From Z=0 to Z=0.02 Type Ia SN
Progenitors: Any influence on LCs ??
SNIa: Where we are ??
Inma Domínguez
Group of Stellar Evolution and Nucleosynthesis
Universidad de Granada
Peter Höflich, University of Texas, USA
Oscar Straniero, L. Piersanti, A. Tornambe, Osservatorio di Teramo, Italy
F. Brachwitz, F.K. Thielemann, Univ. of Basel, Switzerland
E. Bravo, UPC, Barcelona
Cosmic
Concordance
Ωm~ 0.3
Ωλ ~ 0.7
Ho = 65 km/s/Mpc
Age of the
Universe
14000 Myr
SNe at z~0.4-0.8:
0.25 mag fainter
than for an EMPTY Universe
Fainter x Further
High-z Team
SN Cosmology Project
SN Ia are NOT equal
∆MMAX ~ 3 mag
Results are based on Empirical Relations
MMAX Q LC shape
Calibrated Locally !!!
Systematic effects
MAX-LC Shape Relations
MLCS: Correlation
MMAX Q Peak width
LC:
56Ni
x 56Co x56 Fe
MMAX ∝ MNi
(Arnett 1982)
Brighter
Slower Decline
Dimmer
Faster Decline
Riess et al. , 1997
Maximum Brightness - Decline
Relation
Phillips et al. 1996, 1999
Mmax-∆m15
<σ> = 0.17 mag
∆m15
Caution: local calibrations
Correlation with host galaxy
morphology
Hamuy et al., 2000
Ivanov et al. 2000
Brighter SNIa
in Spirals Galaxies
Hamuy et al. , 1995, 1996
Branch et al. 1996
Caution !!
SNe related with
Ì Populations ??
…
but Mmax Q ∆m15
independent of galaxy
morphology
Few objects „
More observations !!
SNe Statistics
SN rate per unit Mass [10-11 M 10-2 yr x (Ho/65)2]
Galaxy
SN Ia
E-S0
0.12±0.02
S0a-Sb
0.22±0.05
S0c-Sd
0.35±0.08
Cappellaro, Barbon, Turatto 2003
SN Ia Rate
3 times y in late
Spiral Galaxies
Caution !!
Part of SN Ia
comes from
a younger population ?
Evolutionary effects ??
Stellar Population Progenitor „ Light Curve
Still … Key Problems !!
¾ Progenitors ?
MCh CO WD
companion ??
¾ Explosion Mechanism ? begin subsonic
1D parametrization of the Deflagration velocity
3D still NOT a sucessfull explosion
¾ How stellar populations evolve with z ??!!
Numerical Methods
9 STELLAR EVOLUTION:
FRANEC
(Chieffi, Cristallo, Domínguez, Imbriani, Limongi, Straniero)
1D Hydrostatic Code
¾ Extended Nuclear Network (500 isotopes)
¾ Physics and Chemestry coupled
¾ Time dependent mixing
9 EXPLOSION & LIGHT CURVES
1D Radiation-Hydrodynamic Code (PPM)
¾ Extended Nuclear Network
(Höflich, Khokhlov)
¾ γ Ray transport „ Monte Carlo
¾ 3D simulations „ velocity of deflagration
(Domínguez, Höflich)
Mch Delayed Detonations Explosions
„ LC, spectra, Mmax Q ∆M15
56Ni
…
ρtr …
Mmax Q ∆M15
ρtr : 0.8 1.0 1.2 1.4 1.6 1.8 2.0 2.3 2.5 2.7 x 107 g/cm3
ρtr … shorter pre-expansion „ ρburn …
„ 56Ni … IME (Ca, S, Si, Mg) †
Ek ≈
Dependence on the initial Z
LCs
M=5 M (1.5 „ 7 M)
Z
10-10
C/O WD 10-3
(fuel)
0.02
C/OCh MNi (M) Up to ∆MMAX =0.05 mag
0.70
0.55
No dependence of MMAX
with initial Z
0.66
0.54
Domínguez et al. 2001
0.72
0.56
Spectra at Max. (high velocities)
Fe lines
opacity
Z† κ†
Flux …
U UV B
B-V † (bluer)
∆(B-V) < 0.07
Extinction
∆MMAX < 0.2 mag
Höflich, Wheeler,Thielemann, 1998
Other results on Z...
¾ Umeda et al. (1999) & Iwamoto el al. (1999)
DO find a dependence of C/O with Z
¾ Timmes et al. (2003) confirm our results for Z< 0.02
but finds a “strong” dependence for Z>0.02 (Ni mass)
0.6
Timmes et al.
MNi
(M)
0.2
0.1 Z(Z ) 0.02

10
Röpke & Hillebrandt (2004)
in 3D simulations find
that the 56Ni mass does
not depend on C/O
• Strong mix
• Not all the WD is burnt
Dependence
on initial MMS (age)
C/O WD
LCs
MMS
1.5
5.0
7.0
Z=0.02
C/OCh MNi (M)
0.75
0.59
0.72
0.56
0.60
0.52
Up to ∆MMAX = 0.2 mag
Correlated with vph & trise
Domínguez et al. 2001
Explosive conditions
from Ì evolution
Rotation
Piersanti et al. 2003
Expected
∆MMAX < 0.2 mag
Domínguez et al. 2004
Conclusions
¾ The Majority of SNIa D STANDARD BOMBS
¾ ∆MMAX ~ 3 mag D related with population ? (obs.)
due to MNi (models)
It is already included in the Mmax-∆m15 !!!
¾ Peculiar events may be identified by the spectrum
D take good ones at high z !!
¾ Our Study about the influence of Progenitors:
MMS (age)
ρc (WD cooling, accretion)
Rotation
Z D Extinction correction
∆MMAX < 0.2 mag
∆MMAX = 0.2 mag is relevant for Ωλ ??
within
errors
Knop et al. (2003) ΩT=1 w=cte
P = wρ
ρ ∝ R −3( w+1)
Vacuum energy
Not for the
Existence !!
Sí for its
Nature (?)
∆MMAX < 0.05 - 0.1 mag