Observational Properties and Observational Properties and Modelling of HypernovaeModelling of Hypernovae
Jinsong DengJinsong Deng
National Astronomical Observatories of ChinaNational Astronomical Observatories of China
Collaborators: P. A. Mazzali (Trieste Obs. & MPA)
K. Nomoto, K. Maeda (Tokyo Univ.) et al.
DARK ENERGYD EN G
What are hypernovae? Why the studies?
• hyper-energetic supernovae (HNe)~1052 ergs or bigger (normal SN: ~1051ergs)
PI SNe Woosley 1982, GRB-related energetic stellar explo. Paczynski 1998
collapsar alike GRB models Woosley et al. since 1999
• a subset of Type Ic supernovaecore-collapse SNe, massive CO stars
• some are related to gamma-ray burststhe origins of long GRBs
Hypernovae are characterized by very broad spectral lines
• very borad lines
high ejecta velocities (~104-105 km/s)
large kinetic energy (~1052 ergs)
hypernovae
• relatively narrow lines
low ejecta velocities (~103-104 km/s)
normal kinetic energy (~1051 ergs)
normal supernovae
v = r / t
Hypernovae can be very bright
GRB 980425 and SN 1998bw
spatial & temporal coincideneGalama et al. 1998, 1999
Kulkarni et al. 1998
Iwamoto et al. 1998
perculiar GRB
very low Eiso
~ 1048ergs
Spectra and LCs of SN 1998bw
1-D model of SN 1998bw
Mej~10-11Msun
EK~3-5 1052ergs
M(56Ni)~0.3-0.6Msun
MMS~35-45Msun
Iwamoto et al. 1998 NatureNakamura et al. 2001 ApJMaeda, Mazzali, Deng et al. 2003 ApJ
GRB 030329 and SN 2003dh
Stanek et al. 2003
Hjorth et al. 2003
Matheson et al. 2003
1-D model of SN 2003dh
Mazzali, Deng, et al. 2003 ApJLKawabata, Deng, et al. 2003 ApJLDeng et al. 2005 ApJ
Mej~7+/-3Msun
EK~3.5+/-1.5 1052ergs
M(56Ni)~0.3-0.55Msun
MMS~25-40Msun
GRB 031203 and SN 2003lw
Mej~11-15MsunEK~6+/2 1052ergs
M(56Ni)~0.6-0.9Msun
MMS~40-50MsunMazzali, Deng et al. 2005 in preparation
Malesani et al. 2004Thomsen et al. 2004Gal-Yam et al. 2004
Collapsar model
14M☉He star (MZAMS=45M☉) 15.6s
MacFadyen & Woosley 1999
15M☉He star Einit=1.4 1052ergs 7.2s Zhang, Woosley & MacFadyen 2003
Fe
O
2-D features in nebular spectraSN 1998bw: Fe lines broader than O lines
56Fe
16O
56Fe
16
O
Orientation 15 deg
Maeda et al. 2002 ApJLMaeda et al. 2005 ApJ submitted
SN 2003jd: a HN viewed edge-on
Mazzali et al. 2005 Science
More [O I] profiles of SNe Ibc
SN 1997ef and 1997dq
Iwamoto et al. 2000 ApJMazalli et al. 2000 ApJMazalli, Deng et al. 2004 ApJ
MMS ~ 25-30Msun
EK~1-2 1052ergs
M(56Ni)~0.14-0.2Msun
SN 2002ap: low-energy end of HNe
Mazalli, Deng et al. 2002 ApJLDeng et al. 2005 in preparation
MMS ~ 20-25sun
EK~0.4-1 1052ergs
M(56Ni)~0.08+/-0.01Msun
SN 1999as: the brightest SN
~2－ 5 Msun 56Ni!
Deng et al. 2001-2005 in preparation
MMS ~ 60-80MsunEK~25+/5 1052ergs
E ~ MMS of SNe and HNe
M(56Ni) ~ MMS of SNe and HNe
Open Questions• physical parameters in 2-D modelling
2-D spectrum and LC codes in development
• some HNe GRBs , other HNe notviewing angle? intrinsic parameters (M, E, …)?
• normal Type Ic SNe ? GRBs02lt/GRB021211 (Della Valle et al. 2003)?
XRF030723 (Tominaga, Deng et al. 2004 ApJL)? • Type Ib HNe? Type IIn HNe?
97cy & 99E (CSM-I. Ia Deng et al. 2004 ApJL)? 88Z (Aretxaga et al. 1999)?
• radio & X-ray obs.no relativistic off-axis jets in 97dq, 97ef, 02ap, 03jd? (Soder
berg et al. 2005)
