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Lecture

Astronomy - Tutorial #8.

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Department
Astronomy
Course
ASTA02H3
Professor
Parandis Khavari
Semester
Winter

Description
Astronomy - Tutorial #8.  every main-sequence star  fuses Hydrogen to make Helium to sustain it  until it collapses   mass divided by luminosity  determines how long the star will last    note that any equality for the purpose of this course can be viewed as a proportionality   is a constant   cross out the constant for  mass-luminosity relationship  two more lifetime relationships  note that and are constants of proportionality     cross outand it becomes   replace with  main-sequence stars  (luminosity of the star )s  and  ( )  answer is 0.21   equations that will not be provided on the exam       distance of the Sun to the center of the galaxy is 800kpc  giants  red  have H-shell burning  inert core  yellow  H-shell burning  He core burning   turning of its gravitational energy to heat   red giant  inert core, Hydrogen shell burning  still contracting   luminosity increases  temperature drops  cools down     as the red giant expands, the core is still collapsing  two sources of energy  gravitational energy  H-shell burning  luminosity depends on two things  the more luminous a blackbody is, the lower its temperature will be  red giants  as a rule, are more luminous than the Sun  te
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