  In the {\bf K-}essence Vaidya Schwarzschild spacetime, we apply the dynamical
horizon equation to measure the mass-loss due to Hawking radiation and the
tunneling formalism (Hamilton-Jacobi method) to calculate the hawking
temperature. Assuming the Dirac-Born-Infeld kind of non-standard action for the
{\bf K-}essence here, the background physical spacetime is a static spherically
symmetric black hole, and we constrain the {\bf K-}essence scalar field to be a
function only of either forward or backward time. The {\bf K-}essence emergent
gravity and the generalizations of Vaidya spacetime have been linked by Manna
et al. In this paper, we use Sawayama's modified description of the dynamical
horizon to show that the obtained findings deviate from the standard Vaidya
spacetime geometry.
