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S. Sahal - Bréchot Observatoire de Paris, LERMA CNRS UMR 8112, France

The STARK-B database for spectral line broadening by collisions with charged particles in the framework of the European project VAMDC (Virtual Atomic and Molecular Data Center). S. Sahal - Bréchot Observatoire de Paris, LERMA CNRS UMR 8112, France. http:// www.vamdc.org.

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S. Sahal - Bréchot Observatoire de Paris, LERMA CNRS UMR 8112, France

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  1. The STARK-Bdatabasefor spectral line broadeningby collisionswithchargedparticlesin the framework of theEuropeanprojectVAMDC(Virtual Atomic and Molecular Data Center) S. Sahal-Bréchot Observatoire de Paris, LERMA CNRS UMR 8112, France http://www.vamdc.org http://stark-b.obspm.fr

  2. http://www.ivoa.net STARK-BDatabase for "Stark" widths and shifts of isolatedspectral lines of atoms and ions, due to collisionswithelectrons and ions in a plasmahttp://stark-b.obspm.fr • Calculatedwidths and shifts:more than 150 pubs (1984-2011) • SCP theoryupdated and operated • by M.S. Dimitrijević and S. Sahal-Bréchot and colleagues • Technical development: • Paris Observatory, LERMA, by N. Moreau, engineer • the database has been openedsinceSeptember 2008: 99% of the existing data are currentlyimplemented • It is a part of the atomic and molecular databases of the Paris Observatory • Link (and mirror site in progress) to SerVO - Serbian Virtual Observatory • http://servo.aob.rs/~darko/ • It is a part of VAMDC- Virtual Atomic and Molecular Data Centre • it follows the standards of VAMDC and Virtual Observatories • (Europe: IVOA International Virtual Observatory Alliance) http://www.vamdc.org 2

  3. STARK-Bwidthsand shifts of isolated spectral linesof atoms and ions, due to collisions withelectrons and ions in a plasma Stark broadening of spectral linescanbeapplied to manysubjects Overlappinglines and departuresfrom impact approximation are outside the scope of STARK-B • Astrophysics • Laboratory plasmas • Industrialplasmas • Ionizationdegree ≥ 1% • Moderately hot to very hot plasmas (5 103 to ∼106 K) • Moderateelectrondensity (1013 to 1022 cm-3 )

  4. Diagnostics and Modelling in Astrophysics:Understandingof the evolution of stars • Thanks to considerabledevelopments of • Groundbased and space-born missions • Increasedsensitivity (S/N) and spectral resolution • Powerfulcomputers Interpretationof the faintobservedspectrum: faintobjects, faintlines (trace elements) • Line intensities+ line profiles • Continuum • Spectroscopic diagnostics: • Temperatures • pressure • Abundances • Chemical stratification of the atmosphere Modellingof atmospheres • Syntheticspectra: a greatnumber of lines of a sameelement are required • Radiative transfer Stellarinteriorsstudies and Asterosimology • opacities: a greatnumber of lines oh higlyionizedelements are required • Nuclearprocesses: formation of elements, chemicalenrichment

  5. Diagnostics and Modelling in Astrophysics:Understandingof the evolution of stars • Thanks to considerabledevelopments of • Groundbased and space-born missions • Increasedsensitivity (S/N) and spectral resolution • Powerfulcomputers Interpretationof the faintobservedspectrum: faintobjects, faintlines (trace elements) • Line intensities+ line profiles • Continuum • Spectroscopic diagnostics: • Temperatures • pressure • Abundances • Chemical stratification of the atmosphere Modellingof atmospheres • Syntheticspectra: a greatnumber of lines of a sameelement are required • Radiative transfer Stellarinteriorsstudies and Asterosimology • opacities: a greatnumber of lines oh higlyionizedelements are required • Nuclearprocesses: formation of elements, chemicalenrichment

  6. Sun abundances Diagnostics and Modelling in Astrophysics:Understandingof the evolution of stars • Thanks to considerabledevelopments of • Groundbased and space-born missions • Increasedsensitivity (S/N) and spectral resolution • Powerfulcomputers Interpretationof the faintobservedspectrum: faintobjects, faintlines (trace elements) • Line intensities+ line profiles • Continuum • Spectroscopic diagnostics: • Temperatures • pressure • Abundances • Chemical stratification of the atmosphere Modellingof atmospheres • Syntheticspectra: a greatnumber of lines of a sameelement are required • Radiative transfer Stellarinteriorsstudies and Asterosimology • opacities: a greatnumber of lines oh higlyionizedelements are required • Nuclearprocesses: formation of elements, chemicalenrichment

  7. Diagnostics and ModellinginLaboratory and Industrial plasmas • Thanks to developments and needs (devices an research) • Magnetic confinement fusion: moderately dense and hot plasmas (e.g. ITER) • Inertial confinement fusion (laser fusion, ion-beam fusion): dense and very hot plasmas • Lowtemperatures plasmas • Lightingdischarges Analysis and interpretation of the spectrum in fusion devices and Tokamaks • Light elements in the divertor and edge plasma regions • Importance of Tin, Tungsten, and Aluminium (Al-pellet Ablation Plasmas in Large HelicalDevice) • Temperatures • Pressure Progress in low-energy light sources • Dischargelamps and lighting: • optimisation of performances • cold light from hot atoms and molecules • (white light 3000-5000K, discharge up to 45000K), • highelectrondensity (strong and broademission in the visible spectrum • Fluorescent lamps: improvingefficacity (phosphors) • Rare earthelements Dy, Ho, Ce: excellent radiation sources • HID (High IntensityDischarge): MH (MetalHalide) lamps, e.g. Dy I3, In I, ZnI3 • (LED light-emitting diodes)

  8. i’ i i’ f’ f f’ STARK-B data: Basic approximations (theoryand calculations) • Impact approximation • Collisions betweenradiators and perturbers • actindependently and are additive ρtyp/v << ΔTi.e. ρtyp<< N-1/3 • Complete collision approximation • line broadeningtheorybecomes • an application of the theory of collisions The atom has no time to emit or absorb a photon during the collision process, the collision is not brokenoff. • Isolatedlines • Neighbouringlevels do not overlap •  Lorentz profile; S-matrix, cross-sections • LS coupling: fine (hyperfine) structure • canbeneglectedduringthe collision • (S or I : no time to rotate) • The fine structure (hyperfine) components have the • samewidth and the same shift, thet of the multiplet • High densities: • Debye screening effect 8

  9. STARK-BMethodsof calculations of the data1. The scatteringS-matrix • SCP: Semi-Classical : atom = quantum description (atomic structure), perturber= particlemoving on a classicalpath + Perturbation theory (2ndorder) • (Sahal-Bréchot, A&A1970 and furtherpapers, 6-8 basic papers) • unitarityand symmetrization of the S-matrix, adequatecut-offs • hyperbolae for ion-electron and ion-ion (1970), • complexatoms (1974), verycomplex (2008) • Feshbachresonances for ion-electron collisions (1977) • Updated and operatedwith MS. Dimitrijević (1984 and after) • accuracy: 20%, sometimesbetter, sometimesworse • MSE: ModifiedSemi-Empirical: atom = simplified quantum description Dimitrijevićand colleagues, JQSRT1980 and further A&A papers)

  10. STARK-B Methodsof calculations of the data 2 - The atomic structure • NIST atomicdata • VALD (Vienna Atomic Line Database) • Coulomb approximation with quantum defect(Bates & Damgaard 1949) • TOPbase: R-matrix in LS coupling • Cowan code : HFS multi-confwith exchange and relativisticeffects (by perturbations) • SUPERSTRUCTURE : scaledThomas-Fermi-Dirac-Amaldipotential + relativisticeffects (Breit-Pauli)

  11. STARK-BMethodsof calculations of the data3. Calculationsleading to a greatnumber of data Atomic structure coupled to the S-matrix calculation: Manywidths and shifts for a set of severaltemperatures and densities in a samerun • Ab initiocalculations: no external data insertion • SST + SCP: data for 100 lines and more in a samerun • Cowan code + SCP : in progress (case of Pb IV, more than 100 lines in a samerun) • Coupling to atomic structure databases: • TopBase: data for 150 linesin a samerun • VALD: data for more than 1000 linesin a samerun (case of CII for white dwarfs)

  12. STARK-B: Elements (atoms and ions) currentlyinserted Ag I, Al I, Al III, Al XI Ar I, Ar II, Ar II, Ar VIII Au I B II, B III Ba I, Ba II Be I, Be II, Be III Br I C II, C III, C IV, C V Ca I, Ca II, Ca V, Ca IX, Ca X Cd I, Cd II Cl I, Cl VII Cr I, Cr II Cu I F I, F II, F III ,F IV, F V, F VI, F VII Fe II Ga I GeI He I Hg II I I In II, In III K I, K VIII, K IX Kr I, Kr II, Kr VIII Li I, Li II Mg I, Mg II, Mg XI Mn II N I, N II, N III, N IV, N V Na I, Na X Ne I, Ne II, Ne II, Ne III, Ne IV, Ne V, Ne VIII Ni II O I, O II, O III (in progress), O IV, O V, O VI; O VII P IV, P V Pb IV Pd I Rb I S III, S IV, S V, S VI Sc III, Sc X, Sc XI Se I Si I, Si II, Si IV, Si V, Si VI, Si XI, Si XII, Si XIII Sr I Te I Ti IV, Ti XII, Ti XIII Tl III V V, V XIII Y III Zn I C II in progress (150 lines, 4 temperatures, 3 densities)

  13. STARK-B http://stark-b.obspm.fr

  14. STARK-B: Nextsteps • Insertion of MSE data • Insertion of little “applets” on line for users: • Fittingalongtemperatures (for astrophysics) • extrapolation or interpolation (regularities and systematic trends) • along principal quantum numbers, • charge of the radiating ions (isoelectronicsequences), • homologous ions, • charge of the ion collider • Future: • SCP code on line: STARK-C project • Insertion of quantum data in intermediatecoupling: SST + DW • especiallyadapted to highlycharged ions and resonancelines(Sahal-BréchotwithElabidi & Ben Nessib (2004 and after, an alsowithDubau and Cornille 2007 and after )

  15. VAMDC projectVirtual Atomic and Molecular Data Center • EuropeanprojectFP7 "ResearchInfrastructures • summer 2009 - end of 2012 • Interoperablee-Infrastructure • for exchange of atomic and moleculardata • 15 administrative partners: 24 teams • from6 European Union member states, • Serbia, RussianFederation and Venezuela • strongcoupling • to the users(astrochemistry, atmosphericphysics, plasmas) • scientists and engineersfrom the ICT community(Information and Communication Technologies) • usedto deal withdeployinginteroperable e-infrastructure • e.g. Europlanet IDIS • IVOA (International Virtual Observatory Alliance) • Members: Euro-VO, AstroGrid… http://www.vamdc.org http://www.vamdc.eu

  16. VAMDC: portal user http://portal.vamdc.org/vamdc_portal_test/home.seam

  17. Query

  18. Query by species

  19. Query by species: atom

  20. Query by species: atom (following)

  21. Query by species: atom, processes

  22. Query by species: atom, processes (following)

  23. Query: result, click on download Xsams: XML Schema for Atoms, Molecules and Solids XML: Extensible MarkupLanguage Xsams2SME: convertsXML document into the CSV-format wanted by Spectroscopy Made Easy (SME)

  24. Result of the download:code in XML language for users Xsams XML Schema for Atoms, Molecules and Solids

  25. Thankyou for your attention

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