INAF The advanced evolutionary phases of the massive stars and their explosive yields Alessandro Chieffi Istituto Nazionale di AstroFisica (Istituto di Astrofisica Spaziale e Fisica Cosmica) & Centre for Stellar and Planetary Astrophysics – Monash University - Australia INAF JINA workshop on Massive Stellar Progenitors: "The Final Days of Burning" March 9-10, 2006, Santa Barbara

INAF SOLAR DISTRIBUTION Core collapse supernovae Intermediate mass stars and core collapse supernovae Core collapse and thermonuclear supernovae Intermediate mass stars and core collapse supernovae

INAF r r1r1 T1T1 BASIC PROPERTIES OF THE SHOCK WAVE: Fe core RADIATION DOMINATED: ADIABATIC EXPANSION: r2r2 T2T2 The peak temperature of the blast wave does not depend on the stellar structure CONSEQUENCE: A simple but quite effective computation of the explosive yields may be obtained by assuming:

INAF NSE QSE 2QSE Sc Ti Fe Co Ni V Cr Mn Ti Fe Si S Ar Ca Si S Ar Ca K Ne Na Mg Al P Cl f(,T,Y e ) f(,T,X i )

INAF H burning Monoparametric sequence of models CNO Cycle

INAF He burning Monoparametric sequence of models 3 C

INAF C burning NOT a monoparametric sequence of models any more 12 C ( 12 C, p ) 23 Na 12 C ( 12 C, ) 20 Ne ( p, ) 20 Ne 16 O ( ) 20 Ne

INAF C burning

INAF C burning

INAF Ne burning 20 Ne (, ) 16 O NOT a monoparametric sequence of models O burning 16 O ( 16 O, p ) 31 P( p, ) 28 Si (, ) 32 S 16 O ( 16 O, ) 28 Si 16 O ( 16 O, n ) 31 S( + ) 31 P

INAF a ( b, c ) d Beyond O burning d ( c, b ) a

INAF

1 Year before the explosion 1 month before the explosion 1 day before the explosion Begin of the core collapse 11 M O 1 year before the explosion 1 month before the explosion 1 day before the explosion Begin of the core collapse 120 M O

INAF Thank You !

INAF

Basic core collapse scenario Fe core inner core pre SN star infalling matter outgoing shock from rebounce proto neutron star infalling outer core proto neutron star stalled shock neutrino heated layer revived shock matter flow gets reversed proto neutron star

INAF surface In spite of the many efforts, no successful explosion has been obtained yet Fe core Escamotage: Assume that a shock wave escapes the Fe core proto neutron star Since the explosion is not obtained naturally a few assumptions are unavoidable: 1) Energy deposited in the shock front 2) Time delay between c.c. and the escape of the shock front from the Fe core

INAF Three different tecniques have been used up to now: The piston (Woosley and coworkers) The thermal bomb (Nomoto and coworkers) The kinetic bomb (Limongi and Chieffi) surface Fe core proto neutron star shock front

INAF Ne ( 20 Ne) C s Ne x Na ( 23 Na) C s Ne x Mg ( 24 Mg) C s Ne x Al ( 27 Al) C s Ne x P ( 31 P) Ne x Cl 35 Cl(Ne x ) 37 Cl(C s Ne x ) Sc ( 45 Sc, 45 Ca) Si x (C s Ne x ) Ti ( 48 Cr) Si x (Si xi ) Fe ( 56 Ni 56 Fe 54 Fe) Si xi Si x Co ( 59 Ni) Si x Ni ( 58 Ni) Si x Si ( 28 Si) Si xi O x S ( 32 S) Si xi O x Ar ( 36 Ar) Si xi O x Ca ( 40 Ca) Si xi O x K ( 39 K) O x V ( 51 V) Si xi Cr ( 52 Fe) Si xi Mn ( 55 Fe 55 Co) Si xi PURE EXPLOSIVE ELEMENTS M-R relation electron density Ye Shock wave energy Mass cut Time delay (freeze out) HYDROSTATIC&EXPLOSIVE ELEMENTS He ( 4 He) H c,s He c,s C ( 12 C) He c,s C c,s N ( 14 N) H c,s He c,s O( 16 O) He c Ne s O x F ( 19 F) He s HYDROSTATIC ELEMENTS C shell properties 12 C(, ) 16 O Shock wave energy Convection 12 C(, ) 16 O

INAF 1 Year before the explosion 1 month before the explosion 1 day before the explosion Begin of the core collapse 11 M O

INAF 1 year before the explosion 1 month before the explosion 1 day before the explosion Begin of the core collapse 120 M O