Structure and Evolution of Stars Lecture 16
erred from this.
Table 13.1. 16. Historical supernovae. year (AD) 185 386 393 1006 1054 1181 1572 1604 ∼1667
V (peak)
SN remnant
SN type
compact object
−2
RCW 86 ? ? PKS 1459-41 Crab nebula 3C 58 ‘Tycho’ ‘Kepler’ Cas A
Ia? ? ? Ia? II II Ia Ia? IIb
–
−3 −9 −6 −1 −4 −3 > ∼+6
– NS (pulsar) NS (pulsar) – – NS
sn2001cm-20010617.flm.gif 792×612 pixels
14/10/11 2:48 PM
Type II SN 2001cm
Hα
Hγ Hβ
sn2001n-20010122.flm.gif 792×612 pixels
14/10/11 1:56 PM
Type Ia SN 2001N
Si II
Typical Light Curves of Type II SNe
Doggett & Branch 1985
Annu. Rev. Astro. Astrophys. 2009.47:63-106. Downloaded from www.annualreviews.org by 88.108.86.68 on 09/29/11. For personal use only.
FORS BVI and ISAAC K
a
NACO K
b
5" (95 pc)
WFC F439W, F555W, F814W
c
ACS HRC F330W, F555W, F814W
d
1" (41 pc)
WFPC2 F300W, F606W, F814W
ACS HRC F435W, F555W, F814W
e
f
1" (45 pc)
Slow to moderate rotation
Annu. Rev. Astro. Astrophys. 2009.47:63-106. Downloaded from www.annualreviews.org by Cambridge University on 07/27/11. For personal use only.
8 − 17 M
BIV−O9.5V
Fast rotation
main-sequence
Slow to moderate rotation 17 − 30 M
O9.5V−O6V
Fast rotation
RSG
II-P SN
NS
BSG
SN1987A
NS
Interacting binary
IIb
NS
Ibc
NS
RSG
Faint SN?
BH
WR star
Broad-lined Ibc
NS or BH?
Interacting binary
Ibc or faint SN?
NS
BH
Slow to moderate rotation >30 M
O6V−O3V
Fast rotation
WR
Faint SN?
BH
WR
Broad-lined Ibc
BH
GRB at low-Z
BH
Ultrabright SNe
PISN or Jet?
lln
PISN or Jet?
LBV
Dashed line denotes a rare channel Figure 12
A summary diagram of possible evolutionary scenarios and end states of massive stars. These channels combine both the observational
Annu. Rev. Astro. Astrophys. 2009.47:63-106. Downloaded f by Cambridge University on 07/27/11. For per
2006ov 2004et ransients of Uncertain Nature: Core Collapse or Not? 2008bk 2005cs guing new twist in the story of optical transients occurred in 2007 and 2008. The discovery 2003gd objects with similar luminosities, color temperatures, and line velocities within a few months 2004A
6 5 4 3 2 1
suggestions that they are physically related and that other peculiar transients could be 5 same class. Kulkarni et al. (2007) reported the discovery of an optical transient in M85
5
10
20 19 18 17 16 15 14 13 12 11 10 9 8 7 6 5 4 3 2 1 15
20
25
30
Initial mass (M ) 82
b
(M )
25
95%
Smartt
95%
90%
15
20
25
30
Initial mass (M )
95%
b
95%
25
Maximum initial mass (M )
a
2003ie 1999an 2002hh 1999ev 1999br 1999em 2001du 2004dj 1999gi 2006my 2007aa 2004am 2004dg 2006bc 2006ov 2004et 2008bk 2005cs 2003gd 2004A
10
90%
90%
95%
20
90%
68%
95%
68%
15
90% 95% 90% 95%
5
6
7
8
Minimum initial mass (M )
9
10
Georgy et al. 2009
nuclei
Initial Phase of Collapse (t ~ 0)
RFe~ 3000
Neutrino Trapping (t ~ 0.1s, c ~10¹² g/cm³)
R [km]
$
R [km]
RFe
!e !e !e
~ 100 Si
Si !e
Fe, Ni
Fe, Ni
!e
!e 0.5
~ MCh M(r) [M ]
1.0
0.5 heavy nuclei
Si−burning shell
R [km]
$
$
RFe radius of shock formation
Si−burning shell
Shock Propagation and !e Burst (t ~ 0.12s)
R [km]
Bounce and Shock Formation (t ~ 0.11s, c %< 2 o )
M(r) [M ]
Mhc 1.0
RFe Rs ~ 100 km
!e
!e
R! !e Si
~ 10 Fe, Ni
!e
0.5 nuclear matter
Ni
$ $
Rs ~ 200 !e,µ," ,!e,µ,"
free n, p
10 5
M(r) [M ]
nuclei
Si−burning shell
Neutrino Cooling and Neutrino− Driven Wind (t ~ 10s) !e,µ," ,!e,µ,"
10 4 Ni
10 3
Si
Si
p R ! ~ 50
!e !e
PNS
!e
1.0
Si−burning shell
R [km]
!e
Fe
free n, p
M(r) [M ]
Shock Stagnation and ! Heating, Explosion (t ~ 0.2s)
Rg ~ 100
!e Si
!e
0.5 1.0 nuclear matter nuclei ( >% & )
R [km]
position of shock formation
n
gain layer 1.3 cooling layer
!e,µ," ,!e,µ,"
10
# r−process?
2
R ns~ 10 1.5 M(r) [M ]
R! PNS 1.4
#, n n, p
9
#,n, Be, 12 C, seed
He O
!e,µ," ,!e,µ,"
3 M(r) [M ]
Typical Light Curves of Type II SNe
Doggett & Branch 1985
of decay of 60Co seen After
Before
Detection of neutrino burst by Super-K (~12). IMB saw 8 (out of est. 1020 entering detector!!!)
al” is
er
Matz et al. 1988 (SMM)
Bloom et al. 2009
Nature 461, 1254-1257(29 October 2009) doi:10.1038/nature08459
Quasar
Intergalactic “Clouds”
