Physics – Atomic Physics
Scientific paper
Jun 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003jkas...36...55l&link_type=abstract
Journal of the Korean Astronomical Society, vol. 36, no. 2, pp. 55-60
Physics
Atomic Physics
Scattering, Binaries: Symbiotic, Stars: Individual (Rr Tel), Radiative Transfer, Atomic Physics
Scientific paper
In Lee, Kang & Byun (2001) the discovery of Raman scattered 6545 Å feature was reported in symbiotic stars and the planetary nebula M2-9. The broad emission feature around 6545 Å is formed as a result of Raman scattering of He II n=6--> n=2 photons by atomic hydrogen. In this paper, we introduce a method to compute the equivalent width of He II λ 1025 line and present an optical spectrum of the symbiotic star RR Telescopii as an example for a detailed illustration. In this spectrum, we pay attention to the broad Hα wings and the Raman scattered He II 6545 feature. The broad Hα wings are also proposed to be formed through Raman scattering of continuum around Lyβ by Lee (2000), and therefore we propose that the equivalent width of the He II λ 1025 emission line is obtained by a simple comparison of the strengths of the 6545 feature and the broad Hα wings. We prepare a template Hα wing profile from continuum radiation around Lyβ with the neutral scattering region that is supposed to be responsible for the formation of Raman scattered He II 6545 feature. Isolation of the 6545 feature that is blended with [N II] λ 6548 is made by using the fact that [N II] λ 6584 is always 3 times stronger than [N II] λ 6548. We also fit the 6545 feature by a Gaussian which has a width 6.4 times that of the He II λ 6527 line. A direct comparison of these two features for RR Tel yields the equivalent width EWHe1025=2.3 Å of He II λ 1025 line. Even though this far UV emission line is not directly observable due to heavy interstellar extinction, nearby He II lines such as He II λ 1085 line may be observed using far UV space instruments, which will verify this calculation and hence the origins of various features occurring in spectra around Hα.
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