VLBI observations of main-line OH emission from U Orionis

Journal Article · Wed Oct 15 04:00:00 EDT 1980 · Astrophys. J., Lett. Ed.; (United States)

DOI:https://doi.org/10.1086/183368· OSTI ID:6849289

Fix, J D; Mutel, R L; Benson, J M; Claussen, M L

Compact structure in the 1665 MHz OH emission from the long-period variable star U Orionis was detected using a five-telescope VLBI array. The U Orionis spectrum contains many compact, highly circularly polarized features which are spread over an area about 0''.5 in size. The polarization of the 1665 MHz emission from U Orionis cannot be understood by a simple Zeeman model. The extent of the main-line emission from U Orionis is significantly larger than that of previously measured 1612 MHz emission. This result is at odds with current models of circumstellar maser emission which predict that the main-line masers should lie closer to the central star than do the 1612 MHz masers.

• Research Organization: Department of Physics and Astronomy, University of Iowa
• OSTI ID: 6849289
• Journal Information: Astrophys. J., Lett. Ed.; (United States), Journal Name: Astrophys. J., Lett. Ed.; (United States) Vol. 241:2; ISSN AJLEA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
AMPLIFIERS
CHEMICAL COMPOSITION
COSMIC RADIO SOURCES
ELECTRONIC EQUIPMENT
EMISSION
ENERGY SPECTRA
EQUIPMENT
HYDROXYL RADICALS
INTERFEROMETRY
MASERS
MICROWAVE AMPLIFIERS
MICROWAVE EQUIPMENT
POLARIZATION
RADICALS
SPECTRA
STARS
VARIABLE STARS