UCL DEPT. OF SPACE & CLIMATE PHYSICS SOLAR & STELLAR PHYSICS GROUP Atomic Data for Astrophysics VOTada VO Tools and Atomic Data for Astrophysics Giulio.

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UCL DEPT. OF SPACE & CLIMATE PHYSICS SOLAR & STELLAR PHYSICS GROUP Atomic Data for Astrophysics VOTada VO Tools and Atomic Data for Astrophysics Giulio Del Zanna TRACE image of solar coronal loops

DAMTP, Feb 2007 The VOTADA project aims at providing accurate atomic data and derived products/tools for astrophysical applications within the Astrogrid (PPARC-UK) and VO. Peter Young (RAL) Helen Mason (Univ. Cambridge) Silvia Dalla (Univ. Manchester) Kevin Benson (UCL/MSSL)

DAMTP, Feb 2007 The CHIANTI database Collaboration between UK, US and Italy –K. Dere, E. Landi, H. Mason, G. Del Zanna, M. Landini, P. Young Freely available. First release in 1996, regularly updated. Provides all atomic data necessary for modelling coronal spectra, but also used for a wide range of astrophysical objects (Chandra, XMM--Newton, FUSE, HST). Included in many other spectral codes such as: XSTAR (HEASARC/GSFC -- USA); APED/ATOMDB (CfA, Harvard- Smithsonian --USA); XSPEC (HEASARC/GSFC -- USA); ISIS (MIT -- USA); PINTofALE (CfA, Harvard-Smithsonian -- USA); Arcetri Spectral Code (Italy). Over 800 citations

DAMTP, Feb 2007 CHIANTI atomic package Data, programs, User Guides

DAMTP, Feb 2007 CHIANTI Software CHIANTI IDL software takes the atomic data and calculates line+continuum emissivities. Line emissivities are: Obtain densities, temperatures and elemental abundances from e.g. line ratios. Derive DEM curves. Create synthetic spectra to be compared to observed ones Create synthetic broad-band images Calculate instrument response functions Calculate radiative losses F(T)Ab(Fe) 0.83

DAMTP, Feb 2007

CHIANTI data files CHIANTI is distributed within Solarsoft –$SSW/packages/chianti For each ion there is a directory, e.g.,dbase/fe/fe_12 4 main files for each ion, e.g., fe_12.elvlcEnergy levels (theoretical, observed), level descriptions fe_12.wgfaRadiative decay rates, gf values, wavelengths fe_12.splupsspline fits to the Maxwellian- averaged e- collision strengths

DAMTP, Feb 2007 CHIANTI emissivities are currently calculated for equilibrium plasmas (collisional, optically-thin), but non-equilibrium, non-Maxwellian plasmas will soon be included. building a database of radiative and dielectronic recombination rates, as well as collisional and photo-ionization cross-sections

DAMTP, Feb Written CHIANTI data in a way to be imported into a MySQL database. Wavelength, A-value, gf-value configuration, nLSJ, observed, theoretical energy of upper and lower levels 1.-Use DAL Toolkit to install a SLAP server (DMMapper can translate from CHIANTI data model to Line data model) 2.-Data will appear automatically in VOSpec, once registered

DAMTP, Feb 2007 Summary

DAMTP, Feb 2007

Scattering calculations: Fe XII From Flower (1977) until Storey Del Zanna, Mason (2005), serious problems with the Fe XII spectrum were present. EUV 4 S 3/2, 2 D 3/2, 2 D 5/2, 2 P 1/2, 2 P 3/2 2 D 3/2 4 P 1/2 4 P 3/2 2 P 1/2 SO Iron Project UK Rmax network – new PPARC proposal (APAP network)

DAMTP, Feb 2007 Fe XII: electron densities now 10 times lower. Of the lowest 41 levels:  15 were not known (identified 12)  6 were incorrectly assigned  14 values revised  21/58 new transitions identified/revised (Del Zanna & Mason 2005)

DAMTP, Feb 2007 Whittoeft, Badnell,Del Zanna et al. (2006) Del Zanna (2006 ) Atomic data make a difference! Fe XII Fe XVIII Storey, Del Zanna et al. (2005) Del Zanna & Mason (2005)

DAMTP, Feb 2007 Hydrodynamic equations in 1-D Conservation of Mass Momentum Energy Radiative lossess Time-dependent ionisation Eq. state Heating rate Classical conduction

DAMTP, Feb 2007 Diagnostics of chemical abundances Widing & Feldman (1992) Del Zanna et al. (2003) Te of maximum emissivity in ionization equilibrium Actual Te Incorrect abundances (by a factor of 10) can be obtained if approximations are used. Plumes in coronal holes FIP=10 FIP=0