Comparing Hydrodynamic Models with Observations of Type II … · 2011. 2. 2. · SNII-P Light...
Transcript of Comparing Hydrodynamic Models with Observations of Type II … · 2011. 2. 2. · SNII-P Light...
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Comparing Hydrodynamic Modelswith Observations of Type II Plateau
Supernovae
Melina Cecilia Bersten
IPMU, 2011 February 1st
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Outline
Introduction
Hydrodynamical Code
Data Sample: Bolometric Corrections
Analysis of our Sample of SNe II-P
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Supernovae
Kinetic energy: ∼ 1051 erg = 1 foe = 1 B
Radiated energy: 1-10% Ek during weeks/months (∼ 1010L⊙)
Velocities: vexp ∼ 104 km s−1 ⇒ ∼ 105 R⊙ (few weeks)
Temperature: ∼ T⊙ ⇒ R = (L/L⊙)1/2 R⊙ ∼ 105 R⊙ (few weeks)
CSP supernovae SN 1987A
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Supernova Classification
light curveIIb IILIIP
IIn
ejecta−CSMinteraction
core collapsethermonuclear
yes
yesno
no
noSiIIHeI yes
hypernovae
strong
shape
Ia IcIb
Ib/c pec
III H
Turatto (2003)
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Type II-P Supernovae
Spectroscopy: prominent P-Cygni Balmer lines
Photometry: long plateau phase (L ∼ const. for ∼100 days)
Spectropolarimetry: explosion approximately spherical
Most common type of SN (59% of CCSNe)
Courtesy CSPSNII-P Light Curves – p.5/39
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Type II-P Supernovae
Good distance indicators
Expanding photospheric method (EPM )
Spectral fitting expanding atmosphere method (SEAM)
Standard candle method (SCM)
Connection with final stages of stellar evolution
⇓Physical properties of the progenitor
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SN II-P ProgenitorsWide range of plateau luminosity (Lp), plateau durations (∆tp) andexpansion velocities (vp)=⇒ Different progenitors properties
Light curve + spectral modelling =⇒ Mej, R , Eexp and MNi
Pre-supernova imaging + stellar evolution models =⇒ MZAMS
Litvinova & Nadezhin 1983 Smartt et al. 2009SNII-P Light Curves – p.7/39
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Type II-P Supernovae
Good distance indicators: EPM, SEAM and SCM
Connection with final stages of stellar evolution
Physical properties of the progenitor:
Red supergiant structure with H-rich envelope (Van Dyk et al. 2003)
Stellar evolution: MZAMS: 8 – 25 M⊙ (Heger et al. 2007)
Pre-SN imaging: MZAMS: 8 – 17 M⊙ (Smartt et al. 2009)
Hydrodynamical modelling favors high mass range(Utrobin & Chugai 2008)
Availability of a large of SN II-P
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Sample of SNe II-P∼30 nearby SNe II-P: Calán/Tololo, SOIRS and CATS(1986-2003)
High-quality, well-sampled BV RI light curves and spectra
The CSP is providing even more objects (∼ 80 SNe II-P)
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Type II-P Supernovae
Good distance indicators: EPM, SEAM and SCM
Connection with final stages of stellar evolution
Physical properties of the progenitor:
Red supergiant structure with H-rich envelope (Van Dyk et al. 2003)
Stellar evolution: MZAMS: 8 – 25 M⊙ (Heger et al. 2007)
Pre-SN imaging: MZAMS: 8 – 17 M⊙ (Smartt et al. 2009)
Hydrodynamical modelling favors high mass range(Utrobin & Chugai 2008)
Availability of a large data of SN II-P
Development of our own code to compare with our database of SNe II-P
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Code
Theoretical model of LC =⇒ numerical integration of the hydrodynamicequations + radiative transfer
Assumptions:
Spherically symmetric explosion =⇒ One-dimensional code
Diffusion approximation with flux-limited prescription
Computation of shock wave using an artificial viscosity term
Explosion simulated by a sudden release of energy near the core
Energy released by radioactive decay
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Equations
V = 4π3
∂r3
∂m=⇒ Mass conservation
∂r
∂t= u =⇒ Velocity
∂u
∂t= −4πr2 ∂
∂m(P + q)− Gm
r2=⇒ Momentum conservation
∂E
∂t= ǫNi −
∂L
∂m− (P + q) ∂V
∂t=⇒ Energy conservation
L = −(4πr2)2 λ ac
3κ∂T 4
∂m=⇒ Radiative energy transport
+
Initial and boundary conditions, and constituent equations
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Code
Method of finite differences: space-time grid
Explicit scheme for the hydrodynamics (∆t ≤ tCourant) andimplicit for the temperature
Gamma-ray deposition from 56Ni–56Co–56Fe decay
transfer equation in grey approximation: dIdτ
= −I + S
arbitrary spherically symetric distribution of 56Ni
dEdm
= κγ∫
IdΩ; κγ = 0.03 cm2 g−1
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Initial modelsPolytropic models: single and double
Evolutionary calculations
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Initial modelsPolytropic models: single and double
Evolutionary calculations
Double Polytrope
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Initial modelsPolytropic models: single and double
Evolutionary calculations
Evolutionary models
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RESULTS
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Theoretical Bolometric LCModel with E = 1.3 foes, R0 = 800 R⊙, M0 = 19 M⊙
Evolutionary phases
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Before breakoutModel with E = 1.3 foes, R0 = 800 R⊙, M0 = 19 M⊙
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Before breakoutModel with E = 1.3 foes, R0 = 800 R⊙, M0 = 19 M⊙
Velocity profiles at different times
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After breakoutModel with E = 1.3 foes, R0 = 800 R⊙, M0 = 19 M⊙
Profiles of the fraction of ionized Hydrogen
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After breakoutModel with E = 1.3 foes, R0 = 800 R⊙, M0 = 19 M⊙
Temperature profiles
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Variation of Parameters
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Variation of ParametersLight curves for different energies
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Variation of ParametersLight curves for different radii
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Variation of ParametersLight curves for different masses
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Variation of ParametersLight curves for different 56Ni mass
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Variation of ParametersLight curves for different 56Ni distribution
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DATA SAMPLE
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Bolometric Correction
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Bolometric Correction
Three well-observed supernovae:SN 1987A, SN 1999em, and SN 2003hn
Integration of all the availablebroadband data
Estimation of the missing flux inUV and IR: blackbody (BB) fit
Calculation of BC for two atmospheremodels: Eastman et al. (1996) andDessart & Hillier (2005)
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Bolometric CorrectionBC = mbol − [V − AV ], rms = 0.11 mag
Bersten & Hamuy (2009)
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Sample of SNe II-P
Calculation of bolometric LCs for our sample of SNe II-P
logL[erg s−1] = −0.4 [BC(color) + V − Atotal(V )− 11.64] + log(4πD2)
Olivares et. al (2010): D, Ahost(V )
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Sample of SNe II-PCalculation of bolometric LCs for our sample of SNe II-P
Estimation of parameters to characterize the LCs:
Lp: plateau luminosity
∆tp: plateau duration
∆ log L: luminosity drop
MNi: 56Ni mass
Analysis of observed parameters
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Slope during PlateauBi-modal tendency
slope > −1 mag/100 d −→ “normal plateau”
slope < −1.25 mag/100 d −→ “intermediate-plateau”
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Bolometric Luminosity RangeWeighted average 〈Lp〉 = 1.26× 1042 erg s−1
Range of 1.15 dex in LpSN 1992amSN 2003hgSN 1999emSN 1992baSN 2005csSN 1999br
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56Ni massMNi sensitive to adopted explosion time
Assumed local deposition of gamma rays
Weighted average 〈MNi〉 = 0.024M⊙
MNi < 0.1M⊙,except for SN 1992am (MNi > 0.26M⊙)
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Model vs. Observation
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Hydro-Model of SN 1999em
Proto-type SN II-P
One of the best-oberved SNe II-P
Determination of physical parameters(M0,R0, E and MNi) by comparing
bolometric light curve
photospheric velocity evolution
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Hydro-Model of SN 1999emExtended 56Ni mixing
Very good agreement with observations
Physical parameters similar to previous hydrodynamical studies(Baklanov et al. 2005; Utrobin 2007)
Low-mass models are not favored
Bersten, Benvenuto & Hamuy, ApJ in press
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Grid of Hydrodynamical Models
Set of 46 hydrodynamical models:
M0 = 10, 15, 20 and 25 M⊙
E = 0.5, 1, 2 and 3 foeR0 = 500, 1000, and 1500 R⊙
MNi = 0.02, 0.04 and 0.07 M⊙
For each model: Lp, ∆tp ,∆L, MNi and v−30 are measuredconsistently with observations
Dependence of observable parameters on physicalquantitiesStudy of correlations between observable parameters
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Model dependencesSymbols: size proportional to M0, shape indicates different R0 andcolors related with MNi (fixed mixing)
Plateau luminosity
Strong correlation withexplosion energy
∼0.4 dex of dispersionmainly related toM0 and R0
MNi (fixed mixing) isnot very influential
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Model dependencesSymbols: size proportional to M0, shape indicates different R0 andcolors related with MNi (fixed mixing)
Plateau duration
Weaker correlation withexplosion energy
M0 seems the mostimportant factor but MNi
also produces an effect
R0 produces a minor effect
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Observed and Modeled Correlations
The Standard Candle Method (SCM):
Correlation between luminosity and expansion velocityduring the plateau phase found by Hamuy & Pinto(2002)
Detailed study of this correlation for our sample ofSNe II-P given by Olivares et. al (2010) leading to aprecision of 13% in distance
Study of this correlation using our hydrodynamicalmodels
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Observed and Modeled CorrelationsSymbol Colors: different explosion energies (E)
SCM
Models reproduce very wellthe obverved trend
E is the main driver
Shift between modelsand observations
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Observed and Modeled CorrelationsSymbol Colors: different explosion energies (E)
SCMShift between modelsand observations:
Adopted H0
Extinction correction
Measurementinconsistencies
High-mass models
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Observed and Modeled CorrelationsSymbol Colors: different explosion energies (E)
Models showslight correlationpreviously noted byKasen & Woosley (2009)
Observations showno correlation
Lowest E and high M
are not favored
SNII-P Light Curves – p.31/39
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Kasen& Woosley 2009
Grid hydro Models using pre-SN models from stellar evolutionarycalculations: E=0.5-4 foe, M= 10.9-15.8 M⊙ and R= 625-1349 R⊙
80 100 120 140 160 180 200Plateau duration (Mni = 0
-15
-16
-17
-18
-19
-20
V-b
and
abso
lute
mag
nitu
de (
day
50)
0.55 0.60 0.65 0.70
-0.4
-0.2
0.0
0.2
0.4
0.6
Strong correlation
MV,50 = −18.4− 0.03[tp,0 − 100]
Correction by 56Ni massis needed
tp = tp,0 ×(
1 + 0.35MniE−1/251 R
−10 M
1/2ej
)1/6
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Observed and Modeled CorrelationsSymbol Colors: different explosion energies (E)
Models showslight correlationpreviously noted byKasen & Woosley (2009)
Observations showno correlation
Lowest E and high M
are not favored
SNII-P Light Curves – p.33/39
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SummaryWe implemented a robust method to estimate BC from BV I photometryfor SNe II-P with typical scatter of ∼0.1 mag
We studied SN 1999em in detail obtaining a very good agreement withobservations when extended mixing of 56Ni is used
We calculated a set of observable parameters (Lp, ∆tp, ∆L and MNi) forour data sample and for a grid of hydrodynamical models:
Parameter distribution:Bi-modal tendency of the slope during plateau1.15-dex range in plateau luminositiesMNi < 0.1M⊙, except for SN 1992am with MNi > 0.26M⊙
Dependence on physical quantities (E, R0, M0 and MNi)
Correlations using models and observationsModels confirm the SCM relationLowest E and high M are not favored
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Plateau LengthsWeighted average 〈∆tp〉 = 90.47 days
Most SNe with 〈∆tp〉 between 75 and 105 days
Bi-modal trend in the distribution (secondary peak at ∼60 days)
SN 2003bnSN 1999giSN 1999emSN 2003hn
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Luminosity drop: ∆ log LWeighted average 〈∆logL〉 = 0.783 dex
Range of 0.35–1.46 dex in ∆ log L
SN 1992ba
SN 1999em
SN 2003hn
SN 1999gi
SN 1992af
SN 2003gd
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Model dependencesSymbols: size proportional to M0, shape indicates different R0 andcolors related with MNi (fixed mixing)
Luminosity drop
Some dependence onexplosion energy
Strong correlationwith MNi
Some dependence onR0 but not on M0
SNII-P Light Curves – p.37/39
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Model dependencesSymbols: size proportional to M0, shape indicates different R0 andcolors related with MNi (fixed mixing)
Expansion velocity
Strong correlation withexplosion energy
M0 is the main driverof the dispersion
Slight dependence onMNi but not on R0
SNII-P Light Curves – p.37/39
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Observed and Modeled CorrelationsSymbol Colors: different explosion energies (E)
No correlation
Ni mass affects tailluminosity but not theplateau
SNII-P Light Curves – p.38/39
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Comparison with STELLA CodeSTELLA code (Blinnikov et al. 1998):
implicit hydrodynamics + multi-group radiative transfer
includes the effect of the line opacities
STELLA calculations by N. Tominaga
SNII-P Light Curves – p.39/39