We study the possibility of a cool disk existing in the Galactic Center in the framework of the disk-corona evaporation/condensation model .
Assuming an inactive disk near the gravitational capture distance left over from an earlier evolutionary stage , a hot corona should form above the disk since there is a continuous supply of hot gas from stellar winds of the close-by massive stars .
We study the interaction between the disk and the corona .
Whether the cool disk can survive depends on the mass exchange between disk and corona which is determined by the energy and pressure balance .
If evaporation is the dominant process and the rate is larger than the Bondi accretion rate in the Galactic Center , the disk will be depleted within a certain time and no persistent disk will exist .
On the other hand , if the interaction results in hot gas steadily condensing into the disk , an inactive cool disk with little gas accreting towards the central black hole might survive in the Galactic Center .
For this case we further investigate the Bremsstrahlung radiation from the hot corona and compare it with the observed X-ray luminosity .
Our model shows that , for standard viscosity in the corona ( \alpha = 0.3 ) , the mass evaporation rate is much higher than the Bondi accretion rate and the coronal density is much larger than that inferred from Chandra observations .
An inactive disk can not survive such strong evaporation .
For small viscosity ( \alpha \la 0.07 ) we find condensation solutions .
But detailed coronal structure computations show that in this case there is too much X-ray radiation from the corona to be in agreement with the observations .
From this modeling we conclude that there should be no thin/inactive disk presently in the Galactic Center .
However we do not exclude that the alternative non-radiative model of Nayakshin ( 2004 ) might instead be realized in nature and shortly discuss this question .