PPT-The Formation of Planets

Lecture by CP Dullemond Institute for Theoretical Astrophysics Heidelberg University Image Credit NASA The Big Questions After C Mordasini gt 10 billion galaxies in the Universe 100 billion stars in each. Extra-solar planetary systems. Lecture . 16. Other theory. Tidal Hypothesis. Early attempt to explain the dichotomy of planets.. Problem?. tidal force strong enough to “draw out” a filament from stars will effectively disperse it before it could condense into planets!. 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. Part 1. Survey of the solar system. 1. What do you know (or think you know)?. Confer with your tablemate (or people in front or back of you) and write down five things you think you know about our solar system. . Topic:. Resonances. Lecture by: C.P. Dullemond. Literature: Murray & Dermott „Solar System Dynamics“. What is a resonance?. A resonance is when two characteristic frequencies of a system match up. 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. Session 4 – The Nebular Theory. In the past few sessions we looked at the Big Bang theory and how it tries to explain the universe as a whole. Today we will look on a smaller scale of our solar system, and how the Big Bang theory explains (or doesn’t explain) the formation of the solar system. 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.. 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. Developed by . the SOFIA Team. 0. Topic: . Supernovae. Concepts: . Supernovae, planet formation, infrared observations. Mission: . SOFIA. Coordinated by: . the NASA Astrophysics Forum. An Instructor’s Guide for using the slide sets is available at the ASP website . 4.1 . The Search for Origins. Goals:. Where did the solar system come from?. How did it form?. When did it form?. What properties of our solar system must a formation theory explain? . Patterns of motion of the large bodies . Developed by . the SOFIA Team. 0. Topic: . Supernovae.. Concepts: . Supernovae, planet formation, infrared observations. Missionb. : . SOFIA. Coordinated by: . the NASA Astrophysics Forum. An Instructor’s Guide for using the slide sets is available at the ASP website . This work is protected by U.S. copyright laws and is provided solely for the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students except by instructors using the accompanying text in their classes. All recipients of this work are expected to abide by these restrictions and to honor the intended pedagogical purposes and the needs of other instructors who rely on these materials.. 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. . 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.