عنوان

Mass Loss from Red Giants :

940095428X

9789400954281

b593522

Mass Loss from Red Giants :

[Book]

Proceedings of a Conference held at the University of California at Los Angeles, U.S.A., June 20-21, 1984

edited by Mark Morris, Ben Zuckerman.

Dordrecht

Springer Netherlands

1985

(XVI, 320 pages).

Astrophysics and Space Science Library, A Series of Books on the Recent Developments of Space Science and of General Geophysics and Astrophysics Published in Connection with the Journal Space Science Reviews, 117.

On the Significance of Mass Loss from Bright Red Giants (Review) --; Masses of White Dwarfs and Other Remnants: The Ultimate Constraint on M? (Review) --; Optical Spectroscopy of Red Giants (Review) --; Mass Loss in Metal Deficient Red Giants --; Mass Loss from Red Giants: Results from Ultraviolet Spectroscopy (Review) --; Densities, Temperatures and Geometric Extents of C II Emitting Regions in the Winds of Luminous, Late-Type Stars --; Results from Optical Interferometry (Review) --; High Angular Resolution Interferometric Observations of Betelgeuse in the Visible --; Mass Loss from Red Giants: Infrared Spectroscopy (Review) --; CO Vibration Rotation Lines from Circumstellar Shells --; Circumstellar Dynamics Observed by Infrared Heterodyne Spectroscopy --; The Near Circumstellar Environment of Miras --; The Infrared Characteristics of Circumstellar Silicate Grains --; Infrared Spatial Interferometry (Review) --; 10 Micron Speckle Interferometry of OH/IR Stars --; Far-Infrared and Submillimeter Photometry of Evolved Stars (Review) --; Thermal Radio Emission from Molecules in Circumstellar Outflows (Review) --; Time Variations of SiO (v=0, J=2-1) Emission from Circumstellar Shells --; SiS in Circumstellar Shells --; Infrared Pumping and Polarization of Molecular Lines in IRC+10216 --; The Distribution of HCN in the Circumstellar Envelope of IRC+10216 --; Upper Limit for the Production of 14C in the Carbon Star IRC+10216 from Observations of the 14CO (J=1-0) Line --; The 13C/12C Isotope Ratio in Circumstellar Envelopes --; CO(2-1) Emission from the Circumstellar Envelope of Alpha ORI --; CO (1-0) Maps of NGC7027 --; The NGC 7027 Molecular Cloud --; CO Emission from Planetary Nebulae --; The Gas to Dust Ratio in Circumstellar Envelopes --; 21-CM Line and Radio Continuum Emission from Circumstellar Envelopes Around Late-Type Giants (Review) --; 20 GHZ Continuum and SiS Maser Emission from IRC+10216 --; Radio Continuum Observations of G-M Giants and Supergiants and Inferred Ionized Mass Loss Rates --; Maser Emission as a Tool to Study Mass Loss from Evolved Stars (Review) --; A Search for OH and H2O Maser Emission from Unidentified Iras Sources --; Radio and Infrared Observations of OH/IR Stars --; Mass Loss from OH/IR Stars --; What Circumstellar SiO and OH Masers Tell Us about Mass Loss from Red Giants --; Time Monitoring of SiO (v=1, J=2-1) Maser Emission from Late Type Stars --; New 43 GHz SIO Observations with the MPIFR 100m Telescope --; Mass Loss Mechanisms for Cool, Low-Gravity Stars (Review) --; Pulsation, Mass Loss and Grain Formation in Cool Giants --; Effects of Rotation and Convection on Mass-Loss from Red Giants --; Hydrogen Deficiency and Mass Loss from AGB Stars --; The Physical and Chemical Structure of Circumstellar Envelopes (Review) --; Bipolar Nebulae and Mass Loss from Red Giant Stars (Review) --; Infrared Studies of the Bipolar Nebula OH0739 --; Observations of the Far-Infrared Emission Lines of OI and CII in Planetary Nebulae --; Ammonia and Cyanotriacetylene in the Egg Nebula --; Concluding Remarks --; Object Index.

Red giant and supergiant stars have long been favorites of professional 6 and amateur astronomers. These enormous stars emit up to 10 times more energy than the Sun and, so, are easy to study. Some of them, specifically the pulsating long-period variables, significantly change their size, brightness, and color within about a year, a time scale of interest to a single human being. Some aspects of the study of red giant stars are similar to the study of pre-main-sequence stars. For example, optical astronomy gives us a tantalizing glimpse of star forming regions but to really investiƯ gate young stars and protostars requires infrared and radio astronomy. The same is true of post-main-sequence stars that are losing mass. Optical astronomers can measure the atomic component of winds from red giant stars that are undergoing mass loss at modest rates 6 (M

Proceedings of a Conference held at the University of California at Los Angeles, U.S.A., June 2--21, 1984

Mass loss (Astrophysics) -- Congresses.

Physics.

Red giants -- Congresses.

edited by Mark Morris, Ben Zuckerman.

Ben Zuckerman

Mark Morris

[Book]

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