ASTR-1010 Lecture Notes - Lecture 4: Photosphere, Chromosphere, Electromagnetism
6 Oct 2016
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Document Summary
The sun is 70% hydrogen: 28% helium, 0. 8% oxygen, 0. 3% carbon, 0. 2% iron, trace amounts of anything else, hydrogen and helium are the most important to remember. We know the composition of the sun by identifying the absorption lines in the. Sun"s spectrum: these absorption lines are formed in the photosphere (sun"s atmosphere) Sun: the inner layers are the: core. This is where the sun"s energy is generated. T=1. 5 x 10^7 = 15,000,000 k: radiative zone. Interior zone 1: energy is transported from core to surface: convection zone. Interior zones 1: energy is transported from core to surface. Sun: the outer layers are the: photosphere. This is the yellow surface" that we see. Where the energy is released: chromosphere. A thin layer above the photosphere where most of the sun"s uv light is emitted. Part of the sun that produce the uv rays that can be dangerous: corona. The hot, ionized gas which surrounds the sun.
