Millimeter Recombination Lines from LkHalpha 101
  We present new millimeter observations of the ionized wind from the massive
young stellar object LkHalpha101, made with the IRAM interferometer and 30m
telescope. Several recombination lines, including higher order transitions,
were detected for the first time at radio wavelengths in this source. From
three alpha-transitions we derive an accurate value for the stellar velocity
and, for the first time, an unambiguous expansion velocity of the wind which is
55 km/s, much slower than reported previously, and the mass loss rate is 1.8e-6
solar masses per year. The wide band continuum spectra and the interferometer
visibilities show that the density of the wind falls off more steeply than
compatible with constant-velocity expansion. We argue that these properties
indicate that the wind is launched from a radially narrow region of the
circumstellar disk, and we propose that slow speed and a steep density gradient
are characteristic properties of the evolutionary phase where young stars of
intermediate and high mass clear away the gaseous component of their accretion
disks.
  The recombination lines are emitted close to local thermal equilibrium, but
the higher order transitions appear systematically broader and weaker than
expected, probably due to impact broadening. Finally, we show that LkHalpha101
shares many properties with MWC349, the only other stellar wind source where
radio recombination lines have been detected, some of them masing. We argue
that LkHalpha101 evades masing at millimeter wavelengths because of the disk's
smaller size and unfavorable orientation. Some amplification may however be
detectable at shorter wavelengths.
