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140122 ||| eng |
| 020 |
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|a 9789400954281
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| 100 |
1 |
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|a Morris, Mark
|e [editor]
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| 245 |
0 |
0 |
|a Mass Loss from Red Giants
|h Elektronische Ressource
|b Proceedings of a Conference held at the University of California at Los Angeles, U.S.A., June 20–21, 1984
|c edited by Mark Morris, Arie J. Zuckerman
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| 250 |
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|a 1st ed. 1985
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| 260 |
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|a Dordrecht
|b Springer Netherlands
|c 1985, 1985
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| 300 |
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|a XVI, 320 p
|b online resource
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| 505 |
0 |
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|a 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
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| 505 |
0 |
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|a 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 --
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| 505 |
0 |
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|a 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 AroundLate-Type Giants (Review) -- 20 GHZ Continuum and SiS Maser Emission from IRC+10216 --
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| 505 |
0 |
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|a 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 --
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| 653 |
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|a Astronomy / Observations
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| 653 |
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|a Astronomy, Observations and Techniques
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| 700 |
1 |
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|a Zuckerman, Arie J.
|e [editor]
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| 041 |
0 |
7 |
|a eng
|2 ISO 639-2
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| 989 |
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|b SBA
|a Springer Book Archives -2004
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| 490 |
0 |
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|a Astrophysics and Space Science Library
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| 028 |
5 |
0 |
|a 10.1007/978-94-009-5428-1
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| 856 |
4 |
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|u https://doi.org/10.1007/978-94-009-5428-1?nosfx=y
|x Verlag
|3 Volltext
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| 082 |
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|a 520
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| 520 |
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|a 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 investi 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 $ 10- M9/yr.). But to see dust grains and molecules properly, 5 especially in stars with truly large mass loss rates, ~ 10- M9/yr, one requires IR and radio astronomy. As this stage of copious mass loss only lasts for ~105 years one might be tempted to ask, "who cares?"
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