'Thermal pressure' diaporamas de présentation

Chapter 16 Star Birth

Chapter 16 Star Birth. 16.1 Stellar Nurseries. Our goals for learning Where do stars form? Why do stars form?. Where do stars form?. Star-Forming Clouds. Stars form in dark clouds of dusty gas in interstellar space The gas space between the stars is called the interstellar medium.

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ASTR 1020

ASTR 1020. First Homework Due Today Second Homework due Feb 9 Next Observatory Session Tonight at 7pm. Website http://casa.colorado.edu/~wcash/APS1020/APS1020.html. Escape Velocity. R. Fall from Large Height. Same Energy Needed to Reverse and Fly Away. Escape velocity is the speed

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Schedule

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Schedule

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Physical Conditions of the Nearby Gas

Physical Conditions of the Nearby Gas. Edward B. Jenkins Princeton University Observatory. What Kind of Gaseous Material are we Considering?.

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Cosmic Rays and Thermal Instability

Cosmic Rays and Thermal Instability. T. W. Hartquist , A. Y. Wagner, S. A. E. G. Falle , J. M. Pittard , S. Van Loo. Outline. The thermal instability of a non-magnetized, uniform static fluid, in the absence of cosmic rays The thermal instability and cloud formation

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Interstellar Shocks

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Planetary Magnetism

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Edward A. Startsev, Ronald C. Davidson and Hong Qin

The Heavy Ion Fusion Virtual National Laboratory. Simulation Studies of Temperature Anisotropy Instability in Intense Charged Particle Beams for IBX Parameters. Edward A. Startsev, Ronald C. Davidson and Hong Qin. Princeton Plasma Physics Laboratory. Presented at. APS DPP2003 Meeting.

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ESS154/200C Lecture 10 Solar Wind Interactions: Unmagnetized Planets

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Cooling and Feedback in Early-Type Galaxies (and Groups)

Cooling and Feedback in Early-Type Galaxies (and Groups). C. Jones, W. Forman, E. Churazov, P. Nulsen, R. Kraft. X-ray emission from early-type galaxies = hot gas + stars + LMXBs Heating by radio lobes (e.g. Cen A) Results from a Chandra survey of ~160 galaxies -

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SUPERNOVA NEUTRINOS AT ICARUS

SUPERNOVA NEUTRINOS AT ICARUS. G. Mangano INFN, Napoli. Summary - SN explosion dynamics - Neutrino spectra and overall features - SN 1987A at Kamiokande and IMB - SN & ICARUS - SNO, SK, LVD - Oscillations - Issues to be studied. He and H shell burning. He core burning. He flash.

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The birth of a star Chapter 11

The birth of a star Chapter 11. Questions to be addressed:. Where are the birth places of stars? What are the main components of a protostar? When and how a new is born? What prevents a star from collapsing?. How does a star form?.

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Cosmological Evolution of Blazars: new findings from the Swift/BAT and Fermi/LAT surveys

Cosmological Evolution of Blazars: new findings from the Swift/BAT and Fermi/LAT surveys. M. Ajello [KIPAC/SLAC] L. Costamante, R. Sambruna, N. Gehrels, J. Greiner, J. Tueller, J. Chiang, A. Escala, R. Mushotzky, A. Rau, J. Wall + On behalf of Fermi/LAT collaboration. Instruments.

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Lattice Dynamics

Lattice Dynamics. Thermal Expansion. As temperature changes, density changes Thermodynamics Relates this change to changes in other properties Cannot tell the magnitude or even the sign! Why positive alpha? What value vs. P,T,X? Macroscopic to Microscopic

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Equations of State Ronald Cohen Geophysical Laboratory Carnegie Institution of Washington

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Seminar report I: HYPERCOMPACT HII regions

Ref: M. Sewilo, et al, ApJ,605 ? 285-299 Tara Murphy, et al, Arxiv:1002.4627v1 Stan Kurtz, Proceeding IAU Symposium No. 227. Seminar report I: HYPERCOMPACT HII regions. FengLi 2010-03-22.

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The Most Local Interstellar Medium

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