  We consider marginally trapped surfaces in a spherically symmetric spacetime
evolving due to the presence of a perfect fluid in D-dimensions and look at the
various definitions of the surface gravity for these marginally trapped
surfaces. We show that using Einstein equations it is possible to simplify and
obtain general formulae for the surface gravity in terms of invariant
quantities defined at these marginally trapped surfaces like area radius,
cosmological constant and principal values of the energy-momentum tensor
\r{ho}, p. We then correlate these expressions of surface gravity to the cases
of dynamical horizons and timelike tubes and find which proposals of surface
gravity are causally sensitive as these surfaces undergo causal transitions
from spacelike to timelike and vice versa.
