ASTR 1P01 Lecture Notes - Lecture 18: Electron Neutrino, Positron, Deuterium

• School: Brock University
• Department: Astronomy
• Course: ASTR 1P01
• Professor: Bozidar Mitrovic

Document Summary

First, like all main sequence stars, the sun is in hydrostatic equilibrium. The pressure in the core region must be tremendous to support the weight of the top layers: high pressure (p) in the core region is produced by high temperature (t): High temperature in the core implies high energy production in the core region. Only fusion of light nuclei (h) into heavier ones (he) with a release of energy can produce enough energy to create the temperature and pressure needed to support the top layers of the. In the sun and other stars with masses the fusion of hydrogen into. 10-15m: since the protons repel (like charges always repel) they have to move fast enough to get that close to each other, thus, the fusion will not begin if the temperature is not at least 10 million. Kelvin (the temperature measures the average speed of the constituent particles)