An Introduction to Supernovae - LUTH

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$J. Phys. A: Math. Gen. 32 (1999) - LUTH - Observatoire de Paris$

Further evidence for non-spherical core collapse supernova explosions ● indirect: ● - large pulsar velocities - association with long GRBs - asymmetries in late-time emission-line profiles of SNe Ic ● direct: ● - spectropolarimetry of SNe Ic & ● SNe II-P (SN2004dj, 3.1Mpc; Leonhard et al. '06) ● ● ● ● ● ● ● ● ● ● ● ● Vela SNR: protrusions, fast pulsar ● progeni<strong>to</strong>r: super giant in compact star cluster (Sandage's star 96), ~12 M sol (Wang et al. '05)
Observing the Surface: CCSN length scale problem 30 000 000 km 15 km Blue Giant (Red Giant: × 100) × 20 000 × 100 Neutron star Fe-Ni core 1500 km
Page 1 and 2: An Introduction to Supernovae Ewald
Page 3 and 4: A New Star, as bright and as red as
Page 5 and 6: C h a n d ra : X -ra y c o m p o s
Page 7 and 8: • • Supernovae in the Milky Way
Page 9 and 10: - Supernova 1987A environment & rin
Page 11 and 12: angular size: ~ 8 o (ie. ~16 x size
Page 13 and 14: credit: W.P.Blair (John Hopkins Uni
Page 15 and 16: ESO-VLT: NGC 6118 & SN2004dk ( d ~
Page 17 and 18: SN 1993J in M81 (d = 3.7 Mpc) Evolu
Page 19 and 20: Close-up of SN 1993J explosion site
Page 21 and 22: T y p e Ia s u p e rn o va a t z =
Page 23 and 24: Supernova light curves pronounced m
Page 25 and 26: Number of supernovae per year as fu
Page 27 and 28: • • energy sources for a supern
Page 29: • • • Importance of Supernova
Page 32 and 33: • • Observational evidence for
Page 36 and 37: ● Looking into the heart of a cor
Page 38 and 39: ● Looking into the heart of a cor
Page 40 and 41: Gravitational radiation - leading-o

An Introduction to Supernovae - LUTH

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