  Cygnus OB2 is the most massive association within 2kpc from the Sun, hosting
hundreds of massive stars, thousands of young low mass members, and some sights
of active star formation in the surrounding cloud. Recently, 10
photoevaporating proplyd-like objects with tadpole-shaped morphology were
discovered in the outskirts of the OB association, approximately 6-14pc away
from its center. The classification of these objects is ambiguous, being either
evaporating residuals of the parental cloud which are hosting a protostar
inside, or disk-bearing stars with an evaporating disk, such as the evaporating
proplyds observed in the Trapezium Cluster in Orion. In this paper we present a
study based on low resolution optical spectroscopic observations made with the
Optical System for Imaging and low Resolution Integrated Spectroscopy (OSIRIS),
mounted on the 10.4m Gran Telescopio CANARIAS (GTC), of two of these
protostars. The spectrum of one of the objects shows evidence of accretion but
not of outflows. In the latter object, the spectra show several emission lines
indicating the presence of an actively accreting disk with outflow. We present
estimates of the mass loss rate and the accretion rate from the disk, showing
that the former exceeds the latter as observed in other known objects with
evaporating disks. We also show evidence of a strong variability in the
integrated flux observed in these objects, as well as in the accretion and
outflow diagnostics.
