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Characteristics of IR variable stars as observed from orbitA selection of infrared variable stars was studied at wavelength 2.7 microns during 1971-1975 with data from U.S. Air Force satellites. Stars observed in this program are classified as long-period variable stars, semiregular variables, and irregular variables and are among the strongest stellar sources at this wavelength. In addition, a few new, as yet unclassified variable stars were identified during the course of the investigation. Time scales of reproducible variations range from a few weeks to a few years, and amplitudes of variation are as large as a factor of three for stars with periods of order one year. The minimum infrared flux density of a long-period star repeats accurately from one cycle to the next, whereas the maximum flux density was found to be unstable. The correlation of 2.7 micron and radio emission line data from one, well-studied long-period variable is consistent with the hypothesis that the H2O and OH circumstellar masers are saturated, if pumped by the stellar infrared flux near 2.7 microns.
Document ID
19770053166
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Maran, S. P.
(NASA Goddard Space Flight Center Greenbelt, Md.; California, University, Los Angeles, Calif., United States)
Heinsheimer, T. F.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Stocker, T. L.
(Aerospace Corp. El Segundo, Calif., United States)
Chapman, R. D.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Hobbs, R. W.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Michalitsanos, A. G.
(NASA Goddard Space Flight Center Greenbelt, Md., United States)
Date Acquired
August 9, 2013
Publication Date
January 1, 1976
Subject Category
Astronomy
Meeting Information
Meeting: Seminar on Modern utilization of infrared technology II: Civilian and military
Location: San Diego, CA
Start Date: August 26, 1976
End Date: August 27, 1976
Accession Number
77A36018
Distribution Limits
Public
Copyright
Other

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