spectral line broadening meaning in English
谱线增宽
Examples
- So it is necessary to seek new theories to explain the spectral lines broadening of stars
这样，寻求新的理论解释恒星光谱线的加宽成为必要。 - The historical retrospect of physical mechanisms of spectral lines broadening in stars is presented
本文对引起恒星光谱线加宽的物理机制作了回顾。 - Thus , the nonthermal broadening in the stars " spectral lines above has been explained abstractly by the theory of spectral lines broadening in plasmas
因此，等离子体谱线致宽理论对以上恒星谱线非热加宽给予了理论解释。 - The turbulent effects of plasmas 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 fexiva5303 in corona has been calculated
进一步以日冕绿线f _ exiv 5303为例，计算了它的等离子体加宽值对应的湍动区尺度，发现与实际日冕尺度相符。 - 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 of and fraunhoferx 3704 in corona , fj / a4923 . 9 in dwarf nova oy car and f . / a4934 in the variable star rr lyrae
本文从等离子体波与波相互作用观点出发，由高频电磁波辐射转移方程导出了引起谱线宽度变化的偏微分方程，编写fortran程序求解偏微分方程的数值解，具体计算了日冕绿线f _ exiv 5303和夫朗禾费线3704 、矮新星oycarf _ eii 4923 . 9 、天琴rr型变星f _ ei 4934的谱线加宽值，对以上各谱线加宽中的等离子体致宽效应作了初步计算。