86 GHz SiO Maser Emission Towards Mira

Details 86 GHz SiO Maser Emission Towards Mira 86 GHz SiO Maser Emission Towards Mira

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...193.4515p&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #45.15; Bulletin of the American Astronomical Society, Vol. 30, p.1319

Astronomy and Astrophysics

Astronomy

Scientific paper

Mira (o Ceti) was observed with two independent 3mm VLBI arrays in April 1998. Unlike its counterpart R Aqr, there are no published VLBI results on Mira, and little is known about how the SiO masers are arranged on circumstellar scales. The international 3mm VLBI observations, coordinated through the CMVA, offered baseline lengths from 20 to 330 Mlambda . The major features of the nu = 1, J = 2 -> 1 SiO masers, whose velocity span is roughly 3.5 km s(-1) , will be examined in the context of asymmetry and possible interaction by Mira with its companion VZ Ceti indicated on larger scales by optical and UV instruments such as the HST.

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