By T. Owen (auth.), Bernard F. Burke, Jürgen H. Rahe, Elizabeth E. Roettger (eds.)
`Are there different planetary structures like ours? different planets like ours? Is there existence in different places within the Universe?' So asks Dr. Lew Allen Jr. within the Foreword. In December of 1992, theorists, observers, and device developers accrued on the California Institute of know-how to debate the hunt for solutions to those questions. The overseas convention, entitled `Planetary platforms: Formation, Evolution, and Detection' and supported via NASA's newly shaped TOPS (Toward different Planetary structures) software, used to be the 1st of a chain of meetings uniting researchers throughout disciplines and political obstacles to proportion recommendations and data on planetary platforms. The convention used to be backed via NASA, hosted by means of JPL at Caltech, and counseled via the 1992 foreign area yr organization.
those lawsuits contain discussions of issues starting from stellar, disk, and planetary formation to new methods of attempting to find different stellar structures containing planets. The authors characterize a variety of nationalities, disciplines, and issues of view. the second one foreign convention happened in December of 1993.
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Additional resources for Planetary Systems: Formation, Evolution, and Detection: Proceedings of the First International Conference, held in Pasadena, California on December 8–10, 1992
Example text
FORMATION AND PROPERTIES OF FLUFFY PLANETESIMALS * BERTRAM DONN Department of Materials Science and Engineering. University of Virginia. Charlottesville. Virginia. MARKDUVA Department of Applied Mathematics. University of Virginia. Charlottesville. Virginia. USA Abstract. A mechanism of accumulation of grains in the primordial solar nebula is described. This process produces porous, low density compressible aggregates. Compaction of the aggregates in a collision between them dissipates the kinetic energy of the collision and can result in efficient growth.
44 x 10° For the combinations of the collision parameters chosen, Lo is always substantially less than L, so the energy of the collision can be absorbed. 0 m s-1 will produce a collision sufficiently violent that not all of the energy can be absorbed. If accretion and not fragmentation is to take place as the bodies increase in size, the (average) relative density of the growing body must increase slowly so that the energy per unit area of subsequent collisions remains modest and the energy-dissipating capacity of the aggregate is retained.
_. . _. . . __. . _. . _lD~ yr 1- -/ ~ 107 Ii I lO~LJ , Fig. 2b. As Figure 2a. Dependence on mass accretion rate. "cr = 1 ME / (dM / dt) is 105 , 106 , or 107 yr. Temperatures T. at small planetary masses are determined by the balance between the release of gravitational energy GM Ir. (dM Idt) and blackbody radiation 41rr~(jsBT:. In the later stage of accretion, however, dependence of T. on mass accretion rate is small. 4. Dust Transport in the Atmosphere From the dust condensation zone (r "" 3r s "" 2 x 107 m, when M = 1 ME), condensed dust can be transported outward by convection.