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Phys320_L15.pdf - Lecture 15 Introduction to the Sun Jiong...

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Introduction to the SunLecture 15Jiong Qiu,MSUPhysics Department
Open Q: what physics do we learn about the Sun?1.Energy- nuclear energy- magnetic energy2.Radiation- continuum and line emissions;- particle radiation- other effects;3.Magnetism:- origin- energy build-up- energy release4.Observing techniques:- optical and infrared observation: adaptive optics- radio and X-ray technology
Guiding Questions1.What is the source of the Suns energy?2.What is the internal structure of the Sun?3.How can astronomers measure the properties of theSun’s interior?4.How can we be sure that thermonuclear reactionsare happening in the Sun’s core?5.What is the standard solar model? How is it built?What are the observational tests it has survived?
14.1 IntroductionOur star, the Sun, is a hotplasmaball. It is an average star interms of its mass, size, temperature, composition, and evolution.Similar to JupiterQ:L = ??
Ex.1: spectroscopicobservations of the Sun:numerous absorptionlines superimposed on thecontinuum.Q: what produces thecontinuum? How to findthe surface temperatureof the Sun? Whatproduces the absorptionlines?
Ex.2: the Suns positionin the H-R diagram as anaverage main sequencestar.A main sequence star:- Same chemicalcomposition: 75% hydrogenand 25% helium);- Fueled by thermonuclearreaction;- Lie in the H-R diagramH-R diagram: a starsluminosity (brightness)versus its temperature(color)L=4πR2σT4Mass determines all.

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Term
Fall
Professor
Rettig

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