1. Observational Properties and Modelling of Hypernovae Jinsong Deng National Astronomical Observatories of China Collaborators: P. A. Mazzali (Trieste Obs. & MPA) K. Nomoto, K. Maeda (Tokyo Univ.) et al. DARK ENERGY D EN G

2. What are hypernovae? Why the studies? hyper-energetic supernovae (HNe) ~10 52 ergs or bigger (normal SN: ~10 51 ergs) 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 supernovae core-collapse SNe, massive CO stars some are related to gamma-ray bursts the origins of long GRBs

3. Hypernovae are characterized by very broad spectral lines very borad lines  high ejecta velocities (~10 4 -10 5 km/s)  large kinetic energy (~10 52 ergs)  hypernovae relatively narrow lines  low ejecta velocities (~10 3 -10 4 km/s)  normal kinetic energy (~10 51 ergs)  normal supernovae v = r / t

5. Hypernovae can be very bright

6. GRB 980425 and SN 1998bw spatial & temporal coincidene Galama et al. 1998, 1999 Kulkarni et al. 1998 Iwamoto et al. 1998 perculiar GRB very low E  iso  ~ 10 48 ergs

7. Spectra and LCs of SN 1998bw

8. 1-D model of SN 1998bw M ej ~10-11Msun E K ~3-5 10 52 ergs M( 56 Ni)~0.3-0.6Msun  M MS ~35-45Msun Iwamoto et al. 1998 Nature Nakamura et al. 2001 ApJ Maeda, Mazzali, Deng et al. 2003 ApJ

9. GRB 030329 and SN 2003dh Stanek et al. 2003 Hjorth et al. 2003 Matheson et al. 2003

10. 1-D model of SN 2003dh Mazzali, Deng, et al. 2003 ApJL Kawabata, Deng, et al. 2003 ApJL Deng et al. 2005 ApJ M ej ~7+/-3Msun E K ~3.5+/-1.5 10 52 ergs M( 56 Ni)~0.3-0.55Msun  M MS ~25-40Msun

11. GRB 031203 and SN 2003lw M ej ~11-15Msun E K ~6+/2 10 52 ergs M( 56 Ni)~0.6-0.9Msun  M MS ~40-50Msun Mazzali, Deng et al. 2005 in preparation Malesani et al. 2004 Thomsen et al. 2004 Gal-Yam et al. 2004

12. Collapsar model 14M ☉ He star (M ZAMS =45M ☉ ) 15.6s MacFadyen & Woosley 1999 15M ☉ He star E init =1.4 10 52 ergs 7.2s Zhang, Woosley & MacFadyen 2003

13. Fe O 2-D features in nebular spectra SN 1998bw: Fe lines broader than O lines 56 Fe 16 O 56 F e 16 O Orientation 15 deg Maeda et al. 2002 ApJL Maeda et al. 2005 ApJ submitted

14. SN 2003jd: a HN viewed edge-on Mazzali et al. 2005 Science

15. More [O I] profiles of SNe Ibc

16. SN 1997ef and 1997dq Iwamoto et al. 2000 ApJ Mazalli et al. 2000 ApJ Mazalli, Deng et al. 2004 ApJ M MS ~ 25-30Msun E K ~1-2 10 52 ergs M( 56 Ni)~0.14-0.2Msun

17. SN 2002ap: low-energy end of HNe Mazalli, Deng et al. 2002 ApJL Deng et al. 2005 in preparation M MS ~ 20-25sun E K ~0.4-1 10 52 ergs M( 56 Ni)~0.08+/-0.01Msun

18. SN 1999as: the brightest SN ~2 － 5 Msun 56 Ni! Deng et al. 2001-2005 in preparation M MS ~ 60-80Msun E K ~25+/5 10 52 ergs

19. E ~ M MS of SNe and HNe

20. M( 56 Ni) ~ M MS of SNe and HNe

21. Open Questions physical parameters in 2-D modelling 2-D spectrum and LC codes in development some HNe  GRBs, other HNe not viewing angle? intrinsic parameters (M, E, …)? normal Type Ic SNe  ?  GRBs 02lt/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? ( Soderberg et al. 2005 )