VLBI observations of main-line OH emission from U Orionis

Details VLBI observations of main-line OH emission from U Orionis VLBI observations of main-line OH emission from U Orionis

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...241l..95f&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 241, Oct. 15, 1980, p. L95-L98. NSF-supported research.

Astronomy and Astrophysics

Astronomy

20

Hydroxyl Emission, Interstellar Masers, Radio Sources (Astronomy), Stellar Spectra, Variable Stars, Very Long Base Interferometry, Emission Spectra, Polarization (Waves), Power Spectra

Scientific paper

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 arcsec 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.

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