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ESCAPE OF RESONANTLY SCATTERED LYβ AND Hα FROM HOT AND OPTICALLY THICK MEDIA KCI 등재 SCOPUS
- 언어ENG
- URLhttps://db.koreascholar.com/Article/Detail/383907
pp.5-16
We investigate the escape of Lyβ from emission nebulae with a significant population of excited hydrogen atoms in the level n = 2, rendering them optically thick in Hα. The transfer of Lyβ line photons in these optically thick regions is complicated by the presence of another scattering channel leading to re-emission of Hα, alternating their identities between Lyβ and Hα. In this work, we develop a Monte Carlo code to simulate the transfer of Lyβ line photons incorporating the scattering channel into Hα. Both Hα and Lyβ lines are formed through diffusion in frequency space, where a line photon enters the wing regime after a fairly large number of resonance scatterings with hydrogen atoms. Various line profiles of Hα and Lyβ emergent from our model nebulae are presented. It is argued that the electron temperature is a critical parameter which controls the flux ratio of emergent Lyβ and Hα. Specifically for T = 3 × 104 K and Hα line center optical depth α = 10, the number flux ratio of emergent Lyβ and Hα is ∼ 49 percent, which is quite significant. We propose that the leaking Lyβ can be an interesting source for the formation of Hα wings observed in many symbiotic stars and active galactic nuclei. Similar broad Hα wings are also expected in Lyα emitting halos found in the early universe, which can be potentially probed by the James Webb Telescope in the future.
1. INTRODUCTION
2. MONTE CARLO APPROACH TO RADIATIVETRANSFER
2.1. Atomic Physics
2.2. Monte Carlo Approach
3. LINE TRANSFER OF Hα AND LYβ
3.1. Dependence on Line Center Optical Depth andTemperature
3.2. Flux Ratios in (τ − T) Space
3.3. ProfileWidths of Hα AND LYβ
3.4. Scattering Numbers of Hα AND LYβ
4. APPLICATION TO BROAD Hα WINGS INSYMBIOTIC STARS
5. SUMMARY AND DISCUSSION
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