What determines when and how long a star moves from the Hayashi track to the Henyey track is heavily dependent on its initial mass. Stars that are massive enough (0.6 solar mass) will deviate onto the Henyey Track, depicted as a near-horizontal line on an HR diagram. A core that becomes sufficiently hot enough will become less opaque, making convection inefficient. The core will instead become fully radiative to transfer its thermal energy. During this phase the luminosity stays constant or gradually increases, with the temperature increasing as the core undergoes radiative contraction. At the end of the track, the star will undergo nuclear burning, however, will experience a dip in luminosity, until it reaches the main sequence.