Physical Processes and Conditions Associated with the Formation of Protoplanetary Disks
Abstract
Stars and planetary systems are thought to develop more or less contemporaneously from extended disk-shaped nebulae. Because the dynamical states of such disks are far from their final equilibrium configurations, the nebulae can dissipate large amounts of energy, as matter accumulates in the center and angular momentum moves to the peripheries. Experience with cosmical systems that are far from equilibrium indicates that such rapid dissipative evolution frequently occurs through a variety of collective behaviors, sometimes producing phenomena of surprising violence. This chapter reviews the range of types of collective processes that may occur in protostellar disks and play significant roles in speeding the evolution of the disks, as well as affecting the physical state of the disk and altering the state of protoplanetary matter. The processes considered here include collective angular momentum transport processes, electrostatic lightning and magnetic flares.
- Publication:
-
Protostars and Planets III
- Pub Date:
- 1993
- Bibcode:
- 1993prpl.conf..939M
- Keywords:
-
- Accretion Disks;
- Physical Properties;
- Planetary Evolution;
- Planetary Systems;
- Protoplanets;
- Stellar Systems;
- Angular Momentum;
- Magnetohydrodynamic Turbulence;
- Pre-Main Sequence Stars;
- Surface Temperature;
- Astrophysics