Abstract
The prototype Mira (o Cet) has been extensively studied at radio wavelengths in HI, H 2 O, CO and SiO. It was only detected once in OH, at 1665 MHz, by Dickinson (1975) and never since. We also found emission in Mira at 1665 MHz, using the Nançay radio telescope in November 1990 and have monitored it regularly. The line profile is narrow and limited to the velocity range 45.3–46.8 kms−1 LSR (the stellar velocity is 46.8 kms−1). The total intensity appears to vary periodically but the peak occurs near light minimum. The signal exhibits strong circular polarization.
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References
Dickinson, D.: 1975, Ap.J. 199, 131 1975
Mattei, J.A., Mayall, M.W., Waagen, E.O.: 1990, “The American Assiciation of Variable Stars Observers”: Maxima and Minima of Long Period Variables.
Mennessier, M.O.: 1991, private communication.
Gérard, E., Bourgois, G.: 1992, IAU Circular No. 5427.
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© 1993 Springer-Verlag
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Gérrad, E., Bourgois, G. (1993). Unusual OH radio emission in Mira (o CET). In: Clegg, A.W., Nedoluha, G.E. (eds) Astrophysical Masers. Lecture Notes in Physics, vol 412. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-56343-1_280
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DOI: https://doi.org/10.1007/3-540-56343-1_280
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