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. Chapters 10.1-10.4; 11.1 Lectures Sept. 11, 16. Exam is Sept 18 (Thursday) Conventional requirements for habitability P lanet -- dif 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 . The processes by which stars and planets form are active areas of research in modern astrophysics. The formation of our own solar system is central to the first half of our course, and important to the second half as well when we study the formation of stars. Go to the Physics and Astronomy Department website.. www.pa.uky.edu. Click on “. Online Course Evaluation. ” link. Link is open now. Do it soon.. The nearest stars to the Sun.. Barnard’s Star. 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. a. nd stellar multiplicity. Insights from recent surveys. Gaspard . Duchêne. (UC Berkeley, Obs. Grenoble). © NASA/JPL/Caltech. Planets in multiple systems?. © . LucasFilm. Ltd.. They must exist!. Exam on Monday. I’ll have a Mock exam to work on Friday. Solar Eclipse. Freds_excellent_eclipse.mpg. Solar Eclipses . Umbra. – region of total shadow. Penumbra. – region of partial shadow. Totality lasts only a few minutes!. 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. Ninth Edition. Neil F. Comins • William J. Kaufmann III. CHAPTER 5. Formation of the Solar System. and Other Planetary Systems. A montage of the planets in our solar system presented in correct relative sizes. The orbits in the background are also drawn to scale.. ’. s first mission to detect Earth-size planets orbiting in the habitable zone of Sun-like stars.. NASA. ’. s Kepler and . K2 Missions: . 1030 confirmed exoplanets. (as of July . 2015). How many Earths?. Insights from recent surveys. Gaspard . Duchêne. (UC Berkeley, Obs. Grenoble). © NASA/JPL/Caltech. Planets in multiple systems?. © . LucasFilm. Ltd.. They must exist!. Planets in multiple systems!. Learn planetary characteristics such as number of moons, size, composition, type of atmosphere, gravity, temperature and surface features.. Understand the movement of planetary bodies.. Understand which planetary characteristics are more important than others when it relates to our understanding of other worlds. . 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.