Download From Progenitor to Afterlife

From Progenitor to Afterlife
Roger Chevalier
SN 1987A
HST/SINS
Core Collapse Supernova Types
IIP (plateau light
curve)
IIL (linear light curve)
Ib (no H, He present)
Ic (no H, no He)
IIb (H early; like Ib or
Ic late)
IIn (narrow line)
IIpec (peculiar, e.g.,
SN 1987A)
Wheeler 1990
Progenitor stars
IIP (plateau)
– Red supergiant
IIb, IIn (narrow line), IIL (linear)
– Red, or cool, supergiant
Ib, Ic
– Wolf-Rayet star
SN 1987A – like
– Blue supergiant
Single massive star evolution
Heger et al. 2003
Fractional frequency of SN Types
(Cappellaro,….)
Type IIP
Types IIL, IIn, IIb
Types Ib,Ic
SN 1987A – like
0.3
0.3
0.25
0.15 (upper limit)
High incidence of Type IIL/n/b and Ib/c
indicates that binary evolution is important
Element mixing by instabilities
during explosion
Kifonidis et al. 03
Supernova density profile
Break at velocity
vbr ~ (E/M)1/2
(Matzner & McKee 99)
vbr ~ 3000 km/sec
for E=1051 ergs
and M =10 M
Maximum velocity
limited by radiation
Afterlife properties that depend on
SN type
Composition structure
Maximum velocity
Photoionizing radiation at shock
breakout
Core (neutron star/black hole) mass
Fallback of matter to central core
Density structure (on E and M)
Reverse
shock
Freely
expanding
ejecta
Forward
shock
cs wind
Blondin, RAC
Cas A radio
NRAO/AUI
Type Ic SN 1994I in M51
Model with
synchrotron
self-absorption
and interaction
of outer steep
power law
profile with a
wind
n-1.0 spectrum,
R~t0.9
Data from Weiler, Stockdale,….
Type Ib/c, no
GRB
Type Ib/c, GRB
Type IIb
Type IIP
Type IIL
Type IIn
Type Ib/c, GRB
Relativistic
H env. – 0 M
Type Ib/c, no
GRB
H env. - 0 M
Type IIb – WR
H env. - 0.01 M
Type IIb – RSG
H env. - 0.1 M
Type IIL
H env. - 1 M
Type IIP
H env. - 10 M
SN 1987A – delayed radio increase
optically
thick
optically
thin
Data from Ball
X-ray
SN 1994I at 7 years
Chandra Immler et al. 02
Model radio – X-ray spectrum
of SN Ic
Photosphere
Inverse Compton
Synchrotron
Fransson/RAC
X-ray emission
Type II
–Thermal
Type Ib, Ic
–Synchrotron
–Inverse Compton near maximum
light
Mass loss
IIP (plateau)
– ~10-6-10-5 M/yr (vw=10 km/sec)
IIb, IIn (narrow line), IIL (linear)
– ~10-5-10-3 M/yr (vw=10 km/sec)
Ib, Ic, some IIb
– ~10-6-10-4 M/yr (vw=1000 km/sec)
if magnetic amplification efficient
Long duration gamma-ray
bursts
Associated with SNe Ib/c, ~1/200 the
rate
Afterglow theory well-developed, but
generally indicates interaction with a
constant density medium
Synchrotron emission
Spherical relativistic
blast wave early
Jet effects late
Sari et al. 98
Zhang & Woosley
Shocked wind
bubble a
possibility, but
termination shock
radius too large,
transition not
seen,…
SN 1987A
1/3 pc scale HST/SINS
Light echo – dense wind to ~5 pc
Extended mass loss
Fast wind during main sequence phase
gives extended bubble
Slow RSG wind extends to
rRSG
.


M


 5.0 
5
1
 5  10 M sun yr 


1/ 2
1/ 2
 vw   p / k 

  4 3 
 15 km / s   10 cm K 
1 / 2
pc
During possible Wolf-Rayet phase, dense
wind can be swept out by the fast wind
Inner and outer interaction
Shock in ejecta
Reverse
shock
Pulsar wind termination shock
Blondin, RAC, Frierson 01
Forward
shock
Possible IIP - Crab
No outer
interaction
observed
Crab has low
velocity hydrogen
Crab abundances
imply progenitor
mass ~10 M
G21.5-0.9 – initially pure pulsar
nebula
Radio
Becker & Szymkowiak 1981
Chandra – X-ray
Matheson & Safi-Harb 2005
0540-69, Kes 75, MSH 15-52
Kes 75, X-ray
Helfand et al. 03
Radii 9-20 pc
Average velocity
>~10,000 km/sec
Seem to have
crossed “wind
bubble”
Not IIL/n/b
Probably Ib, Ic;
irregular shell may
be RSG wind
swept out by WR
star wind
Young PWNe
SNR
Crab
3C 58
Kes 75
G11.2-0.3
G292.0+1.8
0540-69
MSH 15-52
.
Type
P
IIP
IIP
Ib/c
IIL/n/b
IIL/n/b
Ib/c
Ib/c
(msec)
33
66
325
65
135
50
150
P0
estimate
(msec)
20
40
60
60
20
40
40
B
(1012 G)
4
4
48
2
10
5
14
Wind interaction model for Cas A
- likely IIL/n/b
Expansion rate of
bright shell and
forward shock
consistent with wind
(r~r-2) interaction
model
Wind density: dM/dt
~3x10-5 M/year for
vw=10 km/sec
Contains a quiet,
compact object
RAC & Oishi 03
NASA/SAO/CXC
Summary
Properties of young remnants can be
related to supernova properties; mass loss
environment deduced from interaction
generally consistent with evolutionary
expectations (not the case for GRBs)
Present data do not show a correlation of
pulsar/neutron star properties with
supernova type
Reverse shock in Cas A
(Fesen,Morse,RAC…)