冨永望 (甲南大学)
Sergei Blinnikov (ITEP/IPMU)
2011年12月27日「超新星爆発と数値シミュレーション」
C: A. de Ugarte Postigo (ESO) et al.

What is shock breakout?
Multigroup radiation hydrodynamics
Application for shock breakout
Proposal of future SN survey

Massive Star (>10M8)

e--capture SNe (8-10M8)

HHeC
O

Si
NS/BH
Fe

SNIc

SNIb

SNII

Temp Burning Products
8[10 K] Stage
0.2
H
He
1.5
HeC,O
7CNe,Mg
15NeO,Mg
30OSi40
SiCr,Mn5650NSE
Ni

Core collapse driven byFe photodisociation
NS/BH formation
Energy deposition

Opticallythick

Massive Star (>10M8)
e--capture SNe (8-10M8)

At the shock emergence,a stored energy is released
as radiation.

Luminosity

Core collapse

Spectra are quasi-blackbody
T ~ R-3/4E1/4

Spectra peaked at X-ray-UV.
It lasts a few sec- a few day.

TimeIt is theoretically predicted
in 1970s but observationally
first reported in 2008.

衝撃波後方は輻射優勢

光学的厚さが厚いため物質の衝撃波と輻射の衝撃波が同じ位置に存在衝撃波の速度 < 光子のdiffusion速度
 vs ≲ c/t• 衝撃波からの光子で衝撃波の上流の加熱• 衝撃波の鈍りMatzner & McKee 1999
– The Expulsion of Stellar Envelopes in Core-Collapse Supernovae



Waxman + 2007
– GRB 060218: A Relativistic Supernova Shock Breakout

Li 2007– Shock breakout in Type Ibc supernovae and application to GRB060218/SN 2006aj

Chevalier & Fransson 2008
– Shock Breakout Emission from a Type Ib/c Supernova: XRT080109/SN 2008D



Nakar & Sari 2010
– Early Supernovae Light Curves Following the Shock Breakout



Sapir + 2011
– Non-relativistic Radiation-mediated Shock Breakouts. I. Exact
Bolometric Planar Breakout Solutions

1978年 Klein & Chevalier によって提案された
1-2日以下の物理現象 Radiation hydrodynamics
– 流体と輻射輸送が相互作用⇔超新星光度曲線:流体は大体homologous (r∝v)
Radiative precursor– 異なる輻射の温度とガスの温度– (最低でも2温度の) Radiation hydrodynamics→方程式は Mihalas & Mihalas (1984)
概念は Zel’dovich & Raizer (1966)

Light curve (SN1987A[青色巨星]の場合)

Temperature structure
Radiativeprecursor

Photosphere星表面Trad>Tgas

Optically thinに近づくとradiative transportが重要に

1.2x10-5M8



Luminosity structure“Shock front”

増光Velocity structure“Shock front”

Shockがphotosphereを通過
Preacceleration

ガスの温度・圧力上昇によって加速

Multigroup radiation hydrodynamics code
Spherical symmetry with Lagrangean coordinate
Implicit methods on rad. transfer & hydrodynamics
Non-equlibrium radiation transfer– Moment equations– Closure relation: Variable Eddington factorLTE level population (Saha-Boltzmann eq.)
– 15 most abundant elements (H-Ni)

Opacity– f-f, b-f, 1.5x105 spectral lines, electron scatteringEnergy deposition from radioactive decay– 1-group grey radiative transfer球対称、comoving flame、O(v/c) とすると、In

Mihalas & Mihalas (1984)

Invariant photon distribution function

Angler moments of fnMonochromatic rad. energy eq.

Monochromatic rad. momentum eq.

Hydrodynamical eqs.

Radiative acceleration



EOS for material temperature(Closure relation– Variable Eddington factorBoundary condition– Outer boundary: p=0 &– Inner boundary: diffusion approximation)

In 1 time step, the following procedures areiterated to convergence.
jmn derived by a formal solution with Sn– Feautrier methodfE, hE calculated with jmn
Radiation hydrodynamics eq. solved with fE, hE– Jn, Hn, r, T, v

Sn estimated with new Jnf-f, b-f
Karp+77; Eastman & Pinto 93A supernova is a fast-expanding media.
Doppler shift should be included.
Effective opacity as a function of T, r, dv/dr
Effective line opacity in (n, n+Dn)= ave. num. of interaction(~S(1-e-t))/distance(~ctDn/n)– single scattering assumption scattering, b-b (# of bin=1000)

Q =dln(v)/dln(r) - 1 (~ 0, in SN)
tj: Sobolev optical depth of line jb-b (# of bin=100)
Sj: sum of linesscattering,in (n, n+Dn)

Type II Supernova

Short duration(a few sec-1day)

Light curve
Shock Breakout
Peak wavelength
Soft X-ray-UV
30M8, Z=0.02, E51=1
Extremely bright (L>1044erg/s)

BolometricV-bandPlateauTailFor larger radius,
longer duration,higher total energy, andlower temperature(i.e., redder color).

Adopting Tana/1.5, tana/2, Eana/3, Lana/1.5,
analytical and numerical solutions are consistent (NT+11).

Type II-peculiar SN1987A
ModelObs.

Catchpole + 87
Hamuy + 88
Blinnikov + 00

Type IIb SN1993J

Type Ib SN1999ex

Obs.

Richmond+96

Stritzinger + 01

近傍の超新星でのみ、偶然見つかることがある。

Type Ib SN2008D/XRO080109– Soderberg + 08; Modjaz + 09

Swift

There are 2 Type II-P SNe.
GALEX



Type II-P SN SNLS-04D2dc (z=0.1854)– Schawinski et al. 08; Gezari et al. 08

Type II-P SN SNLS-06D1jd (z=0.324)– Gezari et al. 08

SNLS-04D2dc (z=0.1854)
GALEX

Schawinski et al. 08
Gezari et al. 08(Schawinski et al. 08; Gezari et al. 08)

SNLS-04D2dc
GALEX

Shock
breakout

Plateau

UV
Optical

20M , Z=Z , E =1.28851
Radiationhydrodynamics calculation Schawinski et al. 08al. al.
08 08)
E(B-V)host=0.14mag(Schawinskiet al.
al.09)
08; GezariGezarietet(NT etNUV

FUV

Schawinski + 08

2nd peakE(B-V)gal=0.02mag

Monotonicdecay

We construct a Type II-P SN model
reproducing well
the UV LCs of shock breakout.

NT+09

SNLS-04D2dc
Mms=20M8
MpreSN=18.4M8RpreSN=800R8
E=1.2x1051erg(= E of SN1987A)
Typical Type II-P SN

An observationally-calibrated model forshock breakout is obtained.
NT+09

SNLS-04D2dc

Peak magnitude~26.4magTime scale < 1dayRedshift z=1~27.2mag
hour exposure 5s limit~27.6mag 1with8m telescope

The SN can be detected,
if the extinction of the hostgalaxy is small.
(The current record ofnormal SNe is z<0.9.)

13M8, Menv=9.4M
LargerMms 8
8, R=560R
LargerM8
15M8, Menv
=11.0M, R=510R8
ms
More massive stars have larger RpreSN
18M8, Menv=12.3M8, R=710R8
andthusshockbreakouts
20M8, Menv=13.4M8, R=800R8
with longer
andredderspectra.
25M8,duration
Menv=14.7M,R=1200R
88
30M8, Menv=16.0M8, R=1400R8
40M8, Menv=6.8M8, R=1700R8(Solar-metallicitymodels:
Umeda & Nomoto 05)
It is easy to detect
shockbreakoutsof massive stars.

NT +11

13M8

15M8Brighter

25M830M8

NT + 11

18M8 Brighter 20M8

40M8

z=0.5
z=1z=1.5
z=2
z=2.5
z=3

More massive stars haveapparently more luminous shock breakout.





Cosmic star formation history (Hopkins & Beacom 2006)
Distribution of host galaxy extinction (Olivares 08)
IGM absorption (Madau 95)
Extinction distribution(Olivares 08)
Salpeter’s IMF
Shock breakout models (13-40M8)#

Av [mag.]

Hopkins & Beacom 06

gray: Hopkins (2004)
Hatched region & green: FIR (24 mm)
red: radio (1.4 GHz) & H estimate
blue: UV & UDF

104

Observable
SN rate w/ g’Survey area [degree2]103100
Subaru/HSC(Miyazaki+06)

10

1hr obs. w/ future facilities(5s detection)equal survey
power
LSST

1(Ivezic+08)

Pan-STARRS
PS4(Kaiser+02;04)

99%90% g’ w/ 4m
50% r’ telescope
10%g’ 5s det.
1hr int.

With 8m telescope, 50% of detection
are at z>1.2 and 10% are at z>2.3.
The highest z record for normal
CCSN detection will be rewrittenby shock breakout.

w/ 8mtelescope

Reddening (Pei 92)
Our Galaxy
LMC
SMC

Shock breakouts are much bluer thanthe majorities of QSOs or stars.
Color can distinguish shock breakouts
from other short-term variables.

15M8 E51=1
25M8 E51=1
25M8 E51=10

IGM absorption included (Madau95)

QSO
Schneider+02;03;05;07;10
Star SDSSSN rate history
CCSN rate

SNIa rate

It enables observational studies
of CCSNe with DIRECT observations
at the most actively star-forming age.
The study is independent on andcomplementary to the galaxy studies.
(Hopkins & Beacom 2006)

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Shock breakout を取り扱うには、輻射流体計算が必要である。
多波長輻射流体計算コードSTELLAを用いた shockbreakout の輻射流体計算を行った。
観測された shock breakout の多色光度曲線を再現し、さらに遠方宇宙で起こる shock breakout の予想される光度曲線を提出した。
通常の超新星爆発でも遠方宇宙でも観測でき、遠方宇宙における超新星研究に非常に有用な天体である。
多数の観測によって shock breakout の物理が確立することも期待される。