Welcome to Transport Processes and Accretion in Young Stellar Objects
In the magnetospheric accretion paradigm, originally developed 30 years ago for accretion onto white dwarfs, the stellar magnetosphere truncates the disk at the location where the magnetic pressure balances the gravitational pressure. While this paradigm is generally accepted for classical T Tauri stars, critical aspects of the theory remain unknown. What happens where the stellar magnetosphere connects to the disk? What is the structure and morphology of the accretion flow? How does accretion power outflows? Does magnetospheric accretion break down for very young stars with high accretion rates or for high-mass stars? How does the gas accrete onto stars that have disks with large inner holes? How much of the disk is viscous and magneto-rotationally active? These questions are strive to solve the same basic problem: how is gas transported within the protoplanetary disk and from the disk onto the forming star?
The registration is open and will close on 15 October. Capacity is strictly limited at 60 participants, of whom 40 can stay at the castle and another 20 can stay in the nearby town. For more information, please contact firstname.lastname@example.org
We hope to see you in February!
Greg Herczeg and Roy van Boekel
Science Advisory CommitteeAurora Sicilia-Aguilar
Mario van den Ancker
Local Organizing CommitteeMin Fang
Invited SpeakersPeter Abraham
last modified: 26 Jan 2011