AST201H1 Lecture Notes - Lecture 1: Exotic Matter, Type Ia Supernova, Supermassive Black Hole

• School: UTSG
• Department: Astronomy & Astrophysics
• Course: AST201H1
• Professor: Bryan Gaensler

Document Summary

Estimate the age of a star cluster by examining the h-r diagram of its members. Identify and name patterns or groupings of stars in the h-r diagram. Ta(cid:396)(cid:859)s lu(cid:373)i(cid:374)osit(cid:455) (cid:272)lass a(cid:374)d (cid:272)ha(cid:396)a(cid:272)te(cid:396)isti(cid:272)s: supergiants (20 100 x size of sun) Large diameter = enormous luminosity (even though temperature is low) Near-final stage of stellar evolution: not burning hydrogen, main sequence stars. Sequence of mass: measuring their orbits lets us determine their mass (solar masses, white dwarfs. Tiny stars (around same diameter as earth) Same diameter = very low luminosity: even though temperature is high. Final stage of stellar evolution: no fusion taking place, just residual heat from earlier stages. Very common, last for billions of years. Disti(cid:374)guish (cid:271)et(cid:449)ee(cid:374) a sta(cid:396)(cid:859)s lu(cid:373)i(cid:374)osit(cid:455) a(cid:374)d lu(cid:373)i(cid:374)osit(cid:455) (cid:272)lass: smaller stars. Lower luminosity: because of small surface area, even if temperature is high, bigger stars. Higher luminosity: because of large surface area, even if temperature is low.