PPT-MODELING FORMATION OF SELF-GRAVITATING DUST CONDENSATIONS A

A B Makalkin I N Ziglina Schmidt Institute of Earth Physics Russian Academy of Sciences Obstacles to the growth of large dust particles and small bodies in a protoplanetary disk Metersized barrier. What force makes stars? . Gravity!. Out of what? Interstellar gas and dust. But this stuff is VERY low density… a dense area may have ~100 atoms / cm. 3. . Compare that the air you’re breathing… ~10. of dust heating in M81, M83 and NGC 2403 with Herschel and Spitzer. George J. . Bendo. Very Nearby Galaxies Survey . Goals. The overall goals of this research are to empirically identify the heating sources for the dust observed at 70-500 µm.. dust. . attenuation. and star formation histories . at. . high. . redshift. Véronique . Buat. Laboratoire d’Astrophysique de Marseille. Elbaz’s. lectures . (. david.elbaz3.free.fr/coursJ1.html), . Topic:. Gravoturbulent planetesimal formation. :. Particle clustering,. Streaming instability,. Particle trapping. Lecture by: C.P. Dullemond. Main idea:. If we can find a way to cluster the dust particles into small regions („dust clouds“) where the density of dust would be very large, then perhaps gravity could then take over and cause the dust cloud to gravitationally collapse (contract) to form a planetesimal.. planetesimal. -formation scenarios. Jürgen Blum. Institut. . für. . Geophysik. . u. nd . extraterrestrische. . Physik. Technische. . Universität. . Braunschweig. Germany. In collaboration with. Topic:. Dust motion and. coagulation. Lecture by: C.P. Dullemond. Coagulation as the start of planet formation. 1. . m. 1m. m. 1. m. 1k. m. 1000k. m. Gravity. keeps/pulls. bodies. together. Gas is. Lecture 8: Dusty starburst galaxies. Prof.. . Dr.. M. . Baes. (. UGent. ). Prof.. . Dr.. C. . Waelkens. (KUL). Academic year 2015-2016. The interstellar medium. The space between the stars in a galaxy is not empty. . debris. . disks. with. . GRaTeR. . (Grenoble Radiative . TransfeR. ). Jérémy Lebreton. EXOZODI . Kick-off. Meeting . 10-02-2011. Different. and . complementary. . approaches. to model . debris. Radiation:. Mineral . Dust. A. Macke, IfT Leipzig. presented. . by. H. Herrmann, IfT Leipzig. Berlin, 23.09.2011. Leipzig Graduate School. A Leibniz Graduate School on . Atmospheric. Research. Integrating. From Supernovae to Planets. Drafted by Manning for the . SOFIA . Team. 0. Topic: . Supernovase. .. Concepts: . Supernovae, planet formation, infrared observations. Missionb. : . SOFIA. Coordinated by: . 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. Amato Evan. Scripps Institution of Oceanography, University of California San Diego, USA. Key Questions. What are the spatial, temporal, and microphysical characteristics of dust over California, and what are the primary source regions for these mineral aerosols?. William . McDoniel. D. . B. Goldstein, P. L. Varghese, L. M. . Trafton. University of Texas at Austin. Department of Aerospace Engineering. DSMC . Workshop . September . 28. th. , . 2011. Supported by the NASA Planetary . Diana . Jordanova. and Neli . Jordanova. National Institute of Geophysics, Geodesy and Geography, Bulgarian Academy of Sciences, Acad. G. . Bonchev. str., block 3, 1113 Sofia, BULGARIA. diana_jordanova77@abv.bg.