From Progenitor to AfterlifeFrom Progenitor to Afterlife

Roger ChevalierRoger Chevalier

SN 1987A HST/SINS

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

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

Single massive star evolutionSingle massive star evolution

Heger et al. 2003

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

Element mixing by instabilities Element mixing by instabilities during explosionduring explosion

Kifonidis et al. 03Kifonidis et al. 03

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)

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)

Forward shock

Reverse shock

Freelyexpanding ejecta

cs wind

Blondin, RAC

Cas A radioNRAO/AUI

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,….

Type Ib/c, no GRBType Ib/c, GRBType IIbType IIPType IILType 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 increaseSN 1987A – delayed radio increase

Data from Ball

opticallythinoptically

thick

X-rayX-ray

Chandra Immler et al. 02SN 1994I at 7 years

Model radio – X-ray spectrum Model radio – X-ray spectrum of SN Icof SN Ic

Fransson/RAC

Inverse ComptonPhotosphere

Synchrotron

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

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

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

Synchrotron emissionSynchrotron emission

Spherical relativistic Spherical relativistic blast wave earlyblast wave early

Jet effects lateJet effects lateSari et al. 98

Zhang & Woosley

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,…

SN 1987ASN 1987A

1/3 pc scale HST/SINSLight echo – dense wind to ~5 pc

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

Inner and outer interactionInner and outer interaction

Blondin, RAC, Frierson 01

Forwardshock

Reverseshock

Shock in ejecta

Pulsar wind termination shock

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

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

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

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

.

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

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

Reverse shock in Cas AReverse shock in Cas A (Fesen,Morse,RAC…)(Fesen,Morse,RAC…)