51) Because they all involve the detonation of a carbon-rich : 1828917
51) Because they all involve the detonation of a carbon-rich white dwarf at the Chandrasekhar limit, all Type I supernovae are approximately equally luminous.
52) The number of Type I and Type II supernovae observed are approximately equal.
53) Neutrinos can move faster than c, the speed of light, as was discovered in SN1987A in 1987.
54) Novae are more closely related to Type II than to Type I supernovae.
55) If a white dwarf gains enough mass from a nearby star to exceed its Chandrasekhar limit it will become a nova.
56) A carbon-detonation supernova starts out as a white dwarf in a close binary system.
57) Most of the energy released during a supernova is emitted as neutrinos.
58) Type II supernova spectra are poor in hydrogen because stars that explode this way use up all their hydrogen before they leave the main sequence.
59) Novae and Type II supernovae are essentially the same phenomena.
60) A 100 million-year-old open cluster will no longer contain any O-type stars.
61) Globular clusters are dominated by bright red supergiants at the top right of the H-R diagram.
62) The blue stragglers represent the horizontal branch for globular clusters.
63) Blue stragglers are among the first stars formed in a cluster.
64) Supernova 1987A matched the theoretical predictions for Type I supernovae well.
65) The spectra of the oldest stars show the most heavy elements.