Previously, it was shown by DeCampli that an isothermal wind of T Tauri stars cannot explain both the mass-loss rates and X-ray observations. Since the assumption of an isothermal wind does not hold in general, we recalculated the structure of a steady and spherically symmetric stellar wind, taking the heating luminosity and its range as input parameters. Our result shows that when the heating luminosity becomes greater than 10−4L⊙, a sonic point lies inside the heating region, contrary to the case of the solar wind. In this case, there exist two solutions for the same heating luminosity and the same mass-loss rate. In one solution, heat is transported by conduction, and in the other solution it is transported by convection. When the heating luminosity is as high as 1 L⊙, the mass-loss rate is about 10−9 ∼ 10−8M⊙ yr−1 . In the former solution, the corona shines with a temperature of about 7 × 107 K and with an X-ray luminosity of about 10−3L⊙, in agreement with X-ray observations. However, the time scale of the angular-momentum loss is greater than 108 yr and this solution, itself, may be insufficient for the angular-momentum loss. This result stems from the smallness of the viscosity coefficient. If global magnetic fields exist, this problem may be solved. In the latter solution, the temperature is at most 4 × 106K, but the time scale of the angular-momentum loss becomes about 107 yr even if magnetic fields do not exist.