PPT-Lecture 3: Formation of Low Mass Stars and Planets

Neal Evans The University of Texas at Austin and KASI The Long and Winding Road Core to Star Disk The idea of a Core Some simple theory Evolutionary Stages and SED Classes Dense Cores Observations find regions of strongly enhanced density decreased turbulence. Richard B. . Larson. Yale University. Conclusions. Compact objects such as stars and black holes generally form in larger systems such as binaries, multiple systems, star clusters, or galaxies.. Gravitational interactions in these larger systems play a major role in the formation of compact objects by transporting angular momentum.. Galaxies. T.Naab. , P. Johansson, R. . Cen. , K. . Nagamine. , R. . Joung. . and J.P.O.. PPPL:, 19 Dec . 2012. ApJ.L.,. 658,710 . (2007) ApJ.,697, . 38 . (2009). ApJ.L.,699,L178 (. 2009. ). ApJ.,725,2312 . Lecture 7. By reading this chapter, you will . learn. 4-1. How ancient astronomers attempted to explain the motions of the planets. 4-2 . What led Copernicus to a Sun-centered model of planetary motion. Dr.. Jade Carter-Bond. (Lillian’s Daughter). U3A. 6 June, 2012. Extrasolar Planets:. What they are, what we know about them, why we should care, where ET lives (just kidding!) what I’ve been doing for the last 12 years and why your tax dollars should continue to help. Soprano I Hence  stars,  you  daz- zle but the sight,   you teach to Soprano II Hence  stars, \r \r \r Alto Hence  stars, hence   stars too  dim of light,  you  daz-  zle  b Lecture by C.P. Dullemond. Institute for Theoretical Astrophysics. Heidelberg University. Image . Credit. : NASA. The Big Questions. After C. Mordasini. > 10 billion galaxies in the Universe. 100 billion stars in each. Stars born with more than 8 — 10 M.  . cannot . lose enough mass to become white dwarfs. . These stars die by supernova explosions.. Ignition of “metals”. The core of an old high-mass star gets little . Stars, solar systems form within giant molecular clouds. Requires . high density. , . dust, and low temperatures. to initiate gravitational . collapse. Most material is hydrogen and helium; only a few percent is other elements. E.ST.05.21. Describe the motion of planets and moons in terms of. rotation on axis and . orbits.. Advanced Note-Taking Practice 101! . Every time you see something typed in . YELLOW. …you need to write it down. . Protoplanetary. disk: condensation and accretion. Solar wind (beginning of fusion). Collisions continue. Planetary migration (orbits shifting). Late Heavy Bombardment (Hadean Era). Planetary Evolution. 20.11. 1. Neutron stars. T. he . remains of cores of some massive stars that have become supernovae. .. Cores are . a degenerate gas of mostly neutrons.. So much compression at each stage of core contraction that final radius is . The end of the class. Assignments this week. Class evaluations for a 100% lab grade, due by weekend!. Canvas post-class assessment: one homework grade, due before final on Wednesday. Canvas . homeworks. Guidepost. In this chapter, you will consider how the interstellar medium condenses into stars and what the conditions inside stars must be like. How do stars form?. What is the evidence that stars are forming now?. Aristotle’s Astronomy (and enough physics to be getting along with). 9/19/13. 1. s. ome pictures of the cosmos. 9/19/13. 2. Celestial phenomena. Motion of the stars, motions of the sun. Look for the daily, or .