from progenitor to afterlife roger chevalier sn 1987ahst/sins
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From Progenitor to AfterlifeFrom Progenitor to Afterlife
Roger ChevalierRoger Chevalier
SN 1987A HST/SINS
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Core Collapse Supernova Core Collapse Supernova TypesTypes
IIP (plateau light IIP (plateau light curve)curve)IIL (linear light curve)IIL (linear light curve)Ib (no H, He present)Ib (no H, He present)Ic (no H, no He)Ic (no H, no He)IIb (H early; like Ib or IIb (H early; like Ib or Ic late)Ic late)IIn (narrow line)IIn (narrow line)IIpec (peculiar, e.g., IIpec (peculiar, e.g., SN 1987A)SN 1987A) Wheeler 1990
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Progenitor starsProgenitor stars
IIP (plateau)IIP (plateau) – Red supergiant Red supergiant
IIb, IIn (narrow line), IIL (linear)IIb, IIn (narrow line), IIL (linear)– Red, or cool, supergiantRed, or cool, supergiant
Ib, IcIb, Ic– Wolf-Rayet starWolf-Rayet star
SN 1987A – likeSN 1987A – like– Blue supergiant Blue supergiant
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Single massive star evolutionSingle massive star evolution
Heger et al. 2003
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Fractional frequency of SN TypesFractional frequency of SN Types(Cappellaro,….)(Cappellaro,….)
Type IIP 0.3Type IIP 0.3Types IIL, IIn, IIb 0.3Types IIL, IIn, IIb 0.3Types Ib,Ic 0.25Types Ib,Ic 0.25SN 1987A – like 0.15 (upper limit)SN 1987A – like 0.15 (upper limit)
High incidence of Type IIL/n/b and Ib/c High incidence of Type IIL/n/b and Ib/c indicates that binary evolution is importantindicates that binary evolution is important
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Element mixing by instabilities Element mixing by instabilities during explosionduring explosion
Kifonidis et al. 03Kifonidis et al. 03
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Supernova density profileSupernova density profile
Break at velocityBreak at velocity
vvbrbr ~ (E/M) ~ (E/M)1/21/2
vvbr br ~ 3000 km/sec~ 3000 km/sec
for E=10for E=105151 ergs ergs
and M =10 Mand M =10 M
Maximum velocity Maximum velocity limited by radiationlimited by radiation
(Matzner & McKee 99)
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Afterlife properties that depend on Afterlife properties that depend on SN typeSN type
Composition structureComposition structure
Maximum velocityMaximum velocity
Photoionizing radiation at shock Photoionizing radiation at shock breakoutbreakout
Core (neutron star/black hole) massCore (neutron star/black hole) mass
Fallback of matter to central coreFallback of matter to central core
Density structure (on E and M)Density structure (on E and M)
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Forward shock
Reverse shock
Freelyexpanding ejecta
cs wind
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Blondin, RAC
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Cas A radioNRAO/AUI
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Type Ic SN 1994I in M51Type Ic SN 1994I in M51Model with Model with synchrotron self-synchrotron self-absorption and absorption and interaction of interaction of outer steep outer steep power law profile power law profile with a windwith a wind
-1.0-1.0 spectrum, spectrum, R~tR~t0.90.9
Data from Weiler, Stockdale,….
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Type Ib/c, no GRBType Ib/c, GRBType IIbType IIPType IILType IIn
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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
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SN 1987A – delayed radio increaseSN 1987A – delayed radio increase
Data from Ball
opticallythinoptically
thick
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X-rayX-ray
Chandra Immler et al. 02SN 1994I at 7 years
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Model radio – X-ray spectrum Model radio – X-ray spectrum of SN Icof SN Ic
Fransson/RAC
Inverse ComptonPhotosphere
Synchrotron
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X-ray emissionX-ray emission
Type IIType II –Thermal Thermal
Type Ib, IcType Ib, Ic–Synchrotron Synchrotron
– Inverse Compton near maximum Inverse Compton near maximum lightlight
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Mass lossMass loss
IIP (plateau)IIP (plateau) – ~10~10-6-6-10-10-5-5 M M/yr (v/yr (vww=10 km/sec)=10 km/sec)
IIb, IIn (narrow line), IIL (linear)IIb, IIn (narrow line), IIL (linear)– ~10~10-5-5-10-10-3-3 M M/yr (v/yr (vww=10 km/sec)=10 km/sec)
Ib, Ic, some IIbIb, Ic, some IIb– ~10~10-6-6-10-10-4-4 M M/yr (v/yr (vww=1000 km/sec) =1000 km/sec)
if magnetic amplification efficientif magnetic amplification efficient
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Long duration gamma-ray Long duration gamma-ray burstsbursts
Associated with SNe Ib/c, ~1/200 the Associated with SNe Ib/c, ~1/200 the raterate
Afterglow theory well-developed, but Afterglow theory well-developed, but generally indicates interaction with a generally indicates interaction with a constant density mediumconstant density medium
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Synchrotron emissionSynchrotron emission
Spherical relativistic Spherical relativistic blast wave earlyblast wave early
Jet effects lateJet effects lateSari et al. 98
Zhang & Woosley
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Shocked wind Shocked wind bubble a bubble a possibility, but possibility, but termination shock termination shock radius too large, radius too large, transition not transition not seen,…seen,…
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SN 1987ASN 1987A
1/3 pc scale HST/SINSLight echo – dense wind to ~5 pc
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Extended mass lossExtended mass loss
Fast wind during main sequence phase Fast wind during main sequence phase gives extended bubblegives extended bubble
Slow RSG wind extends toSlow RSG wind extends to
During possible Wolf-Rayet phase, dense During possible Wolf-Rayet phase, dense wind can be swept out by the fast windwind can be swept out by the fast wind
pcKcm
kp
skm
v
yrM
Mr w
sunRSG
2/1
34
2/12/1
15
.
10
/
/151050.5
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Inner and outer interactionInner and outer interaction
Blondin, RAC, Frierson 01
Forwardshock
Reverseshock
Shock in ejecta
Pulsar wind termination shock
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Possible IIP - CrabPossible IIP - Crab
No outer interaction No outer interaction observedobserved
Crab has low Crab has low velocity hydrogenvelocity hydrogen
Crab abundances Crab abundances imply progenitor imply progenitor mass ~10 Mmass ~10 M
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G21.5-0.9 – initially pure pulsar G21.5-0.9 – initially pure pulsar nebulanebula
Radio
Becker & Szymkowiak 1981Chandra – X-ray
Matheson & Safi-Harb 2005
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0540-69, Kes 75, MSH 15-520540-69, Kes 75, MSH 15-52
Radii 9-20 pcRadii 9-20 pcAverage velocity Average velocity >~10,000 km/sec>~10,000 km/secSeem to have Seem to have crossed “wind crossed “wind bubble”bubble”Not IIL/n/bNot IIL/n/bProbably Ib, Ic; Probably Ib, Ic; irregular shell may irregular shell may be RSG wind be RSG wind swept out by WR swept out by WR star windstar wind
Kes 75, X-ray Helfand et al. 03
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Young PWNeYoung PWNe
SNRSNR TypeType PP PP00
estimateestimateBB
(msec)(msec) (msec)(msec) (10(101212 G) G)
CrabCrab IIPIIP 3333 2020 44
3C 583C 58 IIPIIP 6666 4040 44
Kes 75Kes 75 Ib/cIb/c 325325 6060 4848
G11.2-0.3G11.2-0.3 IIL/n/bIIL/n/b 6565 6060 22
G292.0+1.8G292.0+1.8 IIL/n/bIIL/n/b 135135 2020 1010
0540-690540-69 Ib/cIb/c 5050 4040 55
MSH 15-52MSH 15-52 Ib/cIb/c 150150 4040 1414
.
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Wind interaction model for Cas AWind interaction model for Cas A- likely IIL/n/b- likely IIL/n/b
Expansion rate of Expansion rate of bright shell and bright shell and forward shock forward shock consistent with wind consistent with wind ((~r~r-2-2) interaction ) interaction modelmodel
Wind density: dM/dt Wind density: dM/dt ~3x10~3x10-5-5 M M/year for /year for
vvww=10 km/sec=10 km/sec
Contains a quiet, Contains a quiet, compact objectcompact object
RAC & Oishi 03
NASA/SAO/CXC
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Summary Summary Properties of young remnants can be Properties of young remnants can be related to supernova properties; mass loss related to supernova properties; mass loss environment deduced from interaction environment deduced from interaction generally consistent with evolutionary generally consistent with evolutionary expectations (not the case for GRBs)expectations (not the case for GRBs)
Present data do not show a correlation of Present data do not show a correlation of pulsar/neutron star properties with pulsar/neutron star properties with supernova typesupernova type
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Reverse shock in Cas AReverse shock in Cas A (Fesen,Morse,RAC…)(Fesen,Morse,RAC…)