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Stark-B Database Virtual Atomic and Molecular Data Center (VAMDC) and

Stark-B Database Virtual Atomic and Molecular Data Center (VAMDC) and Data for White Dwarf Atmospheres Analysis Zoran Simić and Milan S. Dimitrijević Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia. VAMDC Project

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Stark-B Database Virtual Atomic and Molecular Data Center (VAMDC) and

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  1. Stark-B Database Virtual Atomic and Molecular Data Center (VAMDC) and Data for White Dwarf Atmospheres Analysis Zoran Simić and Milan S. Dimitrijević Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia

  2. VAMDC Project VAMDC aims at building an interoperable e-Infrastructure for the exchange of atomic and molecular data. VAMDC is a complex project involving 15 administrative partners representing 24 teams from 6 European Union member states, Serbia, the Russian Federation and Venezuela. VAMDC is supported by EU in the framework of the FP7 "Research Infrastructures - INFRA-2008-1.2.2 - Scientific Data Infrastructures" initiative. It started on the 1rst of July for a duration of 42 months.

  3. With the development of astronomical observations from space, trace elements can now be identified in stellar spectra. Here, we investigated theoretically the influence of collisions with charged particles on heavy metal spectral line profiles for neutral emitter Te I, singly charged emitters Cr II, Mn II and Au II and doubly charged emitters Cu III, Zn III, Se III, In III and Sn III in spectra of chemically peculiar stars, especially in A stars and white dwarfs.

  4. Semiclassical theory (Sahal-Bréchot, 1969ab) (Sahal-Bréchot, 1974; 1991; Fleurier et al. 1977; Dimitrijević & Sahal-Bréchot, 1984a;1996; Dimitrijevićet al. 1991)

  5. When SC theory can not be applied in an adequate way, due to the lack of reliable atomic data: modified semiempirical theory (Dimitrijević& Konjević, 1980; Dimitrijević & Kršljanin, 1986)

  6. Chemically Peculiar Stars

  7. Results and Discussion Te I (Z=52) 5p43P2 - Yuschenko & Gopka, (1996): photosphere - WD Procyon (CMi) - Chayer et al. (2005a): photosphere - cool WD DO type: HD 149499 B & HZ 21 SC theory (Sahal-Bréchot, 1969ab; Dimitrijević & Sahal-Bréchot, 1996) 4 spectral lines N=1016 cm-3; T [2500, 50000] K - there are no other theoretical and experimental data

  8. Thermal Doppler and Stark widths for Te I 5125.2 and 9903.9 Å spectral lines for a DB white dwarf atmosphere model: Teff = 15000 K, log g = 7 (Wickramasinghe 1972), as a function of optical depth τ5150

  9. Cr II (Z=24) 3d56S5/2 SC theory (Sahal-Bréchot, 1969ab; Dimitrijević & Sahal-Bréchot, 1996) *7 strongest 4s-4p multiplets, N=1014 cm-3; T [2500, 100000] K 9 resonant 3d5-3d44p multiplets, N=1017 cm-3; T [ 2500, 100000] K *Dimitrijević, M.S., Ryabchikova, T., Simić, Z., Popović, L.Č., & Dačić, M., 2007, A&A, 469, 681.

  10. Mn II (Z=25) 4s 7S3 SC theory (Sahal-Bréchot, 1969ab; Dimitrijević & Sahal-Bréchot, 1996) *6 sp. lines, N=1017 cm-3; T [5000, 100000] K *Popović, L.Č., Dimitrijević, M.S., Simić, Z., Dačić, M.,Kovačević, A., & Sahal-Bréchot, S., 2008, New Astronomy, 13, 85.

  11. Au II (Z=79) 5d101S0 Popović et al. (1999b): 8 Au II multiplets, N=1017 cm-3; T [5000, 50000] K MSE theory (Dimitrijević& Konjević, 1980; Dimitrijević& Kršljanin, 1986) Rafael Mayo, Monserat Ortiz, Milan S. Dimitrijević and Zoran Simić: new experimental data and comparison with theoretical-to be published

  12. Cu III (Z=29) 3d92D5/2 MSE theory (Dimitrijević& Konjević, 1980; Dimitrijević& Kršljanin, 1986) *Stark widths for 6 transitions 3d84s - 3d84p N=1017 cm-3; T [10000, 300000] K *Simić, Z., Dimitrijević, M.S., Popović, L.Č., & Dačić, M., 2006b, New Astronomy, 12, 187. ◦ there are no other theoretical and experimental data

  13. Zn III (Z=30) 3d101S0 MSE theory (Dimitrijević& Konjević, 1980; Dimitrijević& Kršljanin, 1986) *Stark widths for 6 transitions 3d94s - 3d94p N=1017 cm-3; T [10000, 300000] K *Simić, Z., Dimitrijević, M.S., Popović, L.Č., & Dačić, M., 2006b, New Astronomy, 12, 187. ◦ there are no other theoretical and experimental data

  14. Se III (Z=34) 4p23P0 - Chayer et al. (2005ab): atmosphere of cool WD DO type MSE teorija (Dimitrijević& Konjević, 1980; Dimitrijević& Kršljanin, 1986) *Stark widths for 3 transitions 5s - 5p N=1017 cm-3; T [10000, 300000] K *Simić, Z., Dimitrijević, M.S., Popović, L.Č., & Dačić, M., 2006b, New Astronomy, 12, 187. ◦ there are no other theoretical and experimental data

  15. WD atmosphere model (Teff= 15 000 K, log g = 7) (Wickramasinghe, 1972) Cu III 1774.4 Å, Zn III 1667.9 Å & Se III 3815.5 Å For the considered model atmosphere of the DB white dwarfs, the prechosen optical depth points at the standard wavelength λs=5150 Ǻ (τs=5150) are used in Wickramasinghe (1972) and here.

  16. In III (Z=49) 5s 2S1/2 SC teorija (Sahal-Bréchot, 1969ab; Dimitrijević & Sahal-Bréchot, 1996) 10 multiplets, N=1017 cm-3; T [10000, 100000] K

  17. Sn III (Z=50) 5s21S0 SC theory (Sahal-Bréchot, 1969ab; Dimitrijević & Sahal-Bréchot, 1996) 4 sp. lines, N=1017 cm-3; T [10000, 150000] K MSE theory (Dimitrijević& Konjević, 1980; Dimitrijević& Kršljanin, 1986) N=1017 cm-3; T [2500, 50000] K

  18. The Stark broadening parameters obtained here, contribute also to the creation of a set of such data for as large as possible number of spectral lines, of significance for a number of problems in astrophysical, laboratory and technological plasma research.

  19. Thank you for attention!

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