Gravitational Collapse: From Massive Stars to Planets : Ensenada, B.C., México, Diciembre 8-12, 2003

accretion angular assumed axis becomes binary Bodenheimer Boss calculations central cloud clumps cluster collapse computed considered convective cooling core density depends disk distribution dust dwarfs dynamical effects energy envelope equation estrellas et al evolution field Figure fragmentation function giant given grains gravitational HII region important increases initial instability ionized Jeans larger layers lead lower magnetic field mass massive stars material mean medium MNRAS models molecular momentum objects observed opacity orbits parameters phase planetary planets present pressure radiation radiative radius range ratio region resolution rotation scale sequence shell shown simulations solar solid solution stage star cluster star formation stellar stellar wind structure surface temperature thermal tion transfer turbulent University velocity wind Yorke zone