  We present post-outburst (~ 100 days after outburst) radio continuum
observation of the region (~ 30' x 30') around McNeil's nebula (V1647 Orionis).
The observations were carried out using the Giant Metrewave Radio Telescope
(GMRT), India, at 1272 MHz on 2004 Feb 14.5 UT. Although 8 sources have been
detected within a circular diameter of 25' centred on V1647 Ori, we did not
detect any radio continuum emission from McNeil's nebula. We assign a 5-sigma
upper limit of 0.15 mJy/beam for V1647 Ori where the beam size is 5.6" x 2.7".
Even at higher frequencies of 4.9 and 8.5 GHz (VLA archival data), no radio
emission has been detected from this region. Three scenarios namely, emission
from homogeneous HII region, ionised stellar wind and shock ionised gas, are
explored in the light of our GMRT upper-limit. For the case of homogeneous HII
region, the radius of the emitting region is constrained to be <~ 26 AU
corresponding to a temperature >~ 2,500 K, which is consistent with the
reported radio and H-alpha emission. In the ionised stellar wind picture, our
upper limit of radio emission translates to the ratio of mass loss rate and
terminal velocity, (M_dot/v_infinity) < 1.2-1.8 x 10^(-10) (M_sun/yr)/(km/s).
On the other hand, if the stellar wind shocks the dense neutral (molecular)
cloud, the radio upper limit implies that the fraction of the wind encountering
the dense obstacle is <50%. Based on a recent measurement of X-ray outburst and
later monitoring, the expected radio emission has been estimated. Using our
radio limit, the radius (<~ 36 AU) and electron density (>~ 7.2 x 10^7 cm^(-3)
of the radio emitting plasma have been constrained using a two phase medium in
pressure equilibrium for a volume filling factor of 0.9.
