Gamma-Rays from Supernovae Gamma-Rays from Supernovae Roland Diehl MPE Garching • Gamma-Ray Line Astronomy and Supernovae • Specific Objects • Thermonuclear Supernovae ( 56 Co; SN1991T, SN1998bu) •Core-Collapse Supernovae ( 44 Ti; Cas A; 26 Al and 60 Fe) •Prospects with The COMPTEL Team: Hans Bloemen, Robert Georgii, Wim Hermsen, Jürgen Knödlseder, Giselher Lichti, Dan Morris, Uwe Oberlack, Stefan Plüschke, Jim Ryan, Andrew Strong, Volker Schönfelder, et al. and Karsten Kretschmer, Nikos Prantzos, Dieter Hartmann, Mark Leising, Frank Timmes, Georges Meynet, the SPI Team, et al.
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Gamma-Rays from SupernovaeGamma-Rays from Supernovae
Roland DiehlMPE Garching
• Gamma-Ray Line Astronomy and Supernovae• Specific Objects
• Thermonuclear Supernovae (56Co; SN1991T, SN1998bu)•Core-Collapse Supernovae (44Ti; Cas A; 26Al and 60Fe)
•Prospects
withThe COMPTEL Team: Hans Bloemen, Robert Georgii, Wim Hermsen, Jürgen Knödlseder, Giselher Lichti, Dan Morris,
Uwe Oberlack, Stefan Plüschke, Jim Ryan, Andrew Strong, Volker Schönfelder, et al.and Karsten Kretschmer, Nikos Prantzos, Dieter Hartmann, Mark Leising, Frank Timmes, Georges Meynet, the SPI Team,
et al.
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
Supernova Gamma-Ray Astronomy:Supernova Gamma-Ray Astronomy:Lines of InterestLines of Interest
Radioactive IsotopesDecay Time > Source Dilution TimeYields > Instrumental Sensitivities
Isotope MeanLifetime
Decay Chain γγγγ -Ray Energy(keV)
Source
7Be 77 d 7Be →→→→ 7Li* 478 Novae56Ni 111 d 56Ni →→→→ 56Co* →→→→ 56Fe*+e+ 158, 812; 847,
1238Supernovae
57Ni 390 d 57Co→→→→ 57Fe* 122 Supernovae22Na 3.8 y 22Na →→→→ 22Ne* + e+ 1275 Novae44Ti 89 y 44Ti→→→→ 44Sc*→→→→ 44Ca*+e+ 78, 68; 1157 Supernovae26Al 1.04 106y 26Al →→→→ 26Mg* + e+ 1809 Stars, Novae
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
SN1991TSN1991T
SN1991T:SN1991T:in NGC4527 on 10 Apr 1991Distance 9..11..13..17 MpcPeculiar SNIaearly: no Si absorption, Fe emission instead;overluminous; late: ~standard SNIa; overluminous
COMPTEL Measurement:COMPTEL Measurement:Observations at Days 66-79, 176-1903-5σσσσ Significance of Line Detection:11.7 (±3.2 ±2.7) 10-5 ph cm-2 s-1 (all combined)9(±3) 10-5 ph cm-2 s-1 (847 keV day 70)6(±2) 10-5 ph cm-2 s-1 (1238 keV day 70)
Inferred 56Ni Mass: ~ 1.65 Mo (0.7...2.6 Mo)(cmp 1.14 Mo from Bolometric Lightcurve, Contardo et al. 2000)
Large Uncertainties of Gamma-Ray Flux MeasurementInadequate Spectral Resolution
Morris et al., 1995, 1997, 2002
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
SN1998buSN1998bu
Szuntzeff et al., AJ 117 (1999)
Whipple Obs; Jha et al., ApJS 125 (1999)
• SN on May 1..2, 1998• Discovery on May 9.9, Ia Identification on May 14• Host Galaxy M96 / NGC 3368 in Leo I (RA 10 46.8 Dec 11 50; l=234.5, b=57.0)
• ~Closest SNIa: D~8...12 Mpc (D98bu~0.7 D91T)(Ceph.8.2 by Tanvir et al. 1995(!); Tully-F.~8.1; HST-Ceph.11.6±0.8; PN 9.6±0.6)
Early Envelope γγγγ-Transparency (e.g. SNIa within ~30-100d)Gamma-Ray Transport Comparatively StraightforwardLine Ratio Diagnostics -> Envelope Structure; MixingLine Shape Diagnostics -> Velocities of Inner SN Ejecta
-> Rare OpportunitiesTimely Observations are Critical
No Real Help on SN Physics Yet,Let‘s Hope for INTEGRAL et al.
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
44Ti
44Ca
ττττ =89y, EC
44Sc
ττττ = 5.4 h, ββββ+
Core-Collapse Supernovae: Core-Collapse Supernovae: 4444Ti from Cas ATi from Cas A
44Ti Decay: ττττ~89y -> Young SNR
44Ti Decay Gamma-ray Fluxes from Cas A
0
1
2
3
4
5
COMPTEL 1999 OSSE 1996 RXTE 1997 SAX 2000
I * 1
0-5 p
h cm
-2 s
-1
Difficult γγγγ-Ray Region (78, 68, 1157 keV) -> Uncertain Iγγγγ->44Ti Ejected Mass ~0.8-2.5 10-4 Mo
Iyudin et al., 1994; The et al.1996; Rothchild et al. 1998; Vinket al. 2000
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
4444Ti from Cas A / cc-SNae: The IssueTi from Cas A / cc-SNae: The Issue
Consistency ofCas A cc-SN Model:
44Ti Yield in Models: ~2-4 10-5 Mo44Ti Estimate for SN1987A: ~5-20 10-5 Mo44Ti Estimate from γγγγ-Rays for Cas A: ~8-25 10-5 Mo44Ti Ejection Should Be Correlated to
High-Entropy Material -> a-Rich Freeze-OutLarge Explosion EnergyLarge Mass of Ejected 56Ni (Bright Supernova)
Timmes et al., 1996
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
XMM-NewtonXMM-Newton
ISOISO
Cas A: A Well-Studied Young Nearby SNRCas A: A Well-Studied Young Nearby SNR
~330 year-old SNR at ~3.4 kpcMassive Progenitor (10-25 Mo)Filaments, Fast Ejecta (knots),Fe-rich Clumps, No Onion-Shell-Like Elemental Morphology, Jet:Asymmetric ExplosionUnseen SN -> CSM DustCentral Object (NS/BH?)44Ti (and 56Ni) Ejection
ChandraChandra
HSTHST
=> (?)Non-Typical Core Collapse SN,AsymmetriesThe SN with Proven 44Ti Ejection
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
Search for Search for 4444Ti from Galactic cc-SupernovaeTi from Galactic cc-Supernovae
No 44Ti Sourcesin Inner Galaxy
Parent Distribution of Sources ~ 26AlMonte-Carlo Study-> 44Ti SNR Number Low
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
2626Al Map & Possible Source TracersAl Map & Possible Source Tracers
Massive Stars are theMassive Stars are thePlausible SourcesPlausible SourcesMap Irregularity and Scale Height,Bright Spiral-Arm TangentsCorrelated with Star-Forming GasCorrelated with Warm DustCorrelated with Diffuse Ionized Gas
26Al Ejection by WR Starsor by cc-SNae?
CO map ofmolecular gas
IR map at240 µµµµm, dust
Radio map at53 GHz,free electrons
Hαααα Emissionfrom IonizedGas
RD with Knödlseder, Prantzos, Oberlack, Plüschke, Bloemen, et al. (1996...2002)
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
Modeling Modeling 2626Al from Star ClustersAl from Star Clusters
Stellar Content(OB Association Richness, IMF)
Stellar EvolutionLifetimeWR Phase
26Al Yields per Staryields
1.809 MeV “Light Curve” for aMassive-Star Cluster
->-> Plüschke et al., 2001; Cerviño et al. 2002
WR Stars cc-SNae
plusother Observables
UV / Ionization (-> free-free Emission)
Kinetic Energy / X Brightness
Plüschke Ph D Thesis, 2001
Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002
Interesting Nearby Sources infront of Vela Molecular Ridge