ASTRON 1F03 Lecture Notes - Lecture 9: Solar Transition Region, Helioseismology, Chromosphere
12 Mar 2018
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Can be calculated by its fraction that reaches. The sun is in perfect hydrostatic equilibrium: the internal pressure due to colliding molecules are equal to the force of gravity pushing on the outside. Since the sun"s mass it"s huge, the fact that it does not collapse implies that the internal temperature is extremely high=> more kinetic e=> more collisions=> more internal pressure. Analysis of doppler shifts reveals that the surface oscillates and vibrates=> Helioseismology allows us to gather info on the internal structure of the sun. The visible light we see from our sun is emitted by the photosphere. Spectral analysis reveals the different elements that make up photosphere and chromosphere. Solar corona can be seen if both the photosphere and the chromosphere are covered. It is made uo of very highly ionized elements. The solar transition region is a region of the sun"s atmosphere, between the chromosphere and corona. Here the temperature rises sharply to 1 mil k, and.
