[논문]STARS: A 3D GRID-BASED MONTE CARLO CODE FOR RADIATIVE TRANSFER THROUGH RAMAN AND RAYLEIGH SCATTERING WITH ATOMIC HYDROGEN

Chang, Seok-Jun; Lee, Hee-Won

doi:10.5303/jkas.2020.53.6.169

[국내논문] STARS: A 3D GRID-BASED MONTE CARLO CODE FOR RADIATIVE TRANSFER THROUGH RAMAN AND RAYLEIGH SCATTERING WITH ATOMIC HYDROGEN 원문보기

Journal of the Korean astronomical society = 천문학회지, v.53 no.6, 2020년, pp.169 - 179

Chang, Seok-Jun (Department of Physics and Astronomy, Sejong University) , Lee, Hee-Won (Department of Physics and Astronomy, Sejong University)

Abstract ▼ AI-Helper

Emission features formed through Raman scattering with atomic hydrogen provide unique and crucial information to probe the distribution and kinematics of a thick neutral region illuminated by a strong far-ultraviolet radiation source. We introduce a new 3-dimensional Monte-Carlo code in order to describe the radiative transfer of line photons that are subject to Raman and Rayleigh scattering with atomic hydrogen. In our Sejong Radiative Transfer through Raman and Rayleigh Scattering (STaRS) code, the position, direction, wavelength, and polarization of each photon is traced until escape. The thick neutral scattering region is divided into multiple cells with each cell being characterized by its velocity and density, which ensures flexibility of the code in analyzing Raman-scattered features formed in a neutral region with complicated kinematics and density distribution. To test the code, we revisit the formation of Balmer wings through Raman scattering of the far-UV continuum near Lyβ and Lyγ in a static neutral region. An additional check is made to investigate Raman scattering of O vi in an expanding neutral medium. We find a good agreement of our results with previous works, demonstrating the capability of dealing with radiative transfer modeling that can be applied to spectropolarimetric imaging observations of various objects including symbiotic stars, young planetary nebulae, and active galactic nuclei.

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표/그림 (8)

그림 Figure 1. Schematic illustrations of energy levels and elec-tronic transitions associated with Raman and Rayleigh scat-tering of far-UV radiation with a hydrogen atom.
그림 Figure 2. Flow chart of STaRS.
그림 Figure 3. The total scattering cross section (black), and the branching ratio to n = 2 (blue) and n = 3 (red) computed in Chang et al. (2015).
그림 Figure 4. Schematic illustration of the computations of the next scattering position in the grid-based simulation.
그림 Figure 5. Schematic illustrations of the two cases used to test the code.
그림 Figure 6. Raman conversion efficiency of Hα (left panel) and Hβ (right panel) broad wings for the static spherical case. The black solid lines are the spectra given by an analytic method. The red, blue, and green open circles are the spectra given by STaRS for N_xyz = 3, 10, and 100.
그림 Figure 7. Surface brightness (left), degree of polarization (center), and direction of polarization (right) of the projected Hα photons. The panels in the first, second, and third rows represent the results obtained using STaRS for N_xyz = 3, 10, and 100, respectively. The bottom panels represent the result obtained using an analytic method.
그림 Figure 8. Line formation of Raman OVIλ6825 features in an expanding H I region for three different optical depths. The blues olid lines are computed by STaRS. The red dashed lines are the results of Figure 6 in Lee & Lee (1997).

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