PDF-Binary Stars and Accretion Disks

AS 4024 InclinationsRadial velocities give minimum masses149need inclinations150 orbits150eclipsing binaries150apsidal motion 333 AS 4024 Binary Stars and Accretion Disks Astrometric Orbit. Alecian Abstract In this chapter I 64257rst present the premain sequence stars around which accretion disks are observed and summarise the main observed characteristics of the classical T Tauri and Herbig AeBe stars I then review the theoretical and Phil Armitage. Colorado. Processes in Protoplanetary Disks. Disk structure. Disk evolution. Turbulence. Episodic accretion. Single particle evolution. Ice lines and persistent radial structure. Transient structures in disks. Double Stars/Binary Stars. . Binary Star. Double Star. Earth. Earth. Visual Binary Stars. Orbit of Star 1. Orbit of Star 2. Center of Mass. Sirius A & B. Orbit of 12 Persei. (Barlow, Scarfe, and Fekel. do not live alone. B. ackground Design E. . Buunk. / S.E. de Mink, . HST image: NASA . Paresce. Selma E. de Mink. Hubble Science Briefing . , . February 7, 2013. Hubble Fellow at Space Telescope Science Institute / Johns Hopkins University. Garrido. . Goicovic. Supervisor: Jorge Cuadra. PhD thesis project. January 2014. Simulations of a molecular cloud falling into single and binary SMBHs . Galaxies. and . SMBHs. Supermassive. Black . young stars . with . LSST. Gregory J. Herczeg. KIAA. Star Formation: . ISM/Molecular Clouds . Pre-main sequence stellar evolution. (low-mass case). HD141569, . Clampin. et al.. Classical T . Tauri. Stars. Phil Armitage. Colorado. Processes in Protoplanetary Disks. Disk structure. Disk evolution. Turbulence. Episodic accretion. Single particle evolution. Ice lines and persistent radial structure. Transient structures in disks. Masses: . Binary Stars. . The HR Diagram Again. A Diagram for . People. Q. : . What . is happening here. ? . A: . People . grow. . They . are born small, and then grow in height and mass as they age (with a fair bit of individual scatter).. of . planetary nebulae, . jets and cosmic . outbursts. Orsola De . Marco. Macquarie University. Collaborators: . Jan Staff (Florida State). Jean-Claude Passy (Bonn U). Roberto Iaconi (Macquarie U). Todd . Phil Armitage. Colorado. Motivation. What can we directly observe?. Dust. m. m-mm. Gas – . emission &. kinematics. (CO other. molecules, . H. 2. hard). Limited. direct . time . dependence. Evolution. Pawel. . Artymowicz. U of Toronto. MRI turbulence. Some non-MRI turbulence. Roles and the dangers of turbulence. UCSC Santa Cruz 2010. I borrowed some . figures & slides from. X. Wu (2004). R. Nelson (2008). Insights from recent surveys. Gaspard . Duchêne. (UC Berkeley, Obs. Grenoble). © NASA/JPL/Caltech. Planets in multiple systems?. © . LucasFilm. Ltd.. They must exist!. Planets in multiple systems!. are . relatively widely . separated. , . their . evolution proceeds much as it . would . have if they were not . companions.... If they are . closer. , it is possible for . material . to transfer from one star to another, . VEGA. . Recent. . results. and . ongoing. programs. CHARA 2017:. . Year 13 Science Review . –. Adaptive Optics and Open Access. The VEGA instrument. 4-beams visible combiner (3 in standard modes).