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.

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.

Semiclassical theory

(Sahal-Bréchot, 1969ab) (Sahal-Bréchot, 1974; 1991; Fleurier et al. 1977;

Dimitrijević & Sahal-Bréchot, 1984a;1996; Dimitrijević et al. 1991)

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)

Chemically Peculiar Stars

Results and Discussion

Te I

(Z=52) 5p4 3P2

- 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

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

Cr II (Z=24) 3d5 6S5/2

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.

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.

Au II (Z=79) 5d10 1S0

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

Cu III

(Z=29) 3d9 2D5/2

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

Zn III

(Z=30) 3d10 1S0

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

Se III

(Z=34) 4p2 3P0

- 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

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 prechosenoptical depth points at the standard wavelength λs=5150 Ǻ (τs=5150) are used in Wickramasinghe (1972) and here.

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

Sn III

(Z=50) 5s2 1S0

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

The Stark broadening parameters obtained here, contributealso to the creation of a set of such data for as largeas possible number of spectral lines, of significance for anumber of problems in astrophysical, laboratory and technologicalplasma research.

Thank you for attention!