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)!