Cooling of Young Stars Growing by Disk Accretion

摘要: In the initial formation stages young stars must acquire a significant fraction of their mass by accretion from circumstellar disk that forms in center collapsing protostellar cloud. Throughout this period rates reach 10−6 to 10−5 M☉ yr−1, allowing extend all way stellar surface unimpeded magnetic field. We study effect irradiation produced hot inner on properties accreting fully convective low-mass and also look at objects such as brown dwarfs giant planets. At high raises temperature equatorial region above photospheric T0 star would have absence accretion. these regions an almost isothermal outer radiative zone top interior, leading suppression local internal cooling flux derived contraction (similar occurs irradiated ``hot Jupiters''). The high-latitude (polar) parts surface, where is weak, preserve level T0. total intrinsic luminosity integrated over whole reduced compared nonaccreting case, up factor several for some (young dwarfs, quasar disks, forming planets), potentially retardation contraction.