The Spectrum Of Plasma Waves And Wave Interactions Widening

The historical retrospect of physical mechanisms of spectral lines broadening in stars is presented. From the past research work, it has been known that the main mechanisms of spectral lines broadening in the atmospheres of stars are Doppler broadening, spectral lines broadening by rotation and expending, pressure broadening (Stark broadening) , natural broadening, spectral lines broadening in magnetic field, sonic waves and Alfv e n waves broadening, etc. But it is not enough to explain the recent observation phenomena by above theories of spectral lines broadening. The differences between observation data and theoretical data still exist. So it is necessary to seek new theories to explain the spectral lines broadening of stars.Based on the viewpoint of interaction between waves in plasmas, the partial differential equation that causes the spectral lines broadening has been deduced from radiation transfer equation of high-frequency electromagnetic waves in plasmas. The numerical solution has been obtained by using the FORTRAN program we compiled. We concretely calculated the spectral lines widths ofand FraunhoferX 3704 in Corona, FJ/A4923.9 in dwarf nova OY Car and F./A4934 in the variable star RR Lyrae. The turbulent effects ofplasmas in above spectral lines broadening have been calculated primarily. Furthermore, as an example, the turbulent region scale that corresponds to the turbulent broadening value of FeXIVA5303in Corona has been calculated. It has been found that the turbulentregion scale is corresponding with the actual Corona's scale. Thus,the nonthermal broadening in the stars' spectral lines above has beenexplained abstractly by the theory of spectral lines broadening in plasmas.