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AtomDB Workshop Harvard-Smithsonian Center for Astrophysics Cambridge, MA 9-10 August 2012

AtomDB Workshop Harvard-Smithsonian Center for Astrophysics Cambridge, MA 9-10 August 2012.

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AtomDB Workshop Harvard-Smithsonian Center for Astrophysics Cambridge, MA 9-10 August 2012

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  1. AtomDB Workshop Harvard-Smithsonian Center for Astrophysics Cambridge, MA 9-10 August 2012 Fitting X-ray Spectra with Imperfect ModelsNancy S. BrickhouseHarvard-Smithsonian Center for AstrophysicsAcknowledgments to Randall Smith and Adam Foster.This talk is based on benchmarking ATOMDB.Opinions expressed are my own.

  2. How Atomic Rate Uncertainties Affect Fits to X-ray SpectraORIf I can’t find a model that fits my data, have I discovered exotic physics?

  3. Outline • The Coronal Model: Thermal Plasma in Collisional • Ionization Equilibrium (CIE) and Beyond • Guide to Atomic Rate Uncertainties • Examples of Benchmark Studies with Capella • Young Stellar Spectra • Interpreting the Diffuse Emission in SF Regions • Lessons

  4. Thermal Plasma or Non-thermal (exotic)? Energy Distribution Functions • Plasma temperature is defined for gas in thermal equilibrium, for which the most probable velocity distribution is the Maxwellian. • Examples of non-thermal plasmas are particle beams, bumps on tails, Kappa distributions. • Particles of similar mass equilibrate with each other, so e−with e−and p with p first, and then with each other. • Te ≠ Tp

  5. CIE or Non-Equilibrium Ionization? • Ionization equilibrium occurs when collisional ionization by electron impact balances collisional and radiative recombination processes • For short times and/or at low densities the ionization state has not reached its equilibrium value and thus does not reflect Te. 1.00 Fe24+ Fe8+ Fe16+ Frac. Abund. 0.10 400 Red – New (2006) Blue – Old (1998) Iron 200 0 CIE -200 -400 105 106 107 108 Electron Temperature (K) Bryans et al. 2006

  6. Line Emission from Collisional Excitation or something else more exotic? In the “coronal” limit the electron density Ne is low enough that most of the level population is in the ground state. Flux = ∑ε (Te) EM(Te) / (4 π R2), where R is the distance, EM (Te) = ∫ Ne NH dV is the emission measure, and ε (Te) is the emissivity. It depends on a lot of atomic physics, e.g. ionization and recombination rates and collisional excitation rates Level population by other methods (recombination to an upper level, fluorescence) and metastable levels with long lifetimes give interesting diagnostics for exotic processes.

  7. Guide to Atomic Rate Uncertainties Typical Possible • Collisional excitation 20 to 30% 5 to 10% • Radiative decay 20 to 30% 5 to 10% • Collisional ionization 20% 10%? • Radiative recombination 25% ? • Dielectronic recombination 30 to 50% ? • 2-photon emission 25%? • Bremsstrahlung 2% • Wavelengths 0.05 to 2% 0.003% • Missing processes (e.g. recombination to upper levels) • Missing lines (a difficult problem to treat in a spectral fit) Talk to Connor Balance about better uncertainty estimates!

  8. EUV/X-ray Line Ratios from Chandra LETG spectrum of Capella Predicted X-ray fluxes are too low for all the X-ray lines Desai et al. 2006 Talk to Connor Balance about better uncertainty estimates!

  9. Blending of Fe XIX in the Ne IX Region: Wavelength Errors Kotochigova et al. 2010

  10. How complicated can it get? Star formation is pretty messy. • Hard X-rays: corona • Soft X-rays: • corona, jet, shock • Absorption by: ISM, • disk, accretion • stream, nebula Sample of young star spectra from the Chandra HETG

  11. Furthermore, extended emission and crowded fields cannot be observed with optimal spectral resolution. ASCA HETG • CCD vs Grating for the same star (TW Hya)

  12. And it gets worse. The diffuse nebular emission processes are not all known (e.g. photoionization from hot stars, fast wind shocks?) From Townsley et al. 2011, ApJS 194 16

  13. Special thanks to Leisa Townsley for asking. Even with several model components including complex physics, there are many residuals. Are they interesting? Many of them are near strong lines, suggesting atomic data problems. Some of the very large problems may be in the absorption models. From Townsley et al. 2011, ApJS 194 16

  14. Lessons • Thermal plasma in CIE does not provide much spectral information on heating, dynamics, feedback. • Atomic rate uncertainties > calibration and statistical errors. • Uncertainties in the charge state balance can lead to inconsistencies in global models. • Residuals near strong lines are likely related to atomic rate uncertainties. Complex absorption effects will exacerbate this. • Departures from Maxwellian and CIE will be difficult to establish at CCD resolution. • Such departures, if established through resolved line ratios with accurate atomic rate data, are critical to getting to the interesting physics.

  15. Some Words about Charge Exchange (CX) • “Highly ionized plasmas don’t wait.” (R. K. Smith) • Dominance of CX occurs w/ ionized metals, neutral hydrogen, and a rapid transition region. • However, charge neutrality in a stellar wind means that electronic recombination will occur over short distances. • CX allows only ~2 X-ray photons, whereas CE keeps going. Smith & Hughes 2010 • Both recombination processes lead • to large G-ratios and large Ly α /Ly β • Ratios. • Absence of Radiative Recombination • Continua in CX the main distinction.

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