  We present new optical time-resolved photometry and medium-resolution
spectroscopy of V2187 Cyg. We confirm its classification as a beta Cephei star
based on sinusoidal light variations with a period of 0.2539 days and mean
amplitudes of 0.037 and 0.042 magnitudes in "i" and "V", respectively. We
classified the spectrum of this star B2-3V with no evidence of variations in
the profiles of its absorption lines in timescales of hours or days. The
stellar spectrum is totally absent of emission lines. We detected unexpected
faint radio continuum emission (between 0.4 and 0.8 mJy at 6-cm) showing a
sinusoidal variation with a period of 12.8 days. The radio spectrum is thermal.
We searched in the Very Large Array archive for radio continuum emission toward
other 15 beta Cephei stars. None of these additional stars, some of them much
closer to the Sun than V2187 Cyg, was detected, indicating that radio emission
is extremely uncommon toward beta Cephei stars.
