Modeling of SNe I b/c Shock Breakouts:
from XRO080109/SN2008D to the Future Surveys
Alexey Tolstov*, Shigehiro Nagataki*, Sergey Blinnikov(ITEP)*Astrophysical Big Bang Laboratory, RIKEN
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Supernova shock breakout (by N. Tominaga)

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Supernova shock breakout (SB) observations
SN2008D, Type Ib/c, WR candidate progenitor, Swift

SN Type II:SNLS-04D2dc

SNLS-04D2dc, Type II RSG progenitor, GALEX

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Subaru/Hyper Supreme Camera (HSC)

SN Type II:SNLS-04D2dc

Supernova remnant of Cassiopia A• The detection of transients such as shock breakoutof SNe is one of the most important missions of HSC
Interpretation of early light curves and spectra – explanation of the nature of exploding stars.
From Swift , GALEX to Subaru/HSC, PTF, LOSS, CRTS, KWFC, Skymapper, DES, Pan-STARRS, LSST.
Theoretical models are in demand!
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Ibc Presupernova Model• Evolutionary calculation ofhelium star M = 10M ʘ(Woosley et al., 1995)• STELLA provides a shock
velocity at breakout up to 0.5с(Blinnikov et al., 1998)• M = 3.199 M ʘ
R = 1.41·1011 сm
Z = 0.33, ZFe = 0.013
MNi = 0.072 M ʘRIKEN

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Numerical algorithms STELLA and RADA
STELLA (STatic Eddington-factor Low-velocity LimitApproximation) (Blinnikov et al., 1998)• 1D Lagrangian NR Hydro + Radiation Moments Equations,
VEF closure, multigroup (100-300 groups)• Opacity includes photoionization, free-free absorption, lines andelectron scattering (Blandford, Payne 1981). Ionization –Saha’s approximation• STELLA was used in modeling of many SN light curves:
SN 1987A, SN 1993J and many others (Blinnikov et al. 2006)• STELLA shows good agreement with observations in case of
SNLS-04D2dc. (Tominaga et al. 2009, 2011)t δR= t diff :For Ib/c model STELLA is not accurate!
RADA (fully Relativistic rADiative transfer Approximation)(Tolstov, Blinnikov, 2003)• 1D Relativistic Radiative Transfer in comoving frame (McCrea &Mitra 1936, Mihalas, 1980)l – photon mean free pathδR - the distance from the shock to thephotosphereD – shock front velocity• Relativistic transformation of fluxes from the source to the observerRIKEN

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Comoving radiation transfer (Mihalas, 1980)
Transfer equation:

Moments equation:

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SRRHD. Radiation-dominated mildly-relativistic shock wave
Semi-analytic relativistic hydro +Relativistic radiation transfer(no closure condition)

Shock tube configuration(Farris et al., 2008), Pr/Pg ≈ 10

Closure condition: P = fE
• Eddington approximation: f = 1/3• M1-closure (Levermore, 1984)
f = f(E,F) joins “optically thin”
and “thick” cases• Photon Boltzmann equation

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88Transformation of fluxes from source to observer’s frame
Lorentz covariance, Doppler effect and aberration•••

Radiation flux increases
Spectrum becomes harder
The space shrinks towards the direction of motion

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V = 0.5 cГ = 1010/31/2013

Г = 10099

SN Ibc shock breakout modeling (Tolstov et al. 2013)
Explosion energy = 1.8 foe,
Shock velocity at shock breakout ≈ 0.5с•Radiation Transfer – Short Characteristic Method(about 90% of calculation time)•Radius х Angle x Energy = 350 * 100 * 200 == 7 000 000 for 1 time step•

200 steps of RADA , 10000 steps of STELLA,
3 days of calculation

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XRO080109/SN2008D in the Model of SNIb
How to explain the duration and spectrum of the outburst?
External medium is optically thin to affect the radiation(Chevalier, Roger A., Fransson, Claes, 2008, ApJ, 683L, 135C)

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XRO080109/SN2008D in the Model of SNIb with the Stellar Wind
Can we explain the observational data by ‘natural’ model (WR star + wind)?
1.
2.

The growth of photosphere before the shock front
Changes in absorption/emission of the perturbed wind

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XRO080109/SN2008D Spectra and Light Curves• X-Ray light curves and spectra, averaged over the duration of the flash,of XRO 080109 in Swift/XRT band (0.3-10 keV) for 10A presupernova model• No extinction

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XRO080109/SN2008D Spectra and Light Curves (extinction)• X-Ray light curves and spectra, averaged over the duration of the flash,of XRO 080109 in Swift/XRT band (0.3-10 keV) for 10A presupernova model• NH = 22 × 1021 cm−2, XRT response• EK = 262.5 foe (Tanaka et al. 2009) in modeling of SN2008D light curve
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XRO 080109 Spectral Evolution

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Objectives• Analyses, prediction and interpretation of data of Subaru
Hyper-Suprime Cam (HSC) using SB templates for SN type Ib/c
New serveys: Palomar Transient Factory (PTF), Lick Observatory
Supernova Search (LOSS), Catalina Real-Time Transient Survey(CRTS), Kiso/Kiso Wide Field Camera (KWFC), Skymapper, Dark
Energy Survey (DES), Pan-STARRS, Subaru/HSC, Large Synoptic
Survey Telescope (LSST)• Research and development of new and effective numericalmethods for calculating the radiation of relativistic gas dynamics• Numerical Improvements in SRRHD code:• Relativistic radiation hydrodynamics in 1D• Relativistic radiation hydrodynamics in 2D-3D• Scattering processes and radiation mechanisms

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SN Ibc Shock Breakout at High Redshift

PRELIMINARY RESULTS• Cosmological parameters(Komatsu et al. 2009):
H0 = 70.5 km s−1 Mpc−1
k=0Ωλ = 0.726
ΩM = 0.274• Dilated and redshifted multigroup
LCs with the g bandpass of theSubaru/HSC• The horizontal line − 5σ detection
limit in the g-band for theSubaru/HSC 1 hr integration• No extinction and no IGM
absorption

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Conclusions• The phenomenon of XRO080109/SN2008D may well be explained
qualitatively by the explosion of a conventional WR-star surrounded
by a stellar wind. The explosion energy > 3 foe. Previous analytic
estimations do not take into account the growth of the photosphereaccurately• SN2008D light curve must be modeled for the optimal model• For the accurate consideration of mildy relativistic radiation
dominated shock waves it is necessary to solve radiation transfer
equation (Eddington and M1 closure are not good approximations)• Our numerical calculations provides us the opportunity to build
robust templates for the analysis and interpretation of the SN Ibc
observations that will be received by Subaru/Hyper-Suprime Cam(HSC) and a number of others surveys

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Thank you!
E-mail: alexey.tolstov@riken.jp
10/31/2013

Additional Slides

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Optical data(Page K.L. et al. GCN Report 110.1 15 Jan 2008), E = 2.5 foe

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SN2008D light curve modeling, E=2 foe

Tanaka M. et al., 2009, Bersten M. 2013

STELLA
STELLA+RADA
SN2008 data

Density modulations of circumstellar medium
OR

Chemical composition of the progenitorOR

Jet geometry

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