'Free free' presentation slideshows

Solar Radio Emission

Solar Radio Emission. T. S. Bastian NRAO. Plan. Preliminaries Emission mechanisms - Thermal free-free emission - Gyro-emission thermal gyroresonance nonthermal gyrosynchrotron - Plasma emission. Preliminaries.

1.06k views • 83 slides

Solar Radio Emission

Solar Radio Emission. T. S. Bastian NRAO. Plan. Preliminaries Emission mechanisms - Thermal free-free emission - Gyro-emission thermal gyroresonance nonthermal gyrosynchrotron - Plasma emission. Preliminaries.

1.15k views • 83 slides

Data Structures and Algorithms

1.03k views • 74 slides

Bremsstrahlung

1.15k views • 65 slides

733 views • 62 slides

Grains and Gas in the Ejecta of Classical Novae

Grains and Gas in the Ejecta of Classical Novae. R. D. Gehrz Department of Astronomy, University of Minnesota. Outline. Novae and Galactic chemical evolution Outburst parameters from radio/IR data Physical properties of nova grains Comparisons with ISM and the Solar System Grains

648 views • 48 slides

AGN inflow/outflow with SKA

Cygnus A at 240 MHz with LOFAR. AGN inflow/outflow with SKA. (C) J. McKean. Nozomu Kawakatu ( University of Tsukuba ) On behalf of SKA-Japan AGN sub-WG. Workshop on East-Asia collaboration for SKA@KASI, Nov.30-Dec. 2 2011. Members. N. Kawakatu (Univ. of Tsukuba) M. Kino (NAOJ)

737 views • 44 slides

The Radio/X-ray Connection in Young Stellar Objects in the Orion Nebula Cluster

574 views • 42 slides

Physical Processes Definitions Sources of Opacity Hydrogen bf and ff H - H 2 He Scattering. How does k n affect the spectrum? More continuous absorption, less continuum light at that wavelength More continuous absorption, lines must form in shallower layers, at lower optical depth

569 views • 34 slides

Continuous Opacity Sources

Continuous Opacity Sources. Continuous Opacity Sources. Principal Sources: Bound-Bound Transitions Bound-Free Free-Free (Bremstralung) Electron Scattering (Thompson & Compton) Molecular Transitions We consider only H or H-Like cases

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365 views • 25 slides

On the spurious eigenvalues for a concentric sphere in BIEM

The 32 nd National Conference on Theoretical and Applied Mechanics. On the spurious eigenvalues for a concentric sphere in BIEM. Reporter ? Shang-Kai Kao Ying-Te Lee , Jia-Wei Lee and Jeng-Tzong Chen Date ? 2008/11/28-29. National Taiwan Ocean University MSVLAB

369 views • 24 slides

NLTE_5_30

NLTE_5_30. ?? ??. Subroutine opac. [ Opac ] calculate standard and background opacity [OPINIT] initialize opacity package [INJON]read data about atoms for JON [INABS]reading data about absorption coefficient [ABSKO] administer absorption coefficient

254 views • 17 slides

Modeling the Light Curve of V445 Puppis: Helium Nova on a Massive White Dwarfs

Modeling the Light Curve of V445 Puppis: Helium Nova on a Massive White Dwarfs. Mariko KATO (Keio Univ., Japan) collaboration with I. Hachisu (Univ. of Tokyo) S. Kiyota (VSOLJ).

327 views • 17 slides

4. Continuum Transitions & LTE

4. Continuum Transitions & LTE. Rutten: 2.4, 2.5 Continuum transitions Sources of opacity? LTE: Maxwell, Saha, Boltzmann LTE: Planck, Stefan-Boltzmann Statistical weights, partition functions, etc NLTE, Statistical equilibrium. Continuum Transitions. Bound-free:

258 views • 15 slides

New Model Atmospheres for Hydrogen-Deficient Stars

New Model Atmospheres for Hydrogen-Deficient Stars. May 3 rd , 2006 Natalie Behara Armagh Observatory. Hydrogen -Deficient stars. Wolf-Rayet central stars of planetary nebulae. Evolved, massive and extremely hot ( up to ~ 50 000 K)

309 views • 15 slides

Free-Free Absorption from H I

Free-Free Absorption from H I. Much less than bf absorption Kramers (1923) + Gaunt (1930) again Absorption coefficient depends on the speed of the electron (slower electrons are more likely to absorb a photon because their encounters with H atoms take longer)

318 views • 14 slides

NOTES ON THE 15 FIELDS

SPECTRA OF GALACTIC COMPONENTS OBSERVED BY WMAP R.D.Davies, R.J.Davis Jodrell Bank Observatory C.Dickinson California Institute of Technology A.J.Banday, T.R.Jaffe MPI fur Astrophysik K.M.Gorski Caltech and JPL.

222 views • 14 slides

Ballroom & Latin Dancing

158 views • 1 slides

Star Formation

Emission from Star Formation Regions. DMCs. H ? etc. HII Regions. Radio Lines: CO. ionize. Radio Free-free. Star Formation. UV. O/B stars. dust. age & mix. FIR. SN. Optical colors/ spectra. shocks c. rays. Radio Synchrotron.

127 views • 1 slides