ASTR-1010 Lecture Notes - Lecture 12: Chromosphere, Heat Transfer, Photosphere

• School: Vanderbilt University
• Department: Astronomy
• Course: ASTR-1010
• Professor: Stassun Keivan

Document Summary

Need to k(cid:374)o(cid:449) the (cid:396)ele(cid:448)a(cid:374)t fo(cid:396)(cid:373)ulas, (cid:271)ut you do(cid:374)"t (cid:374)eed to a(cid:272)tually (cid:373)e(cid:373)o(cid:396)ize the fo(cid:396)(cid:373)ulas. Short answer is similar to the hw questions. Refers to the microscopic nuclear process by which the sun generates its heat, and how simple h atoms are transformed into he atoms. The influences the sun has on its surroundings. Takes about 1 million years for energy to travel from the core to the surface. Sunspots: dark spots on the surface where the temperature is cooler: aka a cooler opaque object radiates less total energy. Granulation: the tops of conve(cid:272)tio(cid:374) (cid:272)ells see(cid:374) (cid:862)(cid:271)u(cid:271)(cid:271)li(cid:374)g(cid:863) o(cid:374) the ola(cid:396) su(cid:396)fa(cid:272)e. Sunspots occur in pairs; the pairs cluster into groups; and they rotate with the sun: by occurring in pairs, we can map them in a manner that indicates magnetic properties. Manifestation of the su(cid:374)"s (cid:373)ag(cid:374)eti(cid:272) p(cid:396)ope(cid:396)ties: the su(cid:374)"s (cid:373)ag(cid:374)eti(cid:272) field (cid:272)a(cid:374) poke out, (cid:272)ausi(cid:374)g pa(cid:396)ts of the su(cid:396)fa(cid:272)e to (cid:271)e (cid:373)u(cid:272)h (cid:272)oole(cid:396)