'1 pc' presentation slideshows

Modelling Massive Star Formation. Rowan Smith ZAH/ITA University of Heidelberg Ian Bonnell, Henrik Beuther, Paul Clark, Simon Glover, Ralf Klessen, Steven Longmore, Amy Stutz, Rahul Shetty. Motivation. 1. Observations: Environment.

e-government in France. ETSI, March 31, 2005. Overview. Governmental actions to improve Internet ADAE, a specific agency ADELE Program e-gov in Ministry of Interior e-Health. French government program : RE/SO 2007.

Feedback from ACDC3. Kazu Akiba. Data Flow. 12 Tell1s plus Odin put together on the crate NZS Data: 4~5kBx12 per event: 2.0 kEvent/s max DAQ with 1 PC. Tested with MEP factor up to 4 (NZS) and 15 (ZS) Too many packets to route: 1 switch is not enough for the Velo (HP 3400) 2 HP3400 work!

Star Formation in a Dynamic Interstellar Medium. Workshop hosted by the Yale University Astronomy Department May 20, 2002. Simulation is a preview of work by Bate, Bonnell & Bromm…stay tuned. The Plan. Time Speaker Topic 09:40 Alyssa Goodman (CfA/Yale) Introduction

Does turbulence cause the misalignment of outflows and magnetic fields in protostellar cores?. Chat Hull University of California, Berkeley Radio Astronomy Laboratory 4 June 2014 The Early Phase of Star Formation ( EPoS ) Turbulence Focus Group Ringberg Castle, Kreuth , Germany.

Datapath Design I. Systems I. Topics Sequential instruction execution cycle Instruction mapping to hardware Instruction decoding. Overview. How do we build a digital computer? Hardware building blocks: digital logic primitives Instruction set architecture: what HW must implement

Workshop Summary: Formation and Evolution of Stars Near the Galactic Center. Radcliffe Institute for Advanced Study. Nov. 13-15, 2003. Eve Ostriker The University of Maryland. A. Ghez: Observations of Stars Near the Galactic Center.

Generation of Sub-fsec, High Brightness Electron Beams for Single-Spike SASE FEL Operation. J.B. Rosenzweig UCLA Dept. of Physics and Astronomy for SPARC(X)-UCLA collaboration. Ultra-short FEL pulses. Investigations at atomic electron spatio-temporal scales

Main news. DAQ test bench running in Geneva 2 LDCs connected to 2 different PCs, 1 GDCs DAQ trigger distributed using MICE Trigger receiver (V977) Particle trigger given by scintillator signal discriminated by LS 4415 and using logic unit 4516 Network test with the Nortel 5510-24T switch

Fermi Problems and Scale of the Universe. Advanced Introduction to Astronomy Spring 2014 Pomona College. by Dr. Bryan E. Penprase. An Example of a “ Flipped ” Class!!. Enrico Fermi, U. of Chicago Physics professor (and pioneer of nuclear physics) at the chalkboard. Fermi Problems.

Virgo Survey: Single Peak Galaxies. 祖父江義明 U. Tokyo. A LMA 時代の銀河研究 １．日米欧干渉計事情 ２． ALMA は干渉計 3. NMA からの 正面突破. BIMA SONG ( BERKELEY ILLINOIS MARYLAND ASSOCIATION CO Survey of Nearby Galaxies). OVRO (Owens Valley Radio Observatory ). IRAM Plateau de Bure Interferometer.

Observational Magnetohydrodynamics of the Interstellar Medium. Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics. Principal Collaborators Héctor Arce , CfA Javier Ballesteros-Paredes, AMNH Sungeun Kim, CfA Paolo Padoan , CfA Erik Rosolowsky , UC Berkeley

Formation & evolution of protostellar disks around low-mass stars. S.Walch, A.Burkert, T.Naab Munich University Observatory. Initial Conditions. Density: Bonnor-Ebert Sphere Central density:  max =10 -18 g/cm³ Temperature: T = 20K Cut-off radius:  BE  = 6.9  0.1pc

High-mass stars from cradle to first steps: a possible evolutionary sequence ( High-mass  M * >10M ⊙  L * >10 4 L ⊙  B3-O ). The environment of star formation Theory: low-mass versus high-mass stars The birthplaces of high-mass stars Evolutionary scheme for high-mass stars

The H-R Diagram. In 1913, the American astronomer Henry Russel plotted the luminosities of stars versus their spectra class (related to the temperature). Similar to work done in 1911 by Danish astronomer Ejnar Hertzsprung They found that the luminosities and temperatures of star are related

On the structure of the neutral atomic medium. Patrick Hennebelle Ecole Normale supérieure-Observatoire de Paris and Edouard Audit Commissariat à l’énergie atomique. Important Physical Scales and Basic Understanding One static scale

Charge Preamp with On-Board Cable Driver (IO1195-1-REVA). Features: +/- 5V power supply. 165 mW power dissipation. Bipolar operation (Q_input = +/- ) Differential outputs for driving 100 ohm twisted pair cable. Large output voltage swing -- +/- 1.5V (cable terminated at both ends)

Star Formation/ISM with Herschel. Malcolm Walmsley (Arcetri) Floris van der Tak (MPIfR,Bonn). Star Forming Regions are complex. Such as DR21 at roughly 3 Kpc (Marston et al. IRAC). Fundamental steps forward with Herschel. PACS : Maps of star forming regions in continuum and OI 63 micron line

Imaging Quasars with Interferometry. Martin Elvis Harvard-Smithsonian Center for Astrophysics. Why Study Quasars and AGN?. Up to 1000 Galaxy Luminosities Visible to z > 6 (Age < 1 Gyr) Evolve strongly in luminosity and space density Variability: ‘ galaxy power from solar system scales’

LISA double BHs. Dynamics in gaseous nuclear disk. Outlines. Dynamical evolution of MBHBs Code introduction Initial conditions of the simulations Results Future work. MBHs coalescence (1). Collisionless background (Begelman, Blanford & Rees 1980). ● Dynamical friction