00:01
The rate at which a red giant in a binary system transfers mass onto a white dwarf is what i call r.
00:07
This is the rate, and it's 10 to the minus nine solar masses per year.
00:11
So the time taken by the white dwarf to become supernova with a given amount of required mass, m, so the time is t and it's equal to the mass divided by the rate.
00:22
So it is clear that the red giant would require 10 to the nine years for transferring mass onto its companion white dwarf and making it into one.
00:30
Solar mass star based on this rate.
00:32
For a white dwarf to become a supernova, it should have a mass of the shangar -shankar limit of 1 .44 times the solar masses.
00:39
So if the white dwarf mass starts at 0 .6 solar masses, then the mass required for the white dwarf to become supernova, m, is equal to the shandar -shakar limit of 1 .44 solar masses minus the current mass.
00:54
So this is 1 .44, m -solar minus the current mass of the star, which we're told is 0 .6 m -solar...