Online Astronomy Solar System Homework Help
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1. At one time, the protostar that became our Sun had a surface temperature of about 3000K and a radius about 25 times that of the present-day Sun. How much more (or less) luminous, compared to today, was our Sun when it was a protostar? At what distance would you have to be from the protostar for it to have the same brightness as the Sun seen from Earth today?
2. In the 19th century there was much discussion about what could be the energy source of the Sun. Why was it evident that the Sun could not be powered by chemical reactions? Kelvin and Helmholtz thought they had the answer. What was their idea and what 19th century evidence showed that they were wrong?
3.Describe the complete life cycle of the Sun and plot it on an HR diagram. What is a planetary nebula? What process gives rise to such a nebula? What typically lies at the center of a planetary nebula?
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4.What is the mass deficit in nuclear reactions? Where does the mass go? Which elements can fuse together to generate energy and why is iron considered to be the most stable element? Why do thermonuclear reactions occur only in the Sun’s core, and not in the outer parts of the Sun? Why is it more difficult to fuse two helium nuclei than it is to fuse two hydrogen nuclei?
5.Sketch a Hertzsprung-Russell diagram: label the axes, marking off the scales. Indicate the regions on your diagram occupied by main sequence stars, red giants, supergiants, the Sun. Discuss how the one can determine the radius of a star from its position on the Hertzsprung-Russell diagram – you need not go into great mathematical detail, a short outline of the ideas will suffice.
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