'Molecular clouds' diaporamas de présentation

STAR FORMATION

STAR FORMATION. Still somewhat mysterious, stars are born inside dark clouds and then revealed in all their beauty. Most stars form in GIANT MOLECULAR CLOUDS. GMCs have masses from 10 5 to above 10 6 solar masses (M ? ) typical densities above 1000 cm -3

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The Interstellar Medium

Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). The Interstellar Medium. Chapter 10. Guidepost.

568 views • 48 slides

The Interstellar Medium

Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). The Interstellar Medium. Chapter 10. Guidepost.

620 views • 48 slides

The Interstellar Medium

Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). The Interstellar Medium. Chapter 10. Guidepost.

1.13k views • 48 slides

The Interstellar Medium

Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). The Interstellar Medium. Chapter 10. Guidepost.

576 views • 48 slides

Report from the Oort Cloud

Report from the Oort Cloud. Simulations of the Formation of the Comet Reservoir Luke Dones Hal Levison Paul Weissman Martin Duncan. Scenario for Oort Cloud Formation. Icy planetesimals formed in the region of the giant planets

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The Interstellar Medium and Interstellar Molecules

The Interstellar Medium and Interstellar Molecules. Ronald Maddalena National Radio Astronomy Observatory. Interstellar Medium The Material Between the Stars. Constituents: Gases: Hydrogen (92% by number) Helium (8%) Oxygen, Carbon, etc. (0.1%) Dust Particles 1% of the mass of the ISM

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Galactic Radio Science

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Large-Scale Molecular mapping Key Issues in Star Formation Lee Mundy (University of Maryland)

Large-Scale Molecular mapping Key Issues in Star Formation Lee Mundy (University of Maryland) a nd MSIP c loud mapping team led by John Carpenter. Credit: Herschel Gould Belt Project lead by P. Andre; Arzoumanian et al 2011. Key Issues in Star Formation.

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Molecular Clouds

Molecular Clouds . 8 April 2003 Astronomy G9001 - Spring 2003 Prof. Mordecai-Mark Mac Low. Molecular Emission. CO emission Quickly becomes optically thick Rare isotopes have lower optical depth: 13 CO and C 18 O More easily photodissociated than H 2

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August 2006

TELESCOPES and DETECTORS. LSST - A Plan for Photo-z Calibrations. August 2006 Bogdan Popescu. OVERVIEW 1.

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The Milky Way

The Milky Way. The Milky Way. The Milky Way is the great band of light that is best seen in the summer from a dark site . The name "Milky Way" is derived from its appearance as a dim un-resolved "milky" glowing band arching across the night sky .

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Galactic Line Science (with ALMA Band 1)

School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES. Galactic Line Science (with ALMA Band 1). Paola Caselli. Outline. Molecular cloud and cloud cores HC 3 N Deuterium fractionation S-bearing molecules SiO P-bearing molecules Complex molecules Summary.

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Where and How Are Massive Stars Formed in Isolation?

Where and How Are Massive Stars Formed in Isolation?. You-Hua Chu (U of Illinois) In collaboration with: R. Gruendl, R. Chen*, M. Gelman, M. Johnson (Illinois) H. Zinnecker (Potsdam). Galactic O-Type Stars. 70% in clusters or OB associations > 10% runaway stars

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Chemical conditions within the G333 Giant Molecular Cloud

Supervisors: Maria Cunningham (UNSW), James Urquhart (CSIRO) Michael Burton (UNSW) Collaborators: Nadia Lo (UNSW/CSIRO), Bhaswati Mookerjea (Tata Institute) Great Barriers in High Mass Star Formation, 14 th September 2010. Vicki Lowe

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Stellar Birth and Stellar Structure

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HI and Molecules

HI and Molecules. 0. Observing Neutral Hydrogen: The 21-cm (radio) line. Forbidden hyperfine-structure transition: A = 2.95x10 -15 s -1. Equal magnetic fields repel => Higher energy. Opposite magnetic fields attract => Lower energy. Magnetic field due to proton spin. 21 cm line.

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The Structure of the Taurus Molecular Cloud Complex

The Structure of the Taurus Molecular Cloud Complex

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Simulations of Compressible MHD Turbulence in Molecular Clouds Lucy Liuxuan Zhang, CITA / University of Toronto, pet_fat@cita.utoronto.ca Chris Matzner, University of Toronto, matzner@cita.utoronto.ca Ue-Li Pen, CITA / University of Toronto, pen@cita.utoronto.ca. Abstract

168 views • 1 slides