ASTR 121 Lecture Notes - Lecture 3: Binary Star, Stellar Classification, Black-Body Radiation
1 Mar 2018
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Three traditional ways to identify a binary system: But we can also get doppler shifts pf pulsars. Combine kepler"s third law with mass balance to derive stellar masses sometimes individually: Find star masses range from >100 to . 08 &"( The individual masses can be found if you have: The relative speed of the stars and the barycenter of the stars (center of gravity) For main sequence life, mass determines fate of star. About half of all stars are in binary systems. At least 80-90% of the most massive ones are in binaries. For the most massive >10% are in complicated systems. One can show that if you can get the period p of an orbit and the maximum orbital speed you see from star 1 is k1, then for inclination i. Star that we can directly observe motion of. We can determine the orbit by measuring the doppler shifts.
