$H{\alpha}$ - $Ly{\beta}$ Formation in Optically Thick Medium

Symbiotic stars and quasars exhibit prominent $H{\alpha}$ emission lines often accompanied with broad wings. $H{\alpha}$ emission nebulae in these objects are proposed to be optically thick to resonance scattering. The transfer of $H{\alpha}$ line photons are further complicated by the existence of another scattering channel leading to re-emission of $Ly{\beta}$. In this work are develop a Monte Carlo code to simulate the transfer of $H{\alpha}$ line photons incorporating the scattering channel into $Ly{\beta}$. We show various line profiles of $H{\alpha}$ and $Ly{\beta}$ emergent from our model nebulae. It is shown that temperature is a critical parameter which controls the ratio of emergent $Ly{\beta}$ flux to that of $H{\alpha}$.