'Cool stars' diaporamas de présentation

Atomic and molecular data for stellar atmosphere modelling: Phoenix

733 views • 63 slides

2 months to go: time to be serious about observing run preparations

2 months to go: time to be serious about observing run preparations. http://glozing.blogspot.com/2012/09/like-scouts-say-be-prepared.html. getting ready for our (any!) observing run. YOU THE OBSERVER should never be the cause of this:. http://cheezburger.com/5797953792.

524 views • 39 slides

X-ray Observations of Stars

324 views • 32 slides

FUSE Spectroscopy of Cool Stars

FUSE Spectroscopy of Cool Stars. Graham Harper CASA, University of Colorado. Far Ultraviolet Spectroscopic Explorer. FUSE USA with France and Canada as partners FUSE Launched June 24, 1999. 765 km circular orbit, inclined 25 degrees, P = 100 minutes. 5-yr in orbit

437 views • 28 slides

Lecture 8

Lecture 8. Optical depth. Review: opacity. How does the intensity of radiation depend on opacity and distance travelled through a homogeneous medium? . Opacity ( k ) is a cross-section per unit mass (units m 2 /kg) of material for absorbing photons of a specific wavelength.

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Basic Properties of Stars

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Perryman 1992

NAHUAL status: A CONCEPT FOR A HIGH RESOLUTION IR SPECTROGRAPH F OR A 10-M SEGMENTED TELESCOPE (GTC). Perryman 1992. Motivation: To extend the parameter space of planet searches (ages, masses, rotation). Very low-mass primaries (Martin et al. 2006, Blake et al. 2007,

340 views • 20 slides

Trish Jibben Smithsonian Astrophysical Observatory Cambridge,MA

202 views • 20 slides

Expansion of the Universe

323 views • 19 slides

COOL STARS and ATOMIC PHYSICS

High Accuracy Atomic Physics In Astronomy. COOL STARS and ATOMIC PHYSICS. Andrea Dupree. Harvard-Smithsonian CfA 7 Aug. 2006. OUTLINE. How does atomic physics influence our understanding of the atmospheres of cool stars ??? Three critical examples:

308 views • 16 slides

Ground Based Observations for the ESP V-1

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Measuring Magnetic fields in Ultracool stars & Brown dwarfs

Measuring Magnetic fields in Ultracool stars & Brown dwarfs. Dong-hyun Lee. How can we measure B-field in star?. Using Zeeman Effect The splitting of a spectral line into several components in the presence of a B-field

214 views • 9 slides