Titlebook: Stellar Atmospheres: Theory and Observations; Lectures Held at the J. P. Greve,R. Blomme,H. Hensberge Conference proceedings 1997 Springer-

BRACE

Cool stars winds and mass loss: Observations,the replenishment of the Interstellar Medium. The aim is to illustrate the richness of the informations provided by the observations obtained in the various wavelength ranges from the optical to the radio. A selection of on-going developments which are potentially important for this theme is present

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The theory of line driven stellar winds, acceleration due to lines. The equation of motion for a line driven wind from a star in the point source limit is solved. This gives simple analytical expressions for the predicted mass loss rates and the terminal velocities. The equations show that . ∼ . . and . . ∼ . . ∼ . ., in agreement with th

Firefly

Circumstellar disks,ing material, and outflow disks, which are formed in rotating stellar winds. Here I discuss the basic hydrodynamics of rotationally supported (nearly Keplerian) accretion disks, as well as how a rotating stellar wind naturally leads to the formation of a dense wind-compressed equatorial disk. To obs

OGLE

Stellar coronae,rvational findings obtained with the . and ROSAT satellites. In particular, coronae appear to exist around all cool stars with outer convection zones with a minimum surface flux agreeing with the X-ray flux observed from solar coronal holes. The overall X-ray output of cool stars can vary enormously

affluent

The theory of line driven stellar winds, these winds are intrinsically unstable. This explains the observed super-ionization and the X-rays from line driven winds. We compare the predictions with observations and show that the theory is very successful in explaining the overall features of the winds of hot stars.

不幸的人

arabesque

0075-8450 e their structure and the interactions with the interior of the stars as well as with the interstellar environment, and the observations that support, modify and sometimes contradict these theories. This volume aims to provide the reader with an insight into problems related to stellar atmospheres b

MURAL

Pigeon

Cool star winds and mass loss: Theory,and on the complex interaction among dust formation, chemistry, hydrodynamics, thermodynamics and radiative transfer. We present some fundamental implications of a consistent description of the dust forming system on its observable appearance.

facilitate

Circumstellar disks,ervationally determine the geometry, density, and velocity structure of these disks, we must be able to calculate their observable properties, so these lectures also cover radiation transport in axisymmetric geometries. Here I discuss the calculation of infrared excess emission, intrinsic linear polarization, and spectroscopic line profiles.