Lecture 22: The Cosmic Distance Problem
Update: 2006-02-06
Description
How do we measure distances to astronomical objects that are too far
away to use Trigonometric Parallaxes? This first lecture of Unit 4
reviews geometric methods like trigonometric parallaxes, and then
introduces the idea of Standard Candles, and how they are used to
develop methods for deriving Luminosity Distances based on the Inverse
Square Law of Brightness. We will explore three luminosity-based
distance methods useful for studying our Galaxy and nearby galaxies:
Spectroscopic Parallaxes, Cepheid Variable Period-Luminosity Relation,
and the RR Lyrae P-L Relation. Recorded 2006 February 6 in 1008 Evans
Laboratory on the Columbus campus of The Ohio State University.
away to use Trigonometric Parallaxes? This first lecture of Unit 4
reviews geometric methods like trigonometric parallaxes, and then
introduces the idea of Standard Candles, and how they are used to
develop methods for deriving Luminosity Distances based on the Inverse
Square Law of Brightness. We will explore three luminosity-based
distance methods useful for studying our Galaxy and nearby galaxies:
Spectroscopic Parallaxes, Cepheid Variable Period-Luminosity Relation,
and the RR Lyrae P-L Relation. Recorded 2006 February 6 in 1008 Evans
Laboratory on the Columbus campus of The Ohio State University.
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