Supernova PHYS390 Astrophysics Professor Lee Carkner Lecture 16
High Mass Stars Variability and mass loss Produce heavy elements in cores Which produces even heavier elements
Luminous Blue Variables T ~ K, L ~ 10 6 L sun Occupy an instability zone on the HR diagram What accounts for mass loss and variability? Pulsation Rapid rotation
Wolf-Rayet Stars Hot, bright stars with rapid rotation and mass loss Have strong emissions lines of different elements WN: He and N WC: He and C from triple alpha WO: O from C + He burning
High Mass Evolution High mass stars go through more post- MS stages compared to low mass stars Can end up in a Wolfe-Rayet stage where outer layers are stripped away End in supernova instead of PN stage
Types of Supernovae A point source that get brighter A supernova is a very bright nova Accretion onto white dwarf causing core collapse (Type Ia) Core collapse of high mass star (Type Ib, Ic, and II)
Classification Type I have no H lines Must be from stars that have lost their outer layers Type Ib have strong He Type II have strong H Type II-P have a plateau in the light curve Type II-L have a more rapid drop off
Core Collapse Excluding the Type Ia, we can refer to the rest as core collapse supernova Generates about J of energy mostly in the form of neutrinos
The Core Lighter on outside, heavier towards middle As the fusion products move towards iron, the energy released per nuclei decreases Iron can’t be burned, so star can’t stay in HSE
Core Processes Produces protons T and P are also high enough that the protons can fuse with electrons, producing neutrons Core’s ability to support outer layers drops rapidly Removing electrons decreases electron degeneracy pressure
Explosion hard to do This causes the collapse to rebound and send a shock wave out A neutrinosphere forms behind the shock The shock front is so dense it can absorb neutrinos to power the shock back out about billion suns
Supernova 1987A Located in a Milky Way satellite called the Large Magellanic Cloud Progenitor was 12 th magnitude blue supergiant mass ~ 20 M sun
End Products If initial star was smaller than about 35 M sun, core will form a neutron star Else it will form a black hole Can produce strong synchrotron emission from high velocity electrons spiraling around magnetic field lines Remnant can also collide with ISM causing emission and triggering star formation
Radioactive Decay The decay of these isotopes add energy to the supernova and effect the shape of the light curve Most important reaction is 56 Ni decaying to 56 Co and then 56 Fe With half life of 6.1 days and 77.7 days
Half-Life How much energy is released by decay? Decay goes as: N(t) = N 0 e - t Where N 0 is the initial number of atoms and N is the number at some time t = (ln 2)/ 1/2 where 1/2 is the half-life (time for ½ of atoms to decay)
Light Curve Slope The magnitude of the supernova is proportional to dM bol /dt = For example supernova 1987A has a light curve after 200 days well matched by 56 Co and 57 Co
Elemental Abundances H and He are the most plentiful Li, Be, B underabundant Some elements (C, O, Ne, …) are abundant because the are created in post-main sequence stars Fe created in supernovae cores
Next Time Read Homework: 16.1b,c,d, 16.4