Abstract
It is known that most stars lose mass through stellar wind. Thermal mass loss is impossible at photospheric and chromospheric temperatures. Coronal temperature makes the thermal contribution significantly significant, but additional mechanisms for particle acceleration from the chromosphere and coronal heating are required, such as radiation pressure, MHD, anomalous strong ambipolar diffusion, or Coulomb acceleration, which go beyond the hydrostatic model. Comparison of the mass loss rate in the tails of the distribution function with actual observed values for increasing main-sequence stars, even at coronal temperatures, indicates an increasing excess of actual mass loss over the gravitational limit. All stars exhibiting a persistently high mass loss rate exceeding gravitational confinement can be classified as nonrelativistic white holes.