a plot of luminostiy against temp (or spectral class) for a group of stars
the amount of energy per second per unit area recieved from a star
how bright a star is
inverse square law
flux=luminosity/area of sphere
apparent shift in position of object when viewed from 2 points
1/60 of an arcminute
1/60 of one degree
parallax secons, 3.262 lightyears
apparent brightness of a star, expressed using the magnitude scale
apparent magnitude a star would have if placed at standard distance 10 parsecs from earth
difference between apparent and absolute magnitude. equivilent to distance by the inverse-square law
bulk of stars
below main sequence, hot but dim
above main sequence, bright but cool
small, cool, faint star, lower right end of the HR diagram
groups stars according to the width of their spectral lines (giants vs. dwarfs)
observational bias in which a measured property of a collection of objects is due to the way in which the easurement was made, rather than being intrinsic to the objects themselves
mthod of determining the distance to a star by measuring its temp and then determining its absolute and apparent brightness of the star's distance from earth
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