Type Ic Core-Collapse Supernovae
Evolved from Very Massive Stars
Takashi Yoshida
Yukawa Institute for Theoretical Physics, Kyoto University
Hideyuki Umeda, Shinpei Okita
Department of Astronomy, University of Tokyo
Supernovae and Gamma-Ray Bursts in Kyoto, 2013
Conference on Supernovae
October 29, 2013

as radioactively powered (SLSN-R), hydrogen-rich (SLSN-II), and hydrogen-poor (SLSN-I, the most sizes in−1a large∼ 200(300)km
areequatorial
rotation
ofthev eSLSN-R
tion sof survey
luminousclass). TheSLSN-II and SLSN-I
classes are morecommon,rates
whereasclassisderived properties of R136a1,
R136a2,
R136a3betterunderstood. The physical origins∼1.75
of the extreme
luminosity
emittedby SLSNe
are aMfocus of(2.75)
Myr fora 300(150)
star.signed to findmassive stars in R136
and NGC 3603 predictions,733!
MCVerymetallicity
evolutionary
undercosmological u
current research.
R136 and NGC 3603 stars used in this study.
fields of view tg

Very Massive Stars
Date

Super-luminous SN-R

MMS~320M starsinR136
upernova explosions play1994 July
1994 July
1996 January

Proposal/PI

5157/Ebbets
5157/Ebbets
6018/HeapS-23

Absolute magnitude (mag)important roles in many
SLSN−IH,
aspectsofastrophysics.
-22
HSLSN−II
H,
1996 January
6018/Heap
They are sources of heavy eleSLSN−R
H
SLSN threshold-21
ments, ionizing radiation, andH,
1996 January
6018/Heap
SN IInHenergetic particles; they driveH1996 November
6417/Massey
SN Ia
-20
gas outflows and shock waves
2005 November–
076.D-0563/Schnurr
SN Ib/c2005 Decemberthat shape star and galaxy for-19
2005 November–
076.D-0563/Schnurr
SN IIbmation; and they leave behind2005 December
2005 November–
076.D-0563/Schnurr
SN II−Pcompact neutron star and black-18
2005 DecemberH
1994 September
5445/Drissenhole remnants. The study of superH
1994 September
5445/Drissen-17
novae has thus been actively
H
1994 September
5445/Drissen
2005 April–
075.D-0577/Moffat
pursued for many decades.
2006 February-16
The past decade has seen the2005 April–
075.D-0577/Moffat(Crowtheretal.
2010)
2006 February
discovery of numerous superlu-15
2005 April–
075.D-0577/Moffat
minous supernova events (SLSNe;2006 FebruaryFig. 1). Their study is motivated-14by their likely association with-13
the deaths of the most massive
-100
0100
200300400500600stars, their potential contribuDays from peaktion to the chemical evolution of(Gal-Yam2012)
the universe and (at early times) Fig. 1. The luminosity evolution (light curve) of supernovae.
Common SN explosions
to its reionization, and the possi- reach peak luminosities of ~1043 ergs s−1 (absolute magnitude > −19.5). Superbility that they are manifestations luminous SNe (SLSNe) reach luminosities that are greater by a factor of ~10. Theof physical explosion mecha- prototypical events of the three SLSN classes—SLSN-I [PTF09cnd (4)], SLSN-II [SNnisms that differ from those of 2006gy (12, 13, 77)], and SLSN-R [SN 2007bi (7)]—are compared with a normal
their more common and less lu- type Ia SN (Nugent template), the type IIn SN 2005cl (56), the average type Ib/c(alsoe.g.,minouscousins.
light curve from (65), the type IIb SN 2011dh (78), and the prototypical type II-P SNet al. 2009)
Withextreme luminosities
ex- 1999em (79). All data are in the observed R (Gal-Yamband (80).
Langeret al. 2007,
tending over tens of days (Fig. 1)
et al.
2013)
and, Yusof
in some cases,
copiousultraviolet (UV) flux, ciple, almost all SLSNe belong to one of two ample of the cSLSN events may become useful cosmic beacons spectroscopic classes: type IIn (hydrogen-rich 18 November
Figure 1. VLT MAD K s -band 12 × 12 arcsec2 (3 × 3 pc2 for the LMC
8with innarrow
emissionlines, Octoberwhich are 29,
enablingstudiesof distant star-forminggalaxies events
sient2013
located a
Takashi
Yoshida“Supernovaeand Gamma-Ray
BurstsKyoto”,
YITP,
distance of 49 kpc) image of R136 (Campbellet al. 2010)
togetherwith aSLSN-R

R136

SN IIP

SN 2007bi
Pair-instability SN?

SN 2007bi

ODEL FOR SN 2007bi-21

CC100 (no mixing)
PISN270
SN 2007bi bol
SN 2006gy (Y10) bol
SN 2006gy (Agnoletto+ 2009) bol
SN 2006gy (Smith+ 2007) R-20
-19
absolute magnitude

L85

Type Ic SLSN
MR,max = -21.3 mag(Gal-Yam et al. 2009)

Z = 0.2-0.4 Z host galaxy-18(Young et al. 2010)-17-16

Ejected 56Ni amountM(56Ni) ~ 3.5-7.4 M-15(Moriya et al. 2010)-14-100

0100
200
days since the maximum magnitude

300

400Figure 3. PISN model for SN 2006gy (PISN270). The bolometric LC of SN
2006gy is taken from Y10 and Agnoletto et al. (2009). The first point of SN
2006gy is the R-band upper limit from Smith et al. (2007). The CC100 nomixing model and the observed bolometric LC of SN 2007bi in Figure 1 arealso shown. The horizontal axis shows the days in the rest frame.
(A color version of thisCOfigure is available in the online journal.)

Possibilities of explosion mechanism
Pair-instability SN (PISN) Core collapse SN (CCSN)
M ~ 95 - 105 M
MCO ~ 43 M

(Moriya et al. 2010)(Gal-Yam et al. 2009)(CC100). Here, we confirm the claim made by G09 that a PISN
model can also be consistent with the bolometric LC of SN
2007bi by using the approximate
PISN
PISN270.
(Chatzopouloset modelal. 2013)(e.g., Nicholl et al. 2013)
The PISN270 model is constructed by scaling the physical7
Takashi Yoshida“Supernovaeand Gamma-RayBursts in Kyoto”, YITP, October 29, 2013
structure of the homologously
expandingmodel CC100
to theInteraction with CSM

Magnetar-energized ejecta

Evolution and SNe of Very Massive Stars
Progenitors for SNe Ic with large 56Ni production

Massive Star evolution (TY & Umeda 2011; Umeda, TY & Takahashi 2012)
MMS = (13 -) 100 - 500 M , Z=0.004
Mass loss rate
Main-sequence

Vink et al. (2001) ∝ Z0.69 , Z0.64

Red giantde Jager et al. (1988) (Z dependence: ∝ Z0.64 )Wolf-Rayet stars

Nugis & Lamers (2000)(Z dependence: Vink & de Koter 2005)

Final mass, CO-core mass, stellar type
56Ni production in aspherical core-collapse SNe Ic

Aspherical SN explosions of 110 and 250 M stars (Z=0.004)
with various opening angles θop
Dependence of M(56Ni) and ejecta amount on θop
Constraints from the observations of SN 2007bi
6Takashi Yoshida “Supernovae and Gamma-Ray Bursts in Kyoto”, YITP, October 29, 2013

Final Mass of Very Massive Stars(TY & Umeda 2011).
.
MC=0.5Mst.
.
MA=Mst
.
.
MB~1.5Mst

Z = 0.004.
.
M
A: standard (Mst).
.
MB ~ 1.5 Mst(WR stars: Crowther 2007).
.
MC = 0.5 Mst(e.g., Discussion in Hirschi 2008,Pulse et al. 2008)

Stellar types○RG star, ■WN star
WC star, WO star
Final mass Mf depends on mass loss rate.
MMS > 100 - 140 M
5WO or WC stars ... SNe Ic

Takashi Yoshida “Supernovae and Gamma-Ray Bursts in Kyoto”, YITP, October 29, 2013

CO Core Mass of Very Massive Stars(TY & Umeda 2011)PISN
SN 2007bi
M(56Ni) > 3 M.
.
MC=0.5Mst.
.
MA=Mst
.
.
MB~1.5Mst
M(56Ni) > 1 M

Z = 0.004
Available 56Ni amountfrom CCSN (Umeda & Nomoto 2008)
M(56Ni) ~> 1 M
MCO ~> 10 M , E51 ~> 10M(56Ni) ~> 3 M
MCO ~> 30 M , E51 ~> 20PISN

MCO > 60 M
(Heger & Woosley 2002,
Umeda & Nomoto 2002)

A: 110 < MMS < 280 M
CC SN Ic with M(56Ni)>3M
Small mass loss rate
PISN is possible for SN 2007bi
4

Takashi Yoshida “Supernovae and Gamma-Ray Bursts in Kyoto”, YITP, October 29, 2013

Pulsational Pair-Instability SNe
Pulsational pair-instability (PPI) SNe
Core-collapsePulsations by pair-instabilitye-e+

250 M“unstable”

250 M → 61 M WO
MCO=56 M(40 ~< MCO ~< 60 M )(Heger & Woosley 2002)

PPI SN (CCSN)
110 M

3110 M → 43 M WO
MCO=39 M(MCO <~ 40 M )CCSNTakashi Yoshida “Supernovae and Gamma-Ray Bursts in Kyoto”, YITP, October 29, 2013

56Ni Production of Aspherical CC SNe

Dependence on opening angle θop
SN 2007bi
Mtotal/10
250M(TY, Okita, Umeda, submitted)

Eθop

Energy injection

M(56Ni)
110M

Mass cut: 2.0 M
250 M model (solid lines)

E = 7×1052 erg
110 M model (dashed lines)

E = 5×1052 erg
Aspherical explosion
Reproducing 56Ni mass in SN 2007bi
One possibility for explosion mechanism of SN 2007bi
2Takashi Yoshida “Supernovae and Gamma-Ray Bursts in Kyoto”, YITP, October 29, 2013

Conclusions
Very massive stars in Z=0.004
Final mass and CO-core mass strongly depend on the mass loss rate.
Progenitor of SNe Ic

MMS > 100 - 140 M

SNe Ic with large 56Ni production
CCSN (PPI SN) with M(56Ni) ~>3M
110 ~< MMS ~< 280 M , E ~> 2×1052 erg
PISN with M(56Ni) ~> 3 M
MMS ~> 500 M(MMS ~> 300 M with small mass loss rate)

Aspherical CC (PPI) SN models
MMS=250M and E=7×1052 erg, MMS=110M and E=5×1052 erg

One possibility for explosion mechanism of SN 2007bi
1Takashi Yoshida “Supernovae and Gamma-Ray Bursts in Kyoto”, YITP, October 29, 2013