Today in Astronomy 142 - Astro Pas Rochester

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The solar spectrumBy and large, the spectrum of theSun resembles closely a blackbody.From the total energy flux atEarth (solar constant):we get the Sun’s luminosity:Setting solar luminosity equal to blackbody power givesSun’s effective temperature:Astronomy 142 2
In detail:absorption linesare also seen inthe solarspectrum; theymatch up withmany knowntransitions ofatoms, ions andmolecules. (SeeLab #2.)The solar spectrum (continued)Figure: the ultimate high-resolution spectrum of the Sun (Nigel Sharp, fromdata by Bob Kurucz et al. ( NOAO/NSO/Kitt Peak FTS/AURA/NSF)Astronomy 142 3
Page 1: Today in Astronomy 142More on the S
Page 5 and 6: Radiation transportkeeping track of
Page 7 and 8: Mean free pathκopacity units g -1
Page 9 and 10: Opacity depends onwavelength becaus
Page 12 and 13: Solar “granulation:” the tops o
Page 14 and 15: Using Adaptive Optics to look at de
Page 16 and 17: Further out: the corona and chromos
Page 18 and 19: Sunspots: solar magnetismFigure: Ch
Page 20 and 21: Sunspot progress, activity during s
Page 22 and 23: 11-year sunspot cycle, for the last
Page 24 and 25: Sunspot formation and cycle: intera
Page 26 and 27: Cooling timescaleAstronomy 142 26
Page 28 and 29: Energy sources for the SunChemical
Page 30 and 31: Energy sources for the Sun (continu

Today in Astronomy 142 - Astro Pas Rochester

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