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)