'Line profile' diaporamas de présentation

David Cohen Dept. of Physics and Astronomy Swarthmore College

X-ray Emission from Massive Stars: Using Emission Line Profiles to Constrain Wind Kinematics, Geometry, and Opacity. David Cohen Dept. of Physics and Astronomy Swarthmore College. astro.swarthmore.edu/~cohen. Outline. Introduction: the context of hot star X-rays

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Spectroscopy

Spectroscopy. 1990 Bruce Gold Medal 1937 AJC Prize. Spectral lines The Fraunhofer spectrum Charlotte Moore Sitterly Multiplet table Rowland table Formalism of spectroscopy. Quantum Numbers of Atomic States. Principal quantum number n defines the energy level Azimuthal quantum number l

475 views • 33 slides

Fe K ? Line in AGN

Fe K ? Line in AGN. Shane Bussmann AGN Class 4/16/07. Importance of Fe K ?. High energy astrophysics ? study accretion disks around BHs Emission feature arises close to BH ? probe strong gravity effects, compare to predictions from GR ? determine BH properties. The Standard Model.

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The CoRoT ground-based complementary archive

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Stellar Surface Structures

Stellar Surface Structures. Surface features associated with activity Chromospheres Spots Plage Coronal holes Flares Types of stellar activity Solar-type stars M dwarfs Active stars Star spots Doppler imaging Spots on A stars Stellar oscillations. Star Spot Properties.

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Developing a Masters Programme to support New Teachers Roseanne Fitzpatrick Amanda Hampton

Developing a Masters Programme to support New Teachers Roseanne Fitzpatrick Amanda Hampton Dr Dean Robson School of Education, University of Aberdeen ICET Conference, 13 July 2011. Content Background and Context Course Structure & Operation Research and Evaluation

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Analysis of Doppler-Broadened X-ray Emission Line Profiles from Hot Stars

Analysis of Doppler-Broadened X-ray Emission Line Profiles from Hot Stars. David Cohen - Swarthmore College with Roban Kramer - Swarthmore College Stanley Owocki - Bartol Research Institute. Outline. 0. The astrophysical context I. Introduction: What line profiles can tell us

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A new modelling approach for DACs and SACs regions in the atmospheres of hot emission stars

A new modelling approach for DACs and SACs regions in the atmospheres of hot emission stars. * Danezis E., *Lyratzi E, *Antoniou A. , **Popovi ? L. ? ., **Dimitrievi ? M. S.

364 views • 24 slides

Where is Coronal Plasma Heated?

Where is Coronal Plasma Heated?. James A. Klimchuk NASA Goddard Space Flight Center, USA Stephen J. Bradshaw Rice University, USA Spiros Patsourakos University of Ionnina , Greece Durgesh Tripathi Inter-University Centre for Astronomy and Astrophysics, India. Three Basic Scenarios.

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Estimate of physical parameters of molecular clouds

Estimate of physical parameters of molecular clouds. Observables: T MB (or F ? ), ? , ? S Unknowns: V , T K , N X , M H 2 , n H 2 V velocity field T K kinetic temperature N X column density of molecule X M H 2 gas mass n H 2 gas volume density. Velocity field.

345 views • 23 slides

Radiation modeling for optically thick plasmas

Radiation modeling for optically thick plasmas. Application to plasma diagnostics. D. Karabourniotis University of Crete GREECE. Plasma Light Model-Inventory workshop , Madeira, April 2005. Outline. General expression of spectral intensity I ? from a plasma layer

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Spectroscopy

Spectroscopy. Spectral lines The Fraunhofer spectrum Charlotte Moore Sitterly (Allen!) Multiplet table Rowland table Formalism of spectroscopy. Quantum Numbers of Atomic States. Principal quantum number n defines the energy level Azimuthal quantum number l

348 views • 17 slides

Spectroscopy of pulsations in ? Doradus Stars

Spectroscopy of pulsations in ? Doradus Stars. Emily Brunsden Department of Physics and Astronomy University of Canterbury emily.brunsden@pg.canterbury.ac.nz. Image: http://gong.nso.edu/. ? Doradus Stars. Pulsating late A to early F stars On or near main sequence

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Sy 1 type The line profile of iron K ? line in

Observations Tanaka, Nandra, Fabian. Nature, 1995, 375 , 659. Galaxy MCG-6-30-15, ASCA satellite, SIS detectors. Sy 1 type The line profile of iron K ? line in X-ray emission from MCG-6-30-15.

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The Classical Damping Constant

The Classical Damping Constant. For a classical harmonic oscillator, The shape of the spectral line depends on the size of the classical damping constant For n - n 0 >> g /4 p , the line falls off as ( n - n 0 ) -2 Accelerating electric charges radiate. and

517 views • 10 slides

Galactic Astronomy

Galactic Astronomy. Velocity fields of disks. Dong-hyun Lee 2007/08/23. Velocity fields of disks. Focus on the central freq. of the received radiation Central vel. & dispersion : line profile Fig. 8.36 : collection of concentric, circular rings

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Supplementary Figure Legends

Supplementary Figure Legends.

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Quantitative heat dissipation in GaN nanowire devices Yi Gu , Washington State University, DMR 0845007

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Valparaiso University Law Alumni Mentor Program

Valparaiso University Law Alumni Mentor Program. The Valparaiso University Law School Alumni Mentor Program provides law students and recent graduates an opportunity to network with alumni and obtain valuable career guidance. HOW DOES IT WORK?

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EXPERIMENTAL CHARACTERISATION OF THE HIGH-PRESSURE METAL-HALIDE Na-Sc-Hg DISCHARGE

EXPERIMENTAL CHARACTERISATION OF THE HIGH-PRESSURE METAL-HALIDE Na-Sc-Hg DISCHARGE Z. Miokovic 1 and D. Veza Physics Department, Faculty of Science, Uni-Zagreb, Bijenicka 32, HR-10002 Zagreb, Croatia (veza@phy.hr)

116 views • 1 slides