ANRV284-AA44-12

ANRV284-AA44-12

ARIARI

28 July 2006

28 July 2006

Hypernova: Eex~1052 erg

SN1998bw→ aspherical scenario(Maeda&Nomoto 2008)

GRB: Some observational
samples associated with SN Ic

Annu. Rev. Astro. Astrophys. 2006.44:507-556. Downloaded from www.annualreviews.org
by University of Tokyo on 06/17/11. For personal use only.

Aspherical Nature

Annu. Rev. Astro. Astrophys. 2006.44:507-556. Downloaded from www.annualreviews.org
by University of Tokyo on 06/17/11. For personal use only.

Type Ic SN• Absence of H & He Emission Line• Core-Collapse Explosion of CO
Wolf-Rayet Star ?

14:21

14:21
Figure 2
The location of SN 1998bw
as viewed at late times by
Chandra (top) and HST(bottom). The circles
represent the 1σ
astrometric position fromChandra. The fading X-ray
source (“S1a”) consistent
with SN 1998bw is to thesoutheast (bottom left). From
Kouveliotou et al. (2004).

! = (1 − β 2 )−1/2 . This does not necessarily require that the SN be bright, or even
exceptionally energetic, though GRB-SNe often are. It also does not preclude theexistence of SNe without GRBs, powered by the same energy source (Section 3.4.2).
But to produce a GRB, one needs at least as much energy in relativistic ejecta as
is observed in γ -ray and afterglow emission. That is, ERel ! Eγ . The value of Eγ isdifficult to measure directly because of the effects of beaming, but in typical bursts, it isaround 1051 erg (Frail et al. 2001; Bloom, Frail & Kulkarni 2003). ERel can be inferredfrom radio observations at such late times that beaming is no longer important, and is∼5 × 1051 erg (Berger et al. 2003c; Berger, Kulkarni & Frail 2004). Of course, there
can be considerable variation in both these numbers.
The SNe accompanying GRBs also differ from common SNe (Filippenko 1997)
in other ways (Table 1), most obviously the absence of hydrogen in their spectra:
GRB-SNe appear to be Type I SNe. Indeed, where spectra of sufficient quality exist
to be sure, the SN is of Type Ic-BL. Some of the broad peaks seen in the GRBSNe spectra are likely due to low opacity, rather than due to emission from a single
ion spread over large velocity ranges (e.g., Iwamoto et al. 2003). Near maximum
light, GRB-SNe do appear to show broad absorption lines of O I, Ca II, and Fe II

Woosley & Bloom 2006	

Table 1 Properties of good candidate supernovae associated with γ -ray bursts, X-ray flashes, and X-ray rich
γ -ray bursts

Name
Burst/SN(Section 2.1.6) are now considered the closest cosmological instance of GRB 980425
and SN 1998bw (Soderberg et al. 2004b).

zPeak [mag]SN likeness/
designationaTpeak[day]

References

2.1.5. Late-time bumps. Viewing GRB 980425, and its origin, as distinct fromGRB 980425/1998bw
0.0085
MV = −19.16 ± 0.05
17Ic-BLbIc-BL

cWoosley 1993; Hansen 1999), no other GRB had obvious late-time emission thatGRB 031203/2003lw
0.1005
MV = −19.0 to −19.7
18 – 25

Ibc-BLdIc-BLe

GRB 011121/2001dk

0.365

I (IIn?)f

GRB 050525a

0.606

GRB 021211/2002lt

1.00

GRB 970228

0.695

XRR 041006

0.716

XRR 040924

0.859

GRB 020405

0.695

the “cosmological’’ set of GRBs was the norm in 1998. Though the detection of a

GRB 030329/2003dh0.1685
MV =−18.8 toof−19.6– 13
contemporaneous SN
would be a naturalconsequencea massive star 10origin(e.g.,resembled a SN. A report of a red emission “bump’’ following GRB 980326 (BloomXRF 020903& Kulkarni 1998) 0.25
= −18.6± a0.5was interpreted M
as Vbeingcaused bycoincident SN∼15
at about aa

MV = −18.5 to −19.6

12 – 14Ig

MU = −18.4 to −19.2∼14IchIi

MV = −18.8 to −19.5∼17

16 − 20Ij∼11?

k∼17IlM ≈ −18.8

12MV ∼ −19.2• Supernova–Gamma-Ray Burst Connection
Vwww.annualreviews.org

MV = −17.6
MV ∼ −18.7515

The time of peak brightness is reported in the rest frame if the redshift is known, observed frame otherwise.
Galama et al. 1998a.
cHjorth et al. 2003; Stanek et al. 2003; Bloom et al. 2004; Lipkin et al. 2004.
dMalesani et al. 2004; Cobb et al. 2004; Thomsen et al. 2004; Gal-Yam et al. 2004.
eSoderberg et al. 2005.
fBloom et al. 2002; Garnavich et al. 2003b; Greiner et al. 2003b.
b

A&A 512, A70 (2010)#%%*D#%%'4E#%%&.F"$$"6<"$$+G:"$$'.7"$$'.9!"#B0,-./01234,5678932:4!#%30, )(C4!"#!"$!#&!#%!#'!#(!#&!#)!#'!#*

Young+2010	!#+,$,)$,#$$,#)$!#(,"$$,")$,+$$,+)$

!"$

,$,"$

,*$

,($, , , , , , , , , , , , , , , , , , , , , , , , , , , , , , ;<0=>,?:6@/A

D. R. Young et al.: Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions !!#"  Fig. 5. R-band lightcurve comparisons of SNe Ic (V-band used for SN1997ef comparison). All comparison data have been corrected for extinctionand epochs are relative to the R-band maximum light as stated in the literature and given in the rest frame of the individual SNe. References andcolour-excess: SN 1994I with E(B − V) = 0.300 (Richmond et al. 1996), SN 1997ef with E(B − V) = 0.042 (Iwamoto et al. 1998), 1998bw withE(B − V) = 0.065 (Galama et al. 1998; McKenzie & Schaefer 1999; Sollerman et al. 2000; Patat et al. 2001), SN 2002ap with E(B − V) = 0.09(Foley et al. 2003; Yoshii et al. 2003; Pandey et al. 2003; Tomita et al. 2006), SN 2003jd with E(B − V) = 0.14 (Valenti et al. 2008a). The panelon the right provides an expanded view of the early-time behaviour of the lightcurves.
!!#"%::!;%::<=>&""&84&""'?7&""@,9&""A=,&""A=B

Young+2010	!'#$!'#"

*+,)-)./0,)1 2(%L84!'#$MORIYA ET AL.

!'#"

Ejecta Velocity (1000 km s-1)

Scenario 2: Core Collapse SN
Spherical Explosion of 43Msun CO star
○ 56Ni amount & Light curve evolusion(Moriya+2010)	

16

14

12-19!%#"-18!"#$($")")$")%"")%$")&"")&$"

Ejecta Velocity (1000 km s−1)!&#$ of the profiles of the [O I], Mg I] and [Ca II] emission lines found in the nebular spectra of SNe 1998bw (black), 2003jd
Fig. 15. A comparison(grey) and the final +367 d spectrum of SN 2007bi (red).
T-21!&#$CC100 (no mixing)!&#"
Amount of Element
20
CC100 (half mixing)
Ca II H&K λ3976
CC10018(full mixing)
Na I λ5891
12 C Fe II λ5037
1620 Ne
24 Mg
Si II λ6355
Y10 (bolometric)-20Si II λ6355O
18O I λ7774!%#$G09 (with bolometric
Ca II near−IR λ8571
Ca II near-IR λ8571
16 correction)!&#"absolute bolometric magnitude

Scenario 1: Pair Instability SN
PISN of ~100Msun He star
○ Can reproduce the yield× He envelope remains)(   SN2007bi (Gal-Yum+2009)• Very Luminous Ic SN• Large amount of 56Ni (>4Msun)
56Ni→56Co→56Fe• Single peak of observed [OI] emission
line does not suggest asphericity(Young+2010) 	

!"$)'""

1.4
18.7
O I λ7774 (limit)

1.4

1.5

14

Note. Units: M! .
!%#$1210)'$"(&")")&")!"

3.)@"CORE-COLLAPSE SN) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) ) 34+56).78912

We construct several corethem with the observations ovelocities of SN 2007bi shown-16
46
not cover the rising part of thMoriya+2010	
magnitude of the rising part fro
245060708090100110120130140
0 6 of 19-15
102030405060Page
assuming the same bolometri
Epoch(days)-1000100200300400
Epoch (days)
R-bandmaximum.
We also ta
days since the R band maximum magnitudeFig. 16. Ejecta velocities of SN 2007bg. Time given in the SN Fig. 17. Ejecta velocities of SN 2007bi. Time given in the SN restpossible
thata jetframe. Note that the velocity of O I λ7774 measured
in thespectraof emerges fro
rest-frame. Figure 1. Bolometric LCs of the C+O star SN models
CC100(Mejbe=
40 Mas!a, lower-limit; a consequence of conSN 2007bican onlytreatedthe mixing of the ejecta (e.g., Mtaminationin the bolometricblue-wing by theEkin = 3.6 × 1052 erg, and M56 Ni = 6.1 M! ). Theobserved
LCpeculiar [Ca II] feature.
2009).
(open circles) is taken from Y10. The bolometric magnitude of the rising part8. Emission
lines used
to measureof thehost galaxies
TheLCsof successful modeof SN 2007bi (open square) is estimated from theTable
R-bandmagnitude.
Allthe abundances
108Fig. 6. BVRI-17
quasi-bolometric lightcurve comparisons. All comparison data have been corrected for extinction and epochs are relative to theR-band
maximum light and are give in the rest-frame of the individual SNe. References
and colour-excess: as in Fig. 5, also SN 2006gy with
68E(B − V) = 0.56 (Agnoletto et al. 2009). The panel on the right provides an expanded view of the early-time behaviour of the lightcurves.

60
40
2003.3

Progenitor Model• MMS = 110Msun, Z=0.004• Massive CO Wolf-Rayet star deprivedof upto He envelope by mass loss wind
→ MCO= 43.1Msun
Yoshida&Umeda 2011	

180160140120100806040200(b)Yoshida&Umeda2011	
PISNCCSN

100 150 200 250 300 350 400 450 500
MMS/M!
100Figure 1. The final mass (a) and CO core mass (b) as a function of theMS mass. Solid, dashed, and dotted lines correspond to cases A, B and C,respectively. Squares, triangles, crosses and circles indicate WN, ‘He-rich’
WC (see Section 3.3), WC and WO stars. Dark and light shaded regions deothers
note the mass ranges of the CO cores appropriatefor SN 2007bi to explodeas a PI SN10
and a CC SN, respectively.

[Msun]

Hydrodynamics• Code: 2D axis-symmetric• Explosion Energy: Eex= 30×1051 erg
56Ni ~ 4Msun• Inner boundary: absorbing
Fall-back onto central remnant

MCO/M!

100 150 200 250 300 350 400 450 500
MMS/M!

Fall-back56
Nucleosynthesis studies of PI SNe have indicatedNi that PI SNmodels with 95 M!cut
MCO ! 105 M! produce 3 − 10 M! of 56 Ni(Heger & Woosley 2002). The PI SN models of Umeda & Nomoto1(2002) obtainedresult.
0 a similar
510 Therefore
15
20the progenitor
25
30of thePI SN corresponding to SN 2007bi should
be a CO core with 95
Eex [1051 erg]
! MCO ! 105 M! .
The MS mass range deduced from the CO core mass is shownas the dark shaded region in Fig. 1(b). This criterion is not satisfied
Spherical
explosionin the MS
mass range of MMS " 500M! in cases A and B. The
56Ni is MS
51MMS " 575 M!
mass range
in case Aifis E
estimated
to be 515 "totallyejectedex > 25×10 erg	from linear extrapolation in Fig. 1(b). In case C, the appropriate
range reduces to 310 " MMS " 350 M! .
The amount of 56 Ni produced in a CC SN model gives aSNea qua
not bappea
excit
The sHe an
Ni an
ing oIb an(Welor theThe eof midiscu
tal Hof He

two cprevi
0.5 M(Geoporte
1.5 M(2010timeif He
show
limitof 11C no1.5 M
within cas

set thYoon
massstars
Ic.

ers. T4πa 3 4R T
3
4πa 3 4Eex =R T
3Nucleosynthesis
TNi = 5 × 109 K
Eex =Aspherical Explosion• Induced by abrupt energy• Post-process
TNi = 5 × 109 K
56!with 282 isotopes
injectionin polar direction• Network
Mass and Spatial
Distributionof Ni Induced bythe3 Eex• 7 models
calculatedwith CO Star
RNi = ~ Br) !4(n,pAspherical
Explosionof Massive
4πa TNi 3 Eex
RS.
Okita,H.
Umeda
andT.
Yoshidavarious opening angle (θop)
Ni =Input: Thermodynamical
4πa TNi 4 Histories
3(1(2(33{ri (tn )}, {ρi (tn ), Ti (tn )}Introduction{ri (tn )},(for{ρievery(tn ), Tidifferential(tn )}mass)	

Model & Method

Output: Mass Fraction

performed spherically symmetric and aspherical explosion of massive CO star employing 2D special{X j i } (Σj X j i4πa= 1) 3 4
ativistic hydro-dynamical code. The progenitor model is one of investigated in Yoshida+2011 which isE=R T
exend product of M = 110M! andeZop = 0.004 star in main sequence. It loses the H and He envelope by3
ss loss wind until the pre-supernova stage and becomes 42.7 M! of bare CO core. Explosion energy
adjusted to 30 × 1051 erg and injected from just outside from 2M! of mass-cut during 0.1 sec of theginning of calculation. Precedent studies (eg. Umeda+2008, Moriya+2010) show that explosion of{X j i (tn )}TNi = 5 × 109 K
51
56
100M! star with around 30 × 10 erg induces ∼ 3 − 6M! of Ni in spherical explosion. Now wencentrate on the aspherical effects innerof explosionof massive CO star on produced 56 Ni. Summarized in(i × j × n " 5200 × 282 × 5000)
boundary!
* Explosion energy is injected
ble1, calculated models have various opening angle θop . Hydro-dynamical evolution is calculated until
only aroundpolar axis as
3 Eex
500 sec when the velocity becomes almost homologous
as vthe∝ r.
R = 3kinetic form	Name
θopθop /90◦OA1
7.03◦
5/64

Table 1: Calculated models
OA2 OA3 OA4 OA5
11.3◦ 22.5◦ 45.0◦ 67.5◦
1/8
1/4
1/2
3/4

OA6
78.8◦
7/8

OA7
90.0◦
1

Thermodynamical Histories
Trace Particle Method• 5200 particles
Ni(Δmi~0.001M
sunT)Ni 44πa∀56Ni
Ti ( tn )particle< TNi → Xobtains
i =0• EachAfter the hydro-dynamical simulation, we also employed postprocess for calculating nucleosynthesis.
ermodynamical hystories are traced by maker particles. Nθ × Nr = 40 × 130 = 5200 particles initiallyver the whole progenitor, and typical mass resolution is ∆M ∼ 0.001M! around the center of the star.

56NiTi (∃ tn ) >→X{rT{ρi (tni ),=T1i (tn )}Nin )},i (t(4Ejected Mass [Msun]
540

330

220

100°

Aspherical feature
Aspherical explosion induces
large amount of fall-back10OA5 OA645°
Opening Angle

90°0Ejected 56Ni or 28Si
Steep jump in a certain θop→ narrow explosion eject notmuch 56Ni

O, Ejecta

56Ni
28Si16OEjecta

16

Ni, 28Si

45056

Eex =

4πa 3 4R T
3(1)

5RNi = 3

Ni Mass [Msun]!

(2)

3 Eex
4πa TNi 4{X j i } (Σj X j i = 1)

Simple Evaluation of 56Ni	

56Ni
4πaTi (∀ tn ) < TNi→X
3 04
i =Eex =RT
3∃56NiTi ( tn ) > TNi → Xi =1

TNi = 5 × 109 K!

30.3(4)20.2(5)

1

Produced
1OA5
0.1
Ejected(post-process) Ejected
OA6
Fall-back/Produced(6) (1)
000°
45°
90°
(2)
Opening Angle

3 Eex
RNiSimple= 3
44πa TEvaluation
NiLarge θop: Valid by ~5%{ri (tn )},{ρi (tnθ), Ti (t)}Small
op : nPhoto-dissociation
56Ni → 144He{X j i } (Σj X j i = 1)

0.4
(3) Fall-back56{ri (tn )}, {ρi (tn ), Ti (tn )}4

Fall-back/Produced 56Ni

TNi = 5 × 109 K

0.5(3)Fall-back
56Ni (isotopes produced aroundthe (4)center):strongly affected by fall-back(5)Ejected Mass [Msun]
5Ni
28Si16OEjecta

4030

220

145°
Opening Angle

90°

0

50.5

40.4
Fall-back
0.3

20.2

56

31

Produced
Ejected(post-process) Ejected
Fall-back/Produced

00°

45°
Opening Angle

OA50.1
OA690°

0

Fall-back/Produced 56Ni

Ni Mass [Msun]

10OA5 OA600°

O, Ejecta

316Ni, 28Si

4565056

M(ejec) = 17.4 Msun
M(56Ni) = 1.77 Msun

5e+0956Niothers
accreted

4e+09

3e+09
Z [cm]

56

Ni Accretion Rate [Msun/sec]

0.2

2e+09

12Msun

0.1

7Msun

1e+09

02Msun01e+09

2e+09

3e+09
R [cm]

4e+09

05e+09

020

40

60
80
time [sec]100120140Ejected Mass [Msun]
5Ni
28
Si
16O
Ejecta

40
30

220

145°
Opening Angle

90°

050.5

40.4
Fall-back
0.3

20.2

56

31

Produced
Ejected(post-process) Ejected
Fall-back/Produced

00°

45°
Opening Angle

OA50.1
OA690°

0

Fall-back/Produced 56Ni

Ni Mass [Msun]

10OA5 OA600°O, Ejecta

316Ni, 28Si

456

5056

M(ejec) = 28.7 Msun
M(56Ni) = 2.42 Msun

56
Niothersaccreted

3e+09

56

2e+09
Z [cm]

12MsunNi Accretion Rate [Msun/sec]

0.4
0.3

7Msun
1e+09

0.2
0.1

2Msun

0001e+09

2e+09
R [cm]

3e+09

020

40

60
80
time [sec]100120140

M(ejec) = 36.8 Msun
M(56Ni) = 2.47 Msun

56
Niothersaccreted

3e+09

56

2e+09
Z [cm]

12Msun7Msun
1e+092Msun
001e+092e+09R [cm]

3e+09

0.12
0.1
0.08
0.06
0.04
0.02
0020

Ni Accretion Rate [Msun/sec]

406080time [sec]100120140

Ejected Mass [Msun]
5Ni
28Si16OEjecta

4030

220

145°
Opening Angle

90°

0

50.5

40.4
Fall-back
0.3

20.2

56

31

Produced
Ejected(post-process) Ejected
Fall-back/Produced

00°

45°
Opening Angle

OA50.1
OA690°

0

Fall-back/Produced 56Ni

Ni Mass [Msun]

10OA5 OA600°

O, Ejecta

316Ni, 28Si

4565056

M(ejec) = 40.2 Msun
M(56Ni) = 4.01 Msun

56Niothers
accreted

3e+09

56

2e+09
Z [cm]

12MsunNi Accretion Rate [Msun/sec]

0.1
0.08

7Msun
1e+09

0.06
0.04
0.02

2Msun

000

1e+09

2e+09
R [cm]

3e+09

02040

60
80
time [sec]1001201402e+09Z [cm]

12Msun2e+09

12Msun

7Msun

7Msun

2Msun

1e+09

2e+09

2Msun

03e+091e+09

Ni Accretion Rate [Msun/sec]
0.12
0.1
0.08
0.06
0.04
0.02
00.3
0.2
0.1
02040

60
80
time [sec]2e+09

03e+0901e+09

R [cm]

56

0.4

01e+090

R [cm]

56

2e+09

12Msun7Msun

003e+09

1e+09

1e+09

2Msun

56
Niothers
accreted

3e+09

Z [cm]

56
Niothers
accreted

3e+09

Z [cm]

56
Niothersaccreted

100

120

140

M(ejec) = 28.7 Msun
M(56Ni) = 2.42 Msun

2e+09

3e+09

R [cm]

56

Ni Accretion Rate [Msun/sec]

Ni Accretion Rate [Msun/sec]

0.1
0.08
0.06
0.04
0.02
020

40

60
80
time [sec]

100

120

140

M(ejec) = 36.8 Msun
M(56Ni) = 2.47 Msun

0020406080time [sec]100120140

M(ejec) = 40.2 Msun
M(56Ni) = 4.01 Msun

Chemical Abundance Ejectedby Aspherical Explosion of Massive CO Star
• Aspherical Effect: Ejecta decreases toward small θop• Isotopes produced around the center suffer from Fallback or Hydro-dynamical Effect according to θop• 56Ni is ejected more than 4Msun if θop/90° ≥ 7/8→ Observed sphericity of SN2007bi is not accidental