'Abundances' presentation slideshows

576 views • 50 slides

TEMPERATURE STRUCTURE OF GASEOUS NEBULAE AND CHEMICAL ABUNDANCES

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Absolute UV fluxes from the Sun and late-type stars

Absolute UV fluxes from the Sun and late-type stars. C. Allende Prieto McDonald Observatory Univ. of Texas. Not without help. Analisis: D. L. Lambert, I. Ramirez (Texas) Model atmospheres, radiative transfer: I. Hubeny (Arizona), L. Koesterke (Texas) 3D models: M. Asplund (Australia)

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Open Clusters and Galactic Disk Observations with LAMOST

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Chemical Abundances in AGN: the Mrk 279 Outflow

Chemical Abundances in AGN: the Mrk 279 Outflow. Nahum Arav University of Colorado Boulder Collaborators: Jack Gabel , Jelle Kaastra, Gerard A. Kriss , Kirk T. Korista,, Jennifer E. Scott, Daniel Proga, Katrien C. Steenbrugge, Ehud Behar, Ari Laor, Masao Sako.

491 views • 34 slides

Gamma-Rays From Solar Flares

Gamma-Rays From Solar Flares. Content. Electron bremsstrahlung continuum Nuclear de-excitation lines Neutron capture line Positron annihilation Pion decay radiation. Spectrum. Gamma-Rays. bremsstrahlung. bremsstrahlung. Thin target and thick target bremsstrahlung. Thick:. Thin:.

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Sun

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Are recent solar heavy element abundances consistent with helioseismology?

Are recent solar heavy element abundances consistent with helioseismology?. Sarbani Basu H.M. Antia. The Abundances. Envelope models, CZ base and Y forced to have helioseismically determined values. OP opacities give “better” results than OPAL. Serenelli et al. (2009).

209 views • 11 slides

Joanna Brown

Circumstellar Chemistry: The Effects of High Density Shells on the Distribution of Molecules in IRC+10216. Joanna Brown. CW Leo: IRC+10216. Part of Asymptotic Giant Branch. Why is CW Leo chemically interesting?.

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Abundances in the Solar Atmosphere and in the Solar Wind

Abundances in the Solar Atmosphere and in the Solar Wind. Tuesday afternoon - 25 June 2013 Wednesday morning - 26 June 2013 Daniel Wolf Savin (Columbia University). Abundances (Tues PM). Peter Young (George Mason)

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Working Group 3: Gamma Rays and Ions

Working Group 3: Gamma Rays and Ions. Leader: Albert Y. Shih Co-Leader: Alec MacKinnon. Discussion focuses. The present Ongoing analyses Imminent observations Instruments under construction What are the important science questions? Future analyses and observations Future instruments.

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Anna Frebel University of Texas at Austin anna@astro.as.utexas

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Anna Frebel University of Texas at Austin anna@astro.as.utexas

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Interstellar medium

Interstellar medium . Brittany Griner Robin McCollum . interstellar medium. Matter among the stars Made up of two components: gas and dust Gas atoms exists at a size of 10^-10 m and at density of one atom per cubic centimeter

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M Humayun et al. Nature 000 , 1-4 (2013) doi:10.1038/nature12764

Gusev rock and soil analyses 13 have systematically higher Zn abundances than both Martian meteorites and NWA 7533. M Humayun et al. Nature 000 , 1-4 (2013) doi:10.1038/nature12764.

138 views • 1 slides