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12-Supernovae (Type 1a (Intermediate mass elements (Si, Ca,Mg,S.O) near…

- - - - more massive star in a binary system evolves to a white dwarf, which accretes mass from its companion (main sequence or red giant)
      - Difficult to tune accretion so that a classical nova doesn't happen, blowing off more mass than has been accreted
    - - Two white dwarfs in binary lose energy by grav radiation and spiral inward to coalesce
  - - - Burning proceeds as supersonic shock wave, not allowing unburnt material time to expand before being consumed
      - tends to convert whole star to Ni-64
      - not observed, therefore disfavoured
    - - burning front moves outward subsonically, producing complex turbulent boundary layer propagating outward
      - not certain that this can generate an explosion
    - - Initial deflagration converts to detonation as it propagates into lower density regions
      - defo does explode, is the preferred scenario
- - - - 1a
        
        typical
        
        nuclear explosion of low mass star
        
        reproducible light curve
        
        Insignificant neutrinos
        
        no compact remnant
      - 1ax
        
        Fainter, lower ejecta velocity, no 2nd max in IR
      - 27%
    - - Strong He features
        
        1b
        
        7%
      - No/weak He
        
        1c
        
        14%
  - - - IIb
        
        4%
    - - II-P
        
        plateau in light curve
        
        43%
      - II-L
        
        linear decline
        
        2%
      - IIn
        
        Narrow lines
        
        3%