Evolution : He-rich model
Color Evolution
Comparison
iPTF13bvn:Type Ib
à weak/moderate mixingà progenitor is likely to have a massive He envelope.
Comparison
SN 2009jf:Type Ib
à weak/modest Ni mixingà progenitor is likely to have a massive He envelope
Comparison
SN 2013ge :Type Ic(but weak signature of He lines during early times)
à strong Ni mixingà Progenitor must be He-deficient.
Comparison
SN 1994I :Type Ic
à strong Ni mixingà Progenitor must be He-deficient.
red
blue
time until optical maximum
colo
r
Monotonic reddening during the photosphericphase
red
blue
time until optical maximum
colo
r
Non-monotonic evolution during the photospheric phase
He
CO
The progenitor had a He-rich envelope. Weak/moderate mixing
of 56Ni into He envelope
He
CONi
CO
The progenitor was He-poor.
CONi
CO
Difficult to get information about the He content.
CONi
Weak/moderate mixing of 56Ni in the CO core ?
56Ni is almost fully mixed throughout the progenitor
SN 1999ex SN 2008D SN 2009jf iPTF13bvn
SN 2017ein
SN 2013ge SN 1994D
He?
Yoon et al. 2019
Ø Early color evolution of SN Ib/Ic can provide a strong constraint on Ni distribution in the SN ejecta.
Ø Evidence for more Ni mixing into the outermost layers in SN Ic than in SN Ib§ Mixing mechanism? § Asymmetric explosions, SASI, etc. § Some SNe Ic indeed have a He-deficient progenitor
Ø Evidence for relatively weak/modest Ni mixing into the He-rich envelope in SN Ib ejecta§ Mixing due to the Rayleigh-Taylor instability would depend on
the progenitor structure.
Implications
SN Ib v.s. SN Ic - Role of WR mass loss
Yoon 2017
WC stars have systematically higher Mdot , and a less steep luminosity dependence than WN stars.
Stellar evolution prediction with a revised WR mass loss rate
Yoon 2017
He mass
BolometricLuminosity
V-band Magnitude
Surface Temperature SN Ib
SN IcSN Ib
SN Ic
SN Ic
SN Ib
SN Ib
SN Ic
Ø Dichotomy in terms of He envelope mass
SN Ib iPTF13bvn (Cao et al. 2013)
SN Ic2017ein (V ~ -7) ??? (van
Dyk et al. 2018)
Ø In principle, the diversity of SNe IIb and Ib progenitors can be explained well by different initial conditions of binary systems (mass ratio, orbital period, etc) : mass-loss is the key uncertainty!
Ø There exist some observational counterparts for SN IIb/Ib progenitors in binary systems in our Galaxy (HD 45166, u-Sgr).
Ø SN Ic progenitors are not well understood yet.
Ø Some physical processes need to be better understood: mass loss, effect of rotation in binary systems, tidal interactions, common-envelope evolution, etc.
§ e.g., pre-SN eruptions? SN Ibn, LSQ14efd (see the poster by H. Jin)
Conclusions
