最近の超新星爆発研究
冨永望(甲南大)2011年11月6日 第24回理論懇シンポジウム「理論天文学・宇宙物理学の革新」

Contents• Introduction• Recent studies– Detection of progenitor system– Supernova survey era– Update of triple-alpha reaction rate– Progresses• SummarySN classification
IaIbSiIIO CaHe

Type I

Type IISiIc

HNe

H94I
97ef
98bw
Wavelength [Å]HeIa

IbIc© Masaomi Tanaka

“for the discovery of the accelerating expansion of theUniverse through observations of distant supernovae”

Observation of progenitor system-Type Ia supernovae-

Progenitor system of Type Ia SN• White dwarf + binary companion• Binary companion
Single degenerate (SD)Main-sequence star
Redgiant star

Double degenerate (DD)White dwarf

Delay time distribution• Distribution of time since star formation

Totani + 08

Delay time distribution
Single degenerate scenario
Lifetime of binary companion
Hachisu + 08

Double degenerate scenario
Binary separation
Ruiz-Lapuente & Canal 98
3 a
dN dN dR0
DTD(t ) t 4
dt dR0 dt

Gravitational wave:t  R04

Initial separation: R0

Peters 64dN R0 aBinary separation:
dR0Nearby binary systems: a~1

Early light curve of SN Ia
Kasen 10
Hydrodynamical calculation

Multigroup radiative transfer
with an artificial ejecta model

Early light curve of SN Ia

Note: there are no confirmation of model LC by other groups.

Bianco + 11

Kasen 10

Type Ia SN2011fe in M101
Palomar Transient Factory (PTF) found a Type Ia
SN in M101 at ~<1day after the explosion.

d=6.4Mpc
HST observation is available

Li+11

Strongest constraint
on binary companion
SN Ia candidate in our Galaxy
A RG channel in SD scenario with aMms>3.5M8 companion is prohibited
for a progenitor system for SN2011fe.
+Horesh+11SN2011fe
MS channel in SD scenario
or DD scenario

Observation of progenitor system-Core-collapse supernovae-

Evolution of massive star
Massive Star (>10M8)

e--capture SNe (8-10M8)

HHeCO

SiFe

Temp Burning Products
8[10 K] Stage
0.2
H
He
1.5
HeC,O
7
C
Ne,Mg
15NeO,Mg
30
O
Si40
SiCr,Mn5650
NSE
Ni

Core collapse
Fe photodissociation
NS/BH formation

Classes of CCSNe-envelope structureThe different types of CCSNe come from progenitors withdifferent mass loss due to Mms, Z, rotation, and binarity.

Wolf-Rayet stars

Type II SNe

Type Ib SNe

Type Ic SNeObservation of CCSN progenitors
SN1993J progenitor

SN1987A (LMC)(M81, d~3.6Mpc, Aldering+94)

88

Observation of SN IIP progenitors
SN2008bkSmartt 09

RSGs are brighter than BSGs or WRstars. It should be easily detectedin pre-image. But there are only
three gold sets of faint Type IIP SNe.
SN2005cs

SN2003gd

Low upper limit on SN II
Smartt+09

Mmin=8.5+1-1.5M8, Mmax=16.5±1.5M8
This is lower than theoretical prediction.
Enhanced mass loss due to pulsation or rotation is proposed.
Mmax=16.5M8
Mmax=30M8

Enhanced mass loss?
Pulsation (Yoon & Cantiello 10)

Rotation (Ekstrom+11)

Massive stars in LMC
Young star cluster
R136 (30 Doradus)
age: <2Myrmetallicity: 3ZSMC

Crowther+10

Supernova survey era

Supernova surveys• Palomar Transient Factory (PTF)• Lick Observatory Supernova Search (LOSS)• Catalina Sky Survey (CSS)• Pan-STARRS PS1• Nearby Supernova Factory (SNfactory)• Kiso KWFC Supernova Survey/Kiso (KISS)• Hyper Suprime-Cam/Subaru (HSC)Luminous supernovae
z~0.2-0.3

Miller+09

z<~0.5

Quimby+09

Origins of luminous supernovae
CSM interaction

Large amount of 56Ni

Woosley+07

Moriya, NT+ 10

Newborn magnetar

Kasen & Bildsten 10

GRB afterglow

Young+05

Electron-capture supernovae-Explosion of super AGB starKitaura + 06
Janka + 08
Wanajo + 09

ONeMg
core
convective
envelope

Explosion energy
E~1050ergs

Neutron starMB~1.36M8

Ejected 56Ni mass
M(56Ni)~0.002-0.004M8

Detection of electron-capture SNe?
A dust-enshrouded progenitor is found.

M(56Ni)~0.0014M8

Prieto+08;Botticella+09

Update of triple-alpha reaction rate

Triple alpha reaction rate
Disappearance of RGB
Ogata+09

Dotter & Paxton09

Most notable change is the shortening
or disappearance of the red giant phase.

Impacts on massive stars
The influence of the newrate on the evolution ofmassive stars (M>10M8) isminimal.
It is impossible to reach thetypical red giant branch tip
luminosity even if all thereaction rates related toCNO cycles are enhanced bymore than 10 orders ofmagnitude.

Suda+11

Impact on SN Ia progenitor system
Carbon deflagration would
be triggered for lower
accretion rate thandM/dt~4x10-8M8/yr which
has been believed to be
the lower limit of theaccretion rate for thedeflagration supernova.

Nomoto82; Saruwatari&Hashimoto10

Progresses

Low metallicity of GRB hosts
Modjaz+Fundamental plane of GRB hosts
Mannucci+10;11
A relation between stellar mass, gas-phase metallicity, and star formation rate
is followed by high-z gals. up to z~2.5.

Fundamental plane of GRB hosts
Mannucci+10;11
The apparent low metallicity of long GRB hosts is a consequence of the occurrence of a long
GRB in low-mass, actively star-forming galaxies, known to dominate the current cosmic SFR.

But there are scatterson individual galaxies(Yabe, Ohta, prep.
com.).

3D simulation of CCSNe
Critical curves in electron-neutrino driving
luminosity versus accretion rate

Nordhaus+10

The number of tracer-particles travellingin the gain region as a function of theirindividual residency time

Takiwaki+11

Collective neutrino oscillation
Spectral swapping between heavylepton neutrinos and electron-type
neutrinos enhances neutrino heating.
In 2D calculation, E51~0.1  E51~1-4

The postbounce pre-explosion dynamics ofstandard core-collapse supernovae remains
unaffected by neutrino oscillations.
Suwa+11

Dasgupta+11

C-normal Hyper Metal-Poor star
SDSS J102915+172927
Hyper metal-poor(HMP)

Caffau+11(Cayrel+04)

Ultra metal-poor(UMP) C-enhanced
EMP (CEMP)
Extremely metalpoor (EMP)

The abundance pattern issimilar to the EMP stars.

Evidences of SN contributions-Damped Lyman a system-• A system of QSO J0035−0918 (z=2.3, Cooke + 11)– A gaseous system (= no mass transfer from binary companion)– Low N abundance, being similar to EMP stars– High redshift
C-rich DLA ([Fe/H]~-3)
HE 0143−0441 ([Fe/H] = −2.21, Cohen + 04)
BD+44◦493 ([Fe/H] = −3.73, Ito + 09)

Evidences of SN contributions-Damped Lyman a systemC-rich DLA
peculiar DLA (z=1.6, Cooke+10)

Kobayashi, NT + 11

Summary• Detection of progenitor systems in pre-image– Type Ia SN2011fe disfavors RG channel in SD
scenario.
– Lower upper limit on Mms of Type IIP SNe• Supernova survey era– Many rare objects, bright or faint, are found.

• Updated triple-alpha reaction rate
– No RG branch• New discoveries