'Limb darkening' presentation slideshows

The Transit Method

The Transit Method. Photometric Spectroscopic (next time). Detection and Properties of Planetary Systems 18 Apr: Introduction and Background: 25 Apr: The Radial Velocity Method 02 May: Results from Radial Velocity Searches 09 May: Astrometry 16 May: The Transit Method

1.25k views • 91 slides

Folie 1

1.09k views • 88 slides

Model Photospheres

808 views • 69 slides

Model Photospheres

860 views • 69 slides

Understanding interferometric visibility functions

Understanding interferometric visibility functions. J. Meisner. Computing the visibility function V(u,v) from the image function F(x,y). Possible approaches: Do the 2-D fourier transform (not so intuitive) In a circularly symmetric case, perform the Hankel transform (not so intuitive)

432 views • 35 slides

The Sun

The Sun. Abundance of Elements in the Sun. Element % by Number % by Mass Hydrogen 92.0 73.4 Helium 7.8 25.0 Carbon 0.02 0.20 Nitrogen 0.008 0.09 Oxygen 0.06 0.8 Neon 0.01 0.16 Magnesium 0.003 0.06. Moon's Orbit. Visible sphere of the Sun. Relative sizes.

512 views • 34 slides

Stellar Astrophysics based on optical long-baseline interferometry -present and future-

Stellar Astrophysics based on optical long-baseline interferometry -present and future-. Markus Wittkowski (ESO) 1st Joint ARENA/OPTICON JRA4 Workshop Interferometry 10-12 May, 2006 Maison du Seminaire, Nice, France. Outline of the talk. Current interferometric facilities

327 views • 32 slides

Announcements

Announcements. Scores for first exam are available on WebCT. Exams (A and B) with correct answers marked are available on usual course web site (not in WebCT). Two more days of observing for extra credit for first exam. Second exam will be on Friday, October 8 th .

338 views • 27 slides

The Absorption Features in X-ray Emission from Isolated Neutron Stars

The Absorption Features in X-ray Emission from Isolated Neutron Stars. 2004 / 04 / 15. Outline. Assumptions & Global Model. Gravitation Effect (see Isothermal NS Case). Strong M field Effect. Anisotropy of the surface temperature Beaming. Lensing Red-shift.

361 views • 25 slides

Multi-wavelength interferometry of evolved stars

Multi-wavelength interferometry of evolved stars. Markus Wittkowski (ESO) Main collaborators: VLTI/VLBA project: David A. Boboltz (USNO), Thomas Driebe, Keiichi Ohnaka (MPIfR) Stellar atmospheres: Jason Aufdenberg (NOAO), Christian Hummel (ESO),

353 views • 24 slides

The Model Photosphere (Chapter 9)

307 views • 20 slides

The Model Photosphere (Chapter 9)

271 views • 19 slides

Jian-Yang Li, University of Maryland Marc Kuchner, NASA Goddard Space Flight Center

Jian-Yang Li, University of Maryland Marc Kuchner, NASA Goddard Space Flight Center Ron Allen, Space Telescope Science Institute Scott Sheppard, Carnegie Institution of Washington, DTM. Measuring the Physical Properties of Outer Solar System Objects with the Space Interferometry Mission.

289 views • 17 slides

Fundamental Parameters of Stars

Fundamental Parameters of Stars. SUSI workshop, 29.05.2008 at Univ. of Sydney Regner Trampedach, Mt. Stromlo. Which Fundamental Parameters?. Stellar structure and evolution: Mass Age Composition Stellar atmospheres: Effective temperature Surface gravity Composition.

182 views • 10 slides

8. Analytic Solutions II

8. Analytic Solutions II. Rutten: Rosseland Mean Opacity & Diffusion Approx Gray atmosphere Limb darkening. Rosseland Mean Extinction Coefficient a R : Recast diffusion approximation so F is function of d T / d z , use:. Where k R ( z ) = a R ( z ) / r ( z ).

105 views • 9 slides