CHIANTI An atomic database for X-ray spectroscopy Enrico Landi Naval Research Laboratory Overview 1.Introduction why a database? 2.What is CHIANTI 3.CHIANTI DEMO of CHIANTI Software And, IF there is time.. 1.Comparison with X-ray observations 2.Some CHIANTI applications 1 - Introduction X-ray spectra are of primary importance for quantitative studies of the physics of many astrophysical objects Emission and absorption of line and continuum radiation in the X- rays offer a wide variety of diagnostic tools to determine the physical properties of emitting sources For this reason, in the recent past, several instruments have been flown to observe astrophysical sources in the X-ray range: ChandraROSAT XMMYohkoh RHESSISMM RESIKand many others Why a database? X-ray spectra are composed by line and continuum radiation, emitted by highly charged ions. Observed X-ray spectral lines come from H-,He-like ions High-energy configurations (n>2) in highly charged Fe and Ni ions Innershell transitions Dielectronic satellite lines Continuum radiation comes from Free-free radiation Free-bound radiation In order to study this radiation and use it for plasma diagnostic purposes, a large amount of atomic data are needed for both line and continuum radiation To address this need, several databases have been created in the past: CHIANTI MEKAL APEC/APED ADAS Arcetri Spectral Code XSTAR With the only exception of MEKAL, all these databases include CHIANTI data Requirements for a database In order to be suitable for the analysis of modern high-resolution spectra, atomic databases need to - be completeno lines left behind - be accurateplasma diagnostics must not be hindered by atomic physics uncertainties - be easy-to-use - be transparent- the user can independently check the original data and their accuracy - no black box - all data independently refereed in peer reviewed literature Also, atomic data and predicted emissivities from databases need to be benchmarked against observations 2 - The CHIANTI database CHIANTI consists of A database of atomic data and transition rates A suite of IDL programs for plasma diagnostics CHIANTI is able to calculate Line emissivities for - more than 220 ions - innershell transitions - dielectronic satellite lines Continuum emissivities for - free-free radiation - free-bound radiation - two-photon continuum The CHIANTI database can be used at any wavelength range, but it is optimized for the Angstrom range. CHIANTI data are: In ASCII format Selected from the refereed literature (no unpublished data) Critically assessed and evaluated With references to original literature CHIANTI is completely transparent to the end user FREELY available on the web at(and 5 other sites) Fully documented through user guides CHIANTI also provides:a mailing list(I maintain it myself)assistance to users at: Line intensity calculation The intensity of an optically thin line is given by Where (T) is the Differential Emission Measure and G(T,) is the Contribution Function, given by a b c d e Where: -a: relative level populationcalculated by CHIANTI as f(T, N e ) -b: ion fractionprovided by CHIANTI from literature as f(T) -c: element abundanceprovided by CHIANTI for sample plasmas -d: electron/hydrogen ratiocalculated by CHIANTI as f(T) -e: Einstein coefficientprovided by CHIANTI Level population calculation Level populations are calculated by solving statistical balance equations. The excitation processes included are: Electron-ion collisional excitation Proton-ion collisional excitation Photoexcitation by any ambient radiation Radiative cascades Ionization and recombination into excited levels Dielectronic recombination (for satellite lines) The de-excitation processes included are: Spontaneous radiative decay Electron-ion collisional de-excitation Autoionization (for satellite lines) CHIANTI also allows the use of non-Maxwellian distribution of electron velocities Basic assumptions in CHIANTI The plasma is optically thin no radiative transfer The plasma is in ionization equilibrium ionization and recombination rates will be part of Version 6 The plasma density is lower than cm -3 rise of metastable levels for which there are no collisional rates Stimulated emission is neglected CHIANTI diffusion CHIANTI has enjoyed great success in the astrophysical community. CHIANTI data have been Included in the software of several satellite borne missions SOHO/CDS(EUV) SOHO/EIT(EUV) TRACE(UV) RHESSI(X-rays) Solar-B(EUV,X-rays) STEREO(EUV) Included in other spectral codes APEC/APED PintOfAle Arcetri Spectral Code ADAS XSTAR Included in theoretical models (i.e. loop models, irradiance models etc) Referenced in more than 400 papers Benchmarks of CHIANTI data CHIANTI predictions have been compared to several observed spectra to determine its completeness and accuracy: SERTS A(Young etal 1998) SOHO - CDS/NIS A(Landi et al. 2002a) SOHO -SUMER A(Landi et al. 2002b) SMM - FCS7-18 A(Landi & Phillips 2006) These comparisons have: Shown overall excellent agreement Shown areas where improvement was needed led to new CHIANTI versions Showed where new calculations were needed triggered new atomic physics calculations CHIANTI applications Plasma diagnostics Plasma physical parameters Synthetic spectra calculation Line identifications Identification of new diagnostic tools Radiative losses calculation Energy equation in models Plasma response function of imagers Diagnostic use of imagers Optimization of optical design of new instrumentation Calculations of count rates Wavelength range/filter wavelength selection Atomic Physics Check the quality of existing data Promotes calculations of new data Test different atomic physics approximations 3 - CHIANTI 5.1 The CHIANTI database has been recently greatly expanded. The main features of the current version (Version 5.1) are: Physical processes Ionization and recombination effects in level populations Non-Maxwellian distributions of electron velocity Photoexcitation from any user-defined ambient radiation field New data New data for high-energy configurations in Fe XVII-XXIII n=3,4,5,6,7Fe XVII n=3,4,5Fe XVIII-XXIII New data for satellite lines New data for K-alpha emission Complete re-assessment of energy levels and line identifications New data for Fe IX, Fe XII, Fe XV (crucial for narrow-band EUV imagers) Other data and new ions for EUV and UV lines Softwar e More efficient software New data for high-energy configurations in Fe XVII-XXIII We have made use of the Flexible Atomic Code, by Dr. M.F. Gu, to calculate Energy levels Radiative transition rates Electron-ion collisional transition rates (including resonances) for all configurations with n=3,4,5,6,7Fe XVII n=3,4,5Fe XVIII-XXIII These data allow to predict lines in the 7-12 Angstrom range Few, if any data were available in the literature for most of these configurations New data for satellite lines New data have been added to CHIANTI 5.0 for dielectronic satellite lines and innershell transitions, to match observations Fe XVIII to XXIVinnershell transitions Fe II to Fe XXIVdielectronic satellite lines Si XII, S XVI, Ca XVIIIdielectronic satellite lines These new lines also provide diagnostic tools for measuring the plasma electron temperature These lines allow to study RHESSI spectra in the 6-9 keV energy range Fe XXV Fe XXIV satellites Fe XXIV satellites Fe XXIV satellites RHESSI 6.7 keV/8 keV ratio Phillips (2004) Their ratio is temperature sensitive Inclusion of satellites is key to a correct plasma temperature measurement RHESSI is able to resolve the Fe complex at 1.85 A (6.7 keV) and the Ni/Fe complex at A (8 keV). Satellite lines are of crucial importance for X-ray spectroscopy: They allow accurate temperature diagnostics They blend with He-like triplets and alter their line ratios, thus affecting Temperature diagnostics Density diagnostics CHIANTI allows to take explicitly into account such satellites into line ratios, by including levels above the ionization threshold into the level population calculation. Excitation processes are: Dielectronic capture of a free electron Collisional excitation from levels below the ionization threshold Example: the (x+y)/z ratio in Si XIII Both lines are blended with satellite lines: z:1s 2 1 S 0 1s2s 3 S 1 x+y: 1s 2 1 S 0 1s2p 3 P 1,2 The (x+y)/z ratio is strongly density dependent little temperature dependent constant at low density 1s2p 1 P 1 1s2p 3 P 1s2s 3 S wxy z If satellite lines are taken into account, the low-density limit of the (x+y)/z ratio can change by a factor around 4 at low T, and becomes strongly temperature dependent. Ness, Landi & Jordan (2006) Example: the (x+y+z)/w ratio in Si XIII All lines are blended with satellite lines: z:1s 2 1 S 0 1s2s 3 S 1 x+y: 1s 2 1 S 0 1s2p 3 P 1,2 w:1s 2 1 S 0 1s2p 1 P 1 The (x+y+z)/w ratio is strongly temperature dependent little density dependent 1s2p 1 P 1 1s2p 3 P 1s2s 3 S wxy z If satellite lines are taken into account, the temperature dependence of the (x+y+z)/w ratio can change dramatically at low temperatures, where satellite lines dominate. Ness, Landi & Jordan (2006) Effects of Ionization and Recombination on level populations Recently, Behar & Doron (2002) and Gu (2003) demonstrated that ionization and recombination are important contributors to steady-state level population in highly ionized Fe ions CHIANTI 5.0 incorporates data and software to take these two processes into account for Fe XVII to Fe XXIV He-like ions H-like ions Most recombination and ionization data have been taken from the Flexible Atomic Code calculations by Gu (2003). We make use of the Coronal Model Approximation: Without Ionization/Recombination: With Ionization/Recombination: Where:n q-1, n q, n q+1 ion fractions CI, REC total ion. and rec. rates E gi total excitation rate level i D ig total de-excitation rate level i The Coronal Model Approximation is not valid if metastable levels have non-negligible population As the electron density increases, the population of metastable levels also increases The maximum density at which metastable level populations are negligible changes from ion to ion: Ion Log Ne(max) Fe XVII any Fe XVIII > 13 Fe XIX 12 Fe XX 12 Fe XXI 12 Fe XXII 13 Fe XXIII > 13 Fe XXIV any He-like ions From >10 to > 15 H-like ions > 13 Fe XXIFe XXII Fe XXIVFe XXIII Example: the (x+y)/z ratio in Si XIII Recombination is more efficient in populating the 1s2p 3 P 1,2 levels (x and y lines) and therefore it alters the (x+y)/z ratio: Recombination is more efficient at high temperature Different datasets have different effects on the ratio. We used two different datasets: Mewe et al (1985) Porquet & Dubau (2000) We need more calculations Ness, Landi & Jordan (2006) Future CHIANTI features We are working on the next version of CHIANTI (Version 6), which will include: Ionization and recombination rates (both total and level-resolved) to allow studies of transient ionization; New data for high-energy configurations in all isoelectronic sequences to predict lines in X-ray and UV spectra; New data for Fe ions from the Iron Project to predict lines in the X-ray and EUV range; New data for satellite lines to account for all contributions; More data for proton excitation rates 4 - DEMO of CHIANTI software 1.Quick introduction to CHIANTI web sites 1.Download 2.Direct access 3.User guides Synthetic spectra calculation General routine: CH_SS Spectral lines routines: CH_SYNTHETIC, MAKE_CHIANTI_SPEC Continuum routinesFREEFREE, FREEBOUND, TWO_PHOTON Radiative losses: RAD_LOSS Contribution function and emissivity calculation Contribution functions:GOFNT Emissivity:EMISS_CALC Non Maxwellian distributions Only for emissivities:EMISS_CALC Plasma diagnostics Density diagnostics:DENS_PLOTTER Temperature diagnostics:TEMP_PLOTTER DEMCHIANTI_DEM (wont demonstrate it) 2 Synthetic spectra calculation The interactive routine: CH_SS 1 st step: line intensity calculation 2 nd step:Calculate spectrum (plus abundance selection) 3 rd step:Visualize and save results From the IDL prompt, and in users own software Spectral lines: CH_SYNTHETIC Input calculation parameters from keywords No continuum calculation Provides line intensities (no abundances) MAKE_CHIANTI_SPEC Calculates spectrum from line intensities in the output of CH_SYNTHETIC Includes abundances Continuum spectrum: FREEFREE FREEBOUND TWO_PHOTON RAD_LOSS Radiative losses as a function of temperature 3 Contribution functions and emissivities Contribution functions: GOFNT Calculates G(T,Ne) as a function of temperature for fixed densities Several interactive requests Outputs only few selected transitions Contribution functions: CH_SYNTHETIC The /goft keyword gives in the output the contribution functions of all the lines in the selected wavelength range Emissivities: EMISS_CALC Calculates h N j A ji for user selected arrays of T and N e (N j = relative level population) No interactive requests The user needs to multiply results by ion fractions, abundances etc to get Contribution Functions 4 Non-Maxwellian distributions This is a new feature in CHIANTI, so far it has been implemented in the EMISS_CALC program only. This is achieved by approximating the velocity distribution f(v) as a linear combinations of individual Maxwellian distributions: f(E,a i ) = i a i f M (E,T i ) f M (E,T i ) Maxwellian distribution with T i C ij tot = i a i C ij (T i ) C ij (T i ) Maxwellian collision rate coeff. The rate coefficients C ij tot are then used in the level population calculation. The distribution can be input in the program by specifying the coefficients of the linear combination of individual Maxwellians to EMISS_CALC: IDL> data=emiss_calc(8,6,dens=[10],temp=[5.5,6.0],sum_mwl_coeffs=[0.75,0.25]) Example: O VI 173/1031 ratio, Log T=[5.5,6.0] CoefficientsRatio 1.0, , 5 Plasma diagnostics Temperature diagnostics: TEMP_PLOTTER Interactive routine Provides ratios within lines of the same ion Allows blending with lines of the same ion Density diagnostics: DENS_PLOTTER Interactive routine Provides ratios within lines of the same ion Allows blending with lines of the same ion DEM diagnostics: CHIANTI_DEM Additional topics Since it seems there is time.. Comparison with X-ray observations Some CHIANTI applications 1 - Comparison with X-ray observations We have compared the new CHIANTI 5.0 with observations of a moderate solar flare InstrumentSMM/FCS (Bragg crystal spectrometer) Date of observationAugust 25, 1980 Wavelength ranges A (channel 1) A (channel 2) A (channel 3) Spectral resolution1-20 mA (depending on the channel) SourceM 1.5 flare Spectral scan Duration17.5 minutes Ions observedH-likeO,Ne,Mg He-likeO,Ne,Na,Mg,Al Fe ionsFe XVII to Fe XXIII Ni ionsNi XIX, Ni XX Comparison method FCS spectra were not observed simultaneously, so the flare plasma was analyzed as a function of time The Emission Measure analysis showed that The flare plasma was isothermal The temperature was decreasing slowly The emission measure decreased by a factor 6 during the observation This allowed us to use the Emission Measure as a tool to compare CHIANTI 5 emissivities and observed fluxes for each ion, to: Assess the quality of CHIANTI 5 data Identify blends from other ions and evaluate their contribution to the total intensity (additional check on atomic physics) Identify areas where improvements are still needed In case of isothermal plasma We can define, for all the lines of the same ion, the ratio If there are no blends and no atomic physics problems, all the ratios must be the same at all temperatures, within the uncertainties. Example: Fe XIX CHIANTI 4.2 CHIANTI 5 Time bin 1 Time bin 2 Example: Fe XVII Long standing problems: Strong A line lower than predicted Resonant scattering? Satellites in 15.01/15.26 intensity ratios? Disagreement in 2p-3s/2p-3d ratios Innershell ionization to 3s? Satellite contributions to line ratios? Existing atomic data DW collision rates from many authors R-Matrix rates including resonances for some of the lowest levels Doron & Behar (2002) showed that recombination into excited levels is important for Fe XVII We used CHIANTI 5.0 to check the importance of many additional processes in Fe XVII level population: ProcessImportance CascadesModerate Collisional ionizationModerate RecombinationCrucial ResonancesCrucial We have compared the FCS spectrum with predictions obtained with (CHIANTI 5) and without (CHIANTI 4.2) those processes CHIANTI 4.2 CHIANTI A Results and Conclusions CHIANTI 5.0 reproduces observed high- and low- resolution X- ray spectra with great accuracy All relevant configurations in Fe ions are now included Blending from ions of different species is accounted for Most lines are reproduced within 30% CHIANTI 5.0 represents a major advance over previous versions and other databases New diagnostic tools are now available to measure the physical properties of the emitting plasmas 2 - CHIANTI applications Plasma diagnostics Plasma physical parameters Synthetic spectra calculation Line identifications Identification of new diagnostic tools Radiative losses calculation Energy equation in models Plasma response function of imagers Diagnostic use of imagers Optimization of optical design of new instrumentation Calculations of count rates Wavelength range/filter wavelength selection Atomic Physics Check the quality of existing data Promotes calculations of new data Test different atomic physics approximations Applications - Plasma diagnostics in the X-rays X-ray lines are excellent tools for plasma diagnostics in solar active regions and flares. From X-ray lines and CHIANTI data it is possible to measure Electron density Electron temperature Emission measure or Differential Emission Measure Abundances Mass motions Diagnostics - Electron density 1 - He-like systems Ratios between the w, (x+y) and z lines are strongly density and temperature sensitive The ratio (x+y)/z is moderately sensitive to temperature and strongly dependent on density C V, N VI, O VIIactive regions Ne IX, Na X, Mg XIflares Heavier ionsVery high N e Satellite lines need to be taken into account 1s2p 1 P 1 1s2p 3 P 1s2s 3 S wxy z 2 - Fe ions Some n=3 lines from Fe XVII-XXIII are density sensitive relative to other lines of the same or other configurations. Their sensitivity is however limited in the ranges Log Ne < 9 Log Ne > 12 Some lines are weak and can only provide upper/lower limits 1 - He-like systems Ratios involving the w line are strongly temperature sensitive The (x+y+z)/w ratio is very weakly density sensitive Also the w n /y n ratios can be used to measure the electron temperature Diagnostics - Electron temperature 1s2p 1 P 1 1s2p 3 P 1s2s 3 S wxy z 1snp 3 P snp 1 P 1 wnwn ynyn Ratios involving different members of the Lyman series are temperature sensitive Example: O VIII Sensitivity at low temperature Need of having large n Problems of non-simultaneity of observations 2 - H-like systems 2p 2 P 4p 2 P 3p 2 P 6p 2 P 5p 2 P Ly Ly Ly Ly Ly Ratios involving a collisionally excited line from ion X +m and a dielectronic satellite line from the ion X +m+1 are excellent for temperature diagnostics Strong T sensitivity Close in wavelength No ion fractions 3 - Dielectronic satellite lines Ratios between lines of the same Fe ions belong to two classes: Configurations with same n Configurations with different n 1. Moderate T sensitivity1. Excellent T sensitivity 2. Close in wavelength2. Far away in the spectrum 3. No calibration issue3. Possible calibration issues 4 - Lines from the same Fe ion If the plasma is isothermal, the EM can be measured either from spectral lines of from the continuum Fobs = const G(T) EMEM=Fobs/(const G(T)) Both line and continuum measurements depend on the temperature Line-based measurements also depend on element abundance Continuum-based measurements are less dependent on element abundances Comparison between results from the two methods allows a check of the plasma chemical composition Diagnostics - Emission Measure There are two main methods to measure element abundances from X-rays Line to line ratios Line to continuum ratios Gives only relative abundancesMight provide absolute abundancesDepend on temperatureDepend on ion fractions Diagnostics - Element abundances Applications - Plasma response functions The count rate from an imager is given by The function H(T) represents the response of the imager to the temperature of the plasma Knowledge of the function H(T) is necessary in order to Calculate the temperature response of each filter in the imager Calculate predicted filter ratios as a function of temperature, for plasma diagnostic purposes Predicted spectra are also essential to predict count rates in high- resolution spectrometers CR =H(T) (T) dT H(T) = constAeff f -2 -1 G(Ne,T,) dT d STEREO/EUVISolar-B/EIS Effective area Filtered spectrum Response Function Applications - Atomic physics calculations As part of the CHIANTI project, we have interacted with the atomic physics community prompting the production of new or more accurate data to fill gaps or improve the existing dataset: R-Matrix suite of codes: New data for Fe ions, from the Iron Project New data for a few more ions (I.e. Ca VIII ) Flexible Atomic Code (DW code): New data for high-energy configurations in Fe XVII-XXIII Recombination and ionization rates for level populations UCL Suite of Codes (DW code): New data for high-energy configurations in the Be-like, C-like, N-like, O-like sequences