3. Observed O VI 1032, 1038 Å Deviation from 2:1 flux ratio ranges from 1:1 to 2:1 What is going on? Atomic Structure for the S-P Doublet O IV 1032, 1038

4. Atomic structure of Li-like Ions C IV 1548, 1551 Å N V 1238, 1243 Å O VI 1032, 1038 Å In the optically thick medium, the doublet flux ratio approaches unity. Resonance Doublet

5. SPH simulation by Mastrodemos and Morris (1998)

7. Raman Scattering by H

8. Raman 6825 is expected to be stronger than 7082 by a factor of about 6. Two factors are involved. One is the cross section, and the other is the flux ratio of resonance doublets. 2 nd Order Time Dependent Perturbation Theory-Kramers-Heisenberg Formula Rayleigh Scattering Raman Scattering 1. Raman scattering operates in the presence of a thick neutral component in the vicinity of a strong far UV emission source. 2. HI is provided by the Giant and OVI by the white dwarf.

10. Multiple peak profiles are consistent with the accretion flow and the bipolar outflow around the white dwarf. The accretion disk is responsible for the main double peaks. The bipolar outflow provides an additional red peak in the case of the triple peak profile.

11. 1. D type symbiotic star with a Mira companion. 2. Slow nova eruption in 1965 3. Oribtal period of tens of years 4. Suggested orbital separation of 80 AU 5. Shows strong Raman O VI 6825 and 7082 with a double-peak profile. Spectrum of V1016 Cyg (CFHT, 2014) FUSE, 2000, OVI 1032

12. Adopting an accretion disk model, we may explain a double peak profile Accretion flow tends to be convergent on the entrance side and divergent on the opposite side. Overall, we will get red asymmetric double peak profile. Single Profile Analysis WD Accretion Disk H I Region

14. SPH by Mastrodemos and Morris (1998)

15. 1. Profile fitting of the two Raman O VI features incorporating local variation of emissivities. 2. Locally varying OVI 1032: 1038 flux ratios. OVI 1032 OVI 1038

16. Raman 6825 of V455 Sco