Type Ia Supernovae: Progenitor Scenarios and Observational Constraints
Keiichi Maeda (Kyoto U.)
Progenitors – which or even something else?
Double Degenerate (DD)
WD + WDSingle Degenerate (SD)
WD + MS/RG
w/o Common Envelope w/ Common Envelope
MS + MS
+ Other variants (e.g., Core-degenerate: WD + AGB)
Single Degenerate (SD)
C+O WD + MS/RG
C+O WD + He star
Sub-Ch. WD + He star- Double Detonation
(He flash on the surface of WD)
Chandrasekhar WD + MS/RG- Delayed Detonation
(C burn deep inside WD)
- Failed/Weak Deflagration
(only deflagration, no detonation)
- etc (e.g., pulsational detonation)
Ch. WD + He WD- Delayed Detonation
- Failed/Weak Deflagration
- etc.
“Delayed” (e.g., spin-up/down)
Talks in the previous session
Double Degenerate (DD)
C+O WD + He WD
Sub-Ch. WD + He WD- Double Detonation
C+O WD + C+O WD
Explosion at merging- Violent merger
(C burn on the surface of WD)
“Survive”
Talks in the previous session
ONe WD←envelope/disk- No SN explosion (NS formation)
Ch. C+O WD←envelope/disk- Delayed Detonation
- Failed/Weak Deflagration
(Theories predict ONe WD, not SN:
Saio, Yoon, Shen, …)
Viscous/Thermal evolution
(100 secs to 1000 yrs)
Expected Observables
SD DDDelayed-SD
Del-Det. MS/RG None
Weak Def. MS/RG None
Doub.-Det. He None
Violent --- None/---
SD DDDelayed-SD
CSM None(vicinity?)
SD & DD Ejecta Structure
Del-Det. Ch./Sup.-Ch. Quasi-spherical
Weak Def. Ch./Sup.-Ch. Quasi-spherical (clumpy)
Doub.-Det. Sub.-Ch. Quasi-spherical?
Violent “Sub-Ch.” for nucleosynthesis“Ch./Sup.-Ch.” for total mass
Highly Asymmetric
Companion CSM
Progenitor WD mass & Explosion
Explosion and NucleosynthesisChandra vs. Sub-Ch.
“WD density”
Stable/unstable n-rich
Fe-peaks more abundant
in Chandra WD
KM+ 10 Seitenzahl+ 13
Kromer+ 13 Fink+ 10
Tanikawa, … KM+ 15 Roepke+ 12
Many works (e.g., Khokhlov, Hoeflich, Bravo, Woosley, Kasen, Iwamoto, Nomoto, …)
Normal SNe: Companions in pre-SN/SNRs
SN 2011fe: Against RG down to ~ 1 M
SN 2014J: Against RG down to ~ 1 M
and some He donor
Li+ 2011
Kelly+ 2014
LMC SNR 0509-67.5: Against RG/MSSchafer & Pagnotta 2010
SN 1006: Against RG
Tycho: Controversial
González Hernández+ 2012
Ruiz-Lapuente+ 2004, …
So far, seems to disfavor SD for normal SNe Ia.
No Crush of the SN ejecta w/ SD companion?
Kasen 2010
(cf. Kutsuna &
Shigeyama)
V
SN Ia 2012ht Yamanaka, KM+ 2014
Zheng+ 2013
2013dy
Nugent+ 2011
2011fe
Liu, …, KM+, 2013
And very good limits by the Kepler (KEGS, red band: Olling+ 15)
Individual SNe and systematics search (e.g., SDSS-II: Hayden+ 10)
Crush of the SN ejecta w/ SD companion?
Examples with possible signatures
sub-luminous
iPTF14atg
Cao+ 2015
normal
SN2012cg Marion, … KM+ 2016
First detected for an
outlier, but then for
normal.
Observed only for a
specific direction?
MUlti-band Survey w/ the Subaru telescope for Early phase SNe Ia (MUSSES: Jiang+)
First run in Apr-June 2016.
9 early-phase SN candidates within one day.
Follow-up coordinated.
See poster by Jian Jiang (Jiang+, in prep.).
No Crush into CSM (normal SNe)RadioChomiuk+ 2012
X-rayMargutti+ 2012
Radio: Synchrotron
X-Ray: Inverse Compton (+ thermal)
Tight limit for SN 2011fe (<0.01pc):
Mdot/vw < ~10-8M
yr-1/100km s-1
Back in the history of ~ 100 day x (VSN/Vmass-loss) ~ 30 yrs
(~ 0.01 pc)
No echo by CS Environment (normal)
KM, Nozawa, Nagao, Motohara 15
2006X CSM
extinction
Symbiotic
Model (SD)
Back in the history of ~ 100 day x (C/Vmass-loss) ~ 300 yrs(~ 0.1 pc)
No CS-dust echo seen in (normal) SNe Ia.
There is little CSM (dust) at R < 0.5pc.
Not much to cause non-standard extinction
within CSM (Goobar 2008; Nagao, KM, Nozawa+ 16).
SN properties favor the delayed detonation?
Delayed-Detonation Violent Merger
Roepke+ 12
Polarization
Violent
MergerObs.
Bulla+ 16
Talks by S. Blondin, P. Hoeflich, E. Baron, ...
SN properties favor the delayed detonation?
Oxygen High velocity features (HVFs)
Outermost layer @ > 20,000 km/s
Anti-correlated w/ the Si/Ca HVFs.
Burnt (Si/Ca) / Unburnt (O) clumps?
(Not temperature/ionization/density)
Photospheric HVFs
Temperature
Zhao, KM, Wang+ 16
Follow-up on-going
work by Sai+
Chandra or sub-Chandra WD?• Chandra WD (high-ρ) produces n-rich stable/unstable Fe-peaks.
Chandra
Sub-Ch.
←Stable n-rich Fe-
peaks (e.g., 58Ni)
Unstable Fe-
peaks→
Chandra
Sub-Ch.
Chandra
Sub-Ch.
Generally favors
Chandra-WD, but
2011fe?KM+ 10
SN Remnant
Yamaguchi+ 15
Graur+ 15
Shappee+ 16
SN 2012cg
SN 2011fe
Ni/Fe
Mn/Fe
What about “outliers”
KM, Terada 2016
Maybe a mixuture of
different
evolutionary paths
and explosion
modes
Ia-CSM: Crush into CSM
SNe Ia colliding with CSM shells? (← Single degenerate)
Associated SNe are SN 1991T-like (bright SNe Ia)
Taddia+ 2012
Dilday+ 2012
Leloudas+ 2015
Poster by Regis Cartier
A Link between 91T-like and Ia-CSM
Kepler SN RemnsntKatsuda, Moti, KM+ 2015
Ejecta abundance & hist. LC
⇒SN type: bright 91T-like
CSM amount + distribution
⇒Mass loss history:
> 0.3M
@ 2pc (104-5 yrs)
91T
Ia-CSM
Kepler
~ M
0.01pc
(~ 100 – 1000 yrs)PTF 11kx
(Ia-CSM)
Over-luminous Ia (Super-Chandra WD?)
Prototypical: SN
2009dcYamanaka, Tanaka+ 2009
SN 2006gz
KM+ 2009
1.4M
2M
Bright, M(56Ni) > 1M
.
Mej > 1.4M
: “Super Chandra WD”
Two populations?
Luminous & low-vel
SNLS-03D3bb (Howell+ 06)
SN 2009dc (Yamanaka+ 09)
Not-so-luminous & high-vel
SN 2006gz (Hicken+ 07)
SN 2012dn (Chakradhari+14,
Parrent+16)
Echo by CS environment (over-luminous Ia)
Discovery of bright & Long-lasting NIR emission by OISTER ToO.
“Plateau-like evolution, ~ 1,000K thermal emission”
← As predicted for a CS echo (KM+ 2015)
⇒ More sophisticated model: geometry, etc (Nagao+, in prep.).
~ 4 10-6 M
yr-1⇒ SD for overluminous SNe?
Yamanaka, KM+ 2016 Nagao, KM, Yamanaka, in prep.
0.04pcρ∝r-2
Observer
Pure echo (obs – SN)
2012dn
2009dc
2001el
100 d
Type Iax
SN “Iax” 2012Z: He donor? He star progenitor?
SN “Iax” 2008ha: Red source (post-SN).
McCully+ 2014
Foley+ 2014
Many works (Phillips, Foley, Stritzinger, Szalai, Tomasella, Sahu,
Yamanaka, …)
Li+ 03
Jha+
07
Progenitor/companion (or compact remnant)?
Small mass & energy: Failed Deflagration?
Foley+ 13
~1.4M
~0.2-1M
Fink+ 14
Kromer+ 13
WD remnant
Eejcta
Enuc
Mej
1.4M
1.2x1051erg
Δm15
Vsi
Late-time behavior: something left?SN 2014dt by Miho Kawabata (see poster): Kawabata+, submitted
Unfortunately after the peak, but extensive late-time data
SN Iax 2014dtNIR
IRLate phase
Thermal continuum even in the late-phses.
Temperature stop evolving at ~ 60 days, when LC flattened.
Late-time LC follows 56Co-decay, full-trapping.
Non-expanding opaque component? Remnant WD?
λ
5700K@40d
3700K@>130d
50 100d
(Biased) Summary & Remarks• Diversities may reflect different paths.
– Normal SNe Ia:
• Companion/CSM favor DD, while SN properties favor Chandrasekhar WD & delayed detonation.
• But Chandrasekhar WD explosion from the DD is not yet successful in theory (ONe WD formation).
• Something must be missing (either theory or obs, or both).
– Outliers:
• Favors SD? CSM in Ia-CSM (and link to 91T) and in over-luminous SN 2012dn. Companion/remnant WD in Iax?
• Can be accommodated in evolution theory?
– SD and DD are mutually exclusive (common envelope)!