supernova Ia progenitors overview of light curves and spectra - - PowerPoint PPT Presentation

▶
supernova ia progenitors overview of light curves and
SMART_READER_LITE
LIVE PREVIEW

supernova Ia progenitors overview of light curves and spectra - - PowerPoint PPT Presentation

Dec 10, 2022 221 likes •542 views

supernova Ia progenitors overview of light curves and spectra daniel kasen zeroth order SNIa model explosion ejecta progenitor t ~ secs IME ? 56Ni C/O IME C/O need to examine subtleties spectra (line features, asymmetry, CSM) light

slide-1
SLIDE 1

supernova Ia progenitors

  • verview of light curves and spectra

daniel kasen

slide-2
SLIDE 2

C/O

IME

C/O

56Ni

IME

explosion

t ~ secs

progenitor ejecta

zeroth order SNIa model

? spectra light curves

need to examine subtleties (line features, asymmetry, CSM) compare to imperfect models, get mixed messages

slide-3
SLIDE 3

Mch model (central or off-center ignition) C/O WD + H star

merger/collision of two C/O white dwarfs sub-Mch model (double detonation) C/O WD + He star or WD

C/O

He

variety of progenitors/explosions

slide-4
SLIDE 4

Mch delayed detonation models

  • ff-center ignition

central ignition

slide-5
SLIDE 5

delayed detonation models

kasen+ 2009 roepke+ 2012

hoeflich&Khokhlov 1995.6, nugent 1994, pinto&eastman 2000 kasen+ 2009, roepke+ 2012, sim+2013, dessart+ 2014

slide-6
SLIDE 6

delayed detonation models good fit to observed spectra/lightcurves

slide-7
SLIDE 7
  • ff-center ignition

(GCD-like model)

kasen & Plewa 2007 foley & kasen (2011)

lopsided ejecta

variations in Fe-group blanketing affect the UV brightness

56Ni IME

slide-8
SLIDE 8

silicon velocity as a function of viewing angle

Benetti et al (2005)

c.f. maeda+ 2011

slide-9
SLIDE 9

companion interaction and early light curves

supernova companion

slide-10
SLIDE 10
slide-11
SLIDE 11

kutsuna & shigeyama, 2015 RGB companion

different viewing angles

kasen 2010

companion shock signatures

Cao et al (2015) ~20 Rsun Marion et al (2015) ~10 Rsun Shappee (2015) no detection Olling et al (2015) no detection Nugent el al (2015) no detection Bianco et al (2010) no detection Hayden et al (2010) no detection Brown et al (2011) no detection

slide-12
SLIDE 12

shappee+ 2013

No sign of stripped hydrogen in spectra

but how robust our the theory predictions?

slide-13
SLIDE 13

Ni/Fe/Cr/Ti/Ca

Si/S/Ca

56Ni

sub-chandrasekhar explosions (double-detonation)

Nomoto+ 1980, Woosley+ 1980, Livne 1990 Woosley&Weaver 1994, Livne&Arnett 1994, Bildsten+ 2007,Fink+ 2007, Sim+ 2010, Kromer+ 2010 Woosley&Kasen 2011

He

C/O

slide-14
SLIDE 14

double detonation spectra (at maximum)

varying helium shell masses (woosley and kasen 2011)

acc

slide-15
SLIDE 15

spectral evolution

double detonation

Mcore = 0.90 Msun Mshell = 0.12 Msun

black: with burned shell red: without burned shell

slide-16
SLIDE 16

broadband light curves

solid (with shell), dashed (no shell), dots (SN2003du)

double detonation

Mcore = 0.90 Msun Mshell = 0.12 Msun

slide-17
SLIDE 17

sub-chandrasekhar model width luminosity relation

shell only core+shell core + lowmass shell

1D models

c.f. sim+2010

slide-18
SLIDE 18
  • 1.2

0.0 1.2 Residual (1042 erg s−1) 0.0 0.6 1.2 1.8 L (1043 erg s−1)

Us Scalzo+14 MNi (M) 0.55 0.56+0.12

0.12

RNi (M) 0.78 — MIME (M) 0.56 — MCO (M) 0.06 — κ (cm2 g1) 0.10 — MEj (M) 1.17 1.01+0.09

0.07

SNF20060907-000

Best Fit w/Emulator SNFactory Data Emulator 68% CI

fits to observed SNF light curves

physical parameter estimation (danny goldstein, UCB)

slide-19
SLIDE 19

CaII

blue: M = 1 Msun red: M = 1.26 black : sn201llfe Lack of stable iron group elements in nebular spectra?

Mazzali et al 2015

slide-20
SLIDE 20

double white dwarf mergers as SNe Ia

“prompt” (violent) detonation

  • r collision

both stars explode

e.g. pakmor et al (2010) raskin+2009, rosswog+2009

“late” detonation

secondary shredded to disk (“tamped” SNe Ia)

e.g., hoeflich and kokhlov (1996) raskin+2014

“double” detonation

He shell explodes during mass transfer; secondary remains intact?

e.g. guillochon et al (2010)

slide-21
SLIDE 21

moll, raskin, kasen, woosley (2014) raskin, kasen, moll, schwab, woosley (2014)

prompt detonation calculation (CASTRO code)

slide-22
SLIDE 22

raskin and kasen (2013) moll, raskin, kasen, woosley (2014)

slide-23
SLIDE 23

` 28Si 56Ni

white dwarf mergers as SNeIa

compositional structure of prompt explosions

(azimuthal averages)

16O moll, raskin, kasen, woosley (2014)

slide-24
SLIDE 24

violent white dwarf merger

viewing angle dependence 0.9 x 0.81 max light spectrum

(phi averaged)

slide-25
SLIDE 25

white dwarf mergers as SNeIa prompt explosion comparison to

  • bserved spectra

moll, raskin, kasen, woosley (2014) raskin, kasen, et al (2014) c.f. roepke et al (2012)

slide-26
SLIDE 26

prompt explosions of C/O WD mergers

synthetic B-band light curves

moll, raskin, kasen, woosley (2014)

slide-27
SLIDE 27

carbon features near maximum

CII SiII

1.2 x 1.06 merger (~0.1 Msun of carbon)

slide-28
SLIDE 28

asymmetry and polarization

normal SNIa show low continuum polarization <~ 0.3% (higher in SN1991bg-like ~ 0.6%) (higher polarization in lines ~1-2%)

  • ff-center Mch

violent merger head on collision

slide-29
SLIDE 29

continuum polarization curves

3-D models: pure e- scattering, inclination = 90o

kasen+ in prep

slide-30
SLIDE 30

Felicitous agreement with observed light curves/spectra (even the effects of asymmetry), tension with other indicators (e.g., no companion/CSM interaction). Can they contribute at a significant rate?

Mch models

Can we ignite and propagate detonation in low shell masses (< 0.01 Msun) or in a WD merger leadup? Do we need (can we get) stable iron group?

sub-Mch models merger/collision models

Is the high-degree of asymmetry a deal breaker? Are these (just) the “super-Chandrasekhar” events?