II. Three Modes of Energy Transport in the Suna. Outside of the core are two zones because they transport energy differentlyi. Radiation: energy transported through vacuum, EM waves are carrying that energyii. Convection: mass motions of gas transport energy1. Granulation: convective mode of transporta. Granules are convection cells about 1000 km wideb. Rising hot gas produces these granules, cooler gas sinks downward and this gas glows less brightlyc. You also see super granulesi. Blue: areas of rising gasii. Red: areas of sinking gasiii. Conduction occurs in a metal or a solid where the heat is making atoms “jiggle”1. Third mode of energy transportIII. The Sun is in hydrostatic and thermal equilibriuma. Hydrostaticequilibrium: pressure out and gravity in are equal.b. Thermalequilibrium: the temperature is very stable. It does not change drastically. If there is an increase in T in the core, then pressure will increase (higher T, means higher P) so in doing so, more energy can escape, and once it does it will settle back down againIV. Probing the Sun’s interiora. Modes of vibration depends on the material that is vibratingi. Similar observation on vibration modes of the Sunii. Anything that happens on surface is result of what’s going on insideV. The Photosphere:a. The surface that we SEEb. Looks yellowi. The edge of the sun appears a little dimmer because the outer layers of the Sun are a bit cooler (cooler and cooler as you go outc. Sun appears darker around its limbVI. Sunspotsa. Darkest part of the sunspot: umbra (red of EM spectrum)i. Lightest part: penumbraii. They occur because of the magnetic field on the Suniii. We can detect the magnetic field in the Suniv. If you were to take a sunspot and put it out in space, it would still glow orangeb. Sunspots come and go: sunspot cyclec. Sun rotates faster at its equator than at its polesi. Differential rotationii. 25 day rotationd. The cause of solar flaresi. As Sun spins, it takes magnetic field along with it and things get tangled up to the point that it wraps around itselfii. Sunspots ALWAYS come in pairs!ASTRON 89 1st Edition Lecture 14Outline of Last Lecture I. Converting H to He II. Definitions Outline of Current Lecture I. Helium is made in the Core II. Three Modes of Energy Transport in the Sun III. The Sun is in Hydrostatic and Thermal EquilibriumIV. Probing the Sun’s Interior V. The Photosphere VI. Sunspots Current LectureI. Helium is made in the Core a. Sun is basically made up of Hydrogen. When its really hot, the electrons are swimming around freely and it’s so hot that they don’t form an atom. b. But T goes down as you go from core to surface. Once its cool enough, electron and proton are now together, and all of the sudden, it jumps to another level. So atoms in the outer layers have absorbed energy that came from the inside, whichcauses them to move. c. Once energy is generated in core, gamma rays stream right through the inner part of the sun (pure radiation). Then they come to a point where it’s a little bit cooler, those atoms grab energy coming at it and begin to moveII. Three Modes of Energy Transport in the Suna. Outside of the core are two zones because they transport energy differentlyi. Radiation: energy transported through vacuum, EM waves are carrying that energyii. Convection: mass motions of gas transport energy1. Granulation: convective mode of transport a. Granules are convection cells about 1000 km wideb. Rising hot gas produces these granules, cooler gas sinks downward and this gas glows less brightlyc. You also see super granulesThese notes represent a detailed interpretation of the professor’s lecture. GradeBuddy is best used as a supplement to your own notes, not as a substitute.i. Blue: areas of rising gasii. Red: areas of sinking gasiii. Conduction occurs in a metal or a solid where the heat is making atoms “jiggle”1. Third mode of energy transport III. The Sun is in hydrostatic and thermal equilibriuma. Hydrostaticequilibrium: pressure out and gravity in are equal. b. Thermalequilibrium: the temperature is very stable. It does not change drastically. If there is an increase in T in the core, then pressure will increase (higher T, means higher P) so in doing so, more energy can escape, and once it does it will settle back down againIV. Probing the Sun’s interiora. Modes of vibration depends on the material that is vibrating i. Similar observation on vibration modes of the Sunii. Anything that happens on surface is result of what’s going on insideV. The Photosphere: a. The surface that we SEEb. Looks yellow i. The edge of the sun appears a little dimmer because the outer layers of the Sun are a bit cooler (cooler and cooler as you go outc. Sun appears darker around its limbVI. Sunspotsa. Darkest part of the sunspot: umbra (red of EM spectrum)i. Lightest part: penumbraii. They occur because of the magnetic field on the Sun iii. We can detect the magnetic field in the Sun iv. If you were to take a sunspot and put it out in space, it would still glow orangeb. Sunspots come and go: sunspot cyclec. Sun rotates faster at its equator than at its poles i. Differential rotation ii. 25 day rotation d. The cause of solar flares i. As Sun spins, it takes magnetic field along with it and things get tangled up to the point that it wraps around itself ii. Sunspots ALWAYS come in