PHOTON LOSS FROM THE HELIUM LY-ALPHA LINE - THE KEY TO THE ACCELERATION OF WOLF-RAYET WINDS

It is demonstrated that the ionization equilibrium of helium in non-LT E atmospheres for Wolf-Rayet stars is very sensitive to photon loss fr om the He II Ly alpha line. A removal of 0.001% of the photons is suff icient to initiate an abruptly recombining ionization equilibrium. The assumption of photon loss allows to address the wind momentum problem of Wolf-Rayet stars. It is possible for the first time to construct a line blanketed non-LTE model of a Wolf-Rayet star that reproduces the observed spectrum and simultaneously, provides the radiation force to drive its outer velocity structure. A method is developed to determin e the free model parameters L, R-phot, M, v(infinity) v(phot), C (clum ping factor), and f (photon loss factor), by an analysis of an observe d Wolf-Rayet spectrum. The method is applied to the spectrum of the WN 5 star HD 50896 resulting in good fits in shape and strength to the ob served helium emission lines. In particular the profile of the He I la mbda 10830 line, which is a tracer of the outer velocity structure, is reproduced remarkably well. The hydrodynamically calculated velocity law differs significantly from the commonly adopted beta-law with beta = 1. The outer part can be approximated by a beta-law with beta = 3 i f the core radius of the atmosphere model is used, or by beta = 8, if the velocity law is calculated referring to the hydrostatic radius of a stellar evolution model in the Wolf-Rayet phase. Close to the photos phere the velocity structure is flat with an expansion velocity of v(p hot) approximate to 1100 km s(-1). The resulting luminosity L = 5.5 . 10(5) Lo and terminal wind velocity v(infinity) = 2060 km s(-1) are fo und to be considerably larger than the values from previous determinat ions. On the other hand, the mass loss rate is lower M = 3.2 . 10(-5) M. yr(-1) due to an inhomogeneous wind with a clumping factor C approx imate to 4. There is evidence for a decrease of the clumping factor wi th distance from the star. The photon loss factor is determined empiri cally to have a value of f approximate to 10(-4). It is proposed that a Bowen resonance-fluorescence mechanism removes a small fraction of p hotons from the radiation field of the helium Ly alpha resonance line. Photon loss calculated theoretically from the interaction of metal li nes close in wavelength to the He II Ly alpha line yields a depth depe ndent factor in the range 10(-4)...10(-3). In the recombination zone, where the photon loss influences the ionization structure, its value i s f approximate to 10(-4) in excellent agreement with the empirically determined value. The lines Ca V lambda 303.74, Fe VI lambda lambda 3 03.70, 303.80, 303.83, and O III lambda 303.80 are roughly of equal im portance. The wind momentum calculated by the present model exceeds th e single scattering limit by a factor of 6 in contrast to previous est imates that yielded factors 50 - 100. With a momentum ratio of 6 the W olf-Rayet winds are no longer distinct from other radiation driven win ds but they fit as more extreme versions to the winds of O stars.