Astrophysics of Life

Get temperature by comparing b v color to theoretical

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Get temperature by comparing B-V color to theoretical blackbody curve Stellar Temperature: Spectra 7 stars with same chemical composition Temperature affects strength of absorption lines Example: Hydrogen lines are relatively weak in the hottest star because it is mostly ionized. Conversely, hotter temperatures are needed to excite and ionize Helium so these lines are strongest in the hottest star. Spectral Classification: Before astronomers knew much about stars, they classified them based on the strength of observed absorption lines. Classification by line strength started as A, B, C, D, . . . , but became: O, B, A, F, G, K, M, (L) A temperature sequence! Cannon’s system officially adopted in 1910 “Oh be a fine girl/guy kiss me” “Oh brother, astronomers frequently give killer midterms” Stellar sizes: Almost all stars are so small they appear only as a point of light in the largest telescopes A small number are big and close enough to determine their sizes directly through geometry F = o~ T^4 L = 4piR^2 o~ T^4 Stellar size: indirect measurement Stars have a huge range of sizes
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Stefan’s Law: F = o~ T^4 Luminosity is the flux multiplied by entire spherical surface Area of sphere A = 4piR^2 Luminosity = 4piR^2 o~ T^4 or L infinity R^2 x T^4 Hertzsprung-Russell (HR) Diagram HR diagrams plot stars as a function of their luminosity and temperature About 90% of all stars (including the Sun) lie on the Main Sequence . . . where stars reside during their core Hydrogen-burning phase Parallax | | (eyes) The closer your finger is to you, the bigger the angular shift is d = 1pc or (3 LY) parcet – amount of shift The HR Diagram: 100 Brightest Stars Most of these luminous stars are somewhat rare – they lie beyond 5pc We see almost no red dwarfs (even though they are very abundant in the universe)
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Get temperature by comparing B V color to theoretical...

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