Synthetic Spectra for SuperSoft Sources Thomas Rauch Institute

Synthetic Spectra for Super-Soft Sources Thomas Rauch Institute for Astronomy and Astrophysics Kepler Center for Astro and Particle Physics Eberhard Karls Universe Tübingen Germany Background image: Artist’s View of the RS Oph System at the Onset of the Outburst (Illustration Credit & Copyright: David A. Hardy & PPARC; Astronomy Picture of the Day 2006, July 26

Interior of AGB Stars www. g-vo. org The X-ray Universe 2011

Post-AGB Star Spectra www. g-vo. org The X-ray Universe 2011

Fluorine • First discovery of fluorine in hot post-AGB stars: – F VI 1139. 50 Å • 14 N(α, )18 F(β+)18 O(p, α)15 N(α, )19 F • Werner, Rauch & Kruk 2005 www. g-vo. org

FUSE: Ne VII 973. 3Å, one of strongest lines in FUSE spectra first identified 2004 (Werner et al. ) Herald, Bianchi, & Hillier, 2005 Ne VII 973Å – the assumed C III 977Å P Cygni feature www. g-vo. org The X-ray Universe 2011

Overview • Tübingen Model-Atmosphere Package • Applications of TMAP SEDs www. g-vo. org The X-ray Universe 2011

Model Atmospheres • LTE (Local Thermodynamical Equilibrium) – dimension of region in LTE > mean free path of photons – occupation numbers from Boltzmann distribution + Saha equation – S B • NLTE – occupation numbers ni in stationary equilibrium www. g-vo. org The X-ray Universe 2011

Equation System mean intensity 0 equations + frequency points NF equations = NF = NL statistical equations NLTE levels (NL levels) hydrostatic equilibrium particle conservation radiative equilibrium www. g-vo. org 1 1 1 NF + NL + 3 equations The X-ray Universe 2011

Classical Models • before 1986! levels ion HI H II He III NLTE 5 5 6 1 18 LTE 11 16 48 line transitions RBB 6 0 0 6 NF = 65 NL = 18 86 equations numerical accuracy! (32 bit computers …) www. g-vo. org The X-ray Universe 2011

Iteration good for www. g-vo. org The X-ray Universe 2011

Approximate * Operator iteration step i: convergence: advantage: local operator! reduction of equation system! - transfer equations - rate equations www. g-vo. org The X-ray Universe 2011

Accelerated Lambda Iteration • “Classical” models – 1969 H models, complete linearization (CL) • Auer & Mihalas 1969, Ap. J, 156, 157 • “State-of-the-art” models – 2003 H – Ni models, ALI • Rauch 2003, A&A, 403, 709 www. g-vo. org The X-ray Universe 2011

Model Atoms – levels treated in NLTE energies ? – levels treated in LTE energies ? – radiative + collisional transistions • RBB/CBB • RBF/CBF • RFF oscillator strengths ? ionization cross sections ? – line broadening ? www. g-vo. org The X-ray Universe 2011

NLTE Model Atmospheres • • all stars with spectral type B or earlier regarded as a domain of specialists high computational times atomic data C IV doublet “optical” RBB 5 6, 6 8 C III singlet + triplet www. g-vo. org

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Fe X. . . www. g-vo. org The X-ray Universe 2011

TMAP • Tübingen Model-Atmosphere Package – http: //astro. uni-tuebingen. de/~TMAP/TMAP. html • Werner et al. • Rauch & Deetjen, – – – 2003, ASPC, 288, 31 2003, ASPC, 288, 103 NLTE plane-parallel or spherical geometry chemically homogeneous hydrostatic equilibrium radiative equilibrium www. g-vo. org The X-ray Universe 2011

Neon • 14 N(α, n)18 F(e +, )18 O(α, )22 Ne – intershell abundance of 2% by mass (11 solar) expected Ne VII 3644Å first identified 1994 (Werner & Rauch) Iben & Tutukov 1985, Ap. JS, 58, 661 www. g-vo. org The X-ray Universe 2011

VLT: Ne VII Newly discovered Ne VII multiplet in VLT spectra (Werner et al. 2004) Improvement of atomic data of highly excited Ne VII lines NIST (Kramida et al. 2006) www. g-vo. org The X-ray Universe 2011

Ne VIII precise determination of Teff in hottest stars, here DO KPD 0005+5106 before: Teff = 120 000 K now: Teff = 200 000 K www. g-vo. org The X-ray Universe 2011

Iron in PG 1159 Stars • Werner, Rauch, & Kruk 2010, Ap. JL 719, 32 www. g-vo. org The X-ray Universe 2011

www. g-vo. org The X-ray Universe 2011

• FUSE: Ne VII λ 973. 3Å, 2% by mass – Werner, Rauch, …, & Kruk 2004 • FUSE: F VI λ 1139. 5Å, 200 times solar – Werner, Rauch & Kruk 2005 • FUSE: Ar VII λ 1063. 55Å, solar – Werner, Rauch & Kruk 2007 • FUSE: Ne VIII lines, 2% by mass – Werner, Rauch & Kruk 2007 • HST/STIS: Ca X λλ 1462, 1504Å, solar – Werner, Rauch & Kruk 2008 • FUSE: Fe X λλ 979. 3, 1022. 9Å, solar – Werner, Rauch & Kruk 2010 www. g-vo. org The X-ray Universe 2011

VO Service Theo. SSA • based on the Tübingen NLTE Model Atmosphere Package TMAP, the GAVO Service Theo. SSA provides – Spectral Energy Distributions (SEDs) • Theo. SSA (http: //dc. g-vo. de/theossa) – Simulation Software • TMAW (http: //astro. uni-tuebingen. de/~TMAW/TMAW. shtml) – Atomic Data • TMAD (http: //astro. uni-tuebingen. de/~TMAD/TMAD. html) www. g-vo. org The X-ray Universe 2011

Spectroscopy of LS V +46° 21 • exciting star of Sh 2 -216 – closest PN known, d = 130 pc – apparent diameter 1. 6° – LS V +46° 21 about 0. 2 radii off centre Hα + [O III] Dean Salman www. deansalman. com • mild interaction with ISM • thin disk orbit of low inclination and eccentricity – Kerber et al. 2004 • FUSE: 67. 6 ksec in 2003/2004, R 0. 05 Å • STIS: 5. 5 ksec in 2000, R 0. 06 Å www. g-vo. org The X-ray Universe 2011

Spectroscopy of LS V +46° 21 • HHe. CNOFMg. Si. PSAr + Ca. Sc. Ti. VCr. Mn. Fe. Co. Ni – Ir. On. Ic • Rauch & Deetjen 2003 – 686 NLTE levels – 2417 individual lines – 9 million iron-group lines • Kurucz 1996 • Teff = 95 000 K log g = 6. 9 (200 million) (2009, …) Rauch et al. 2007, A&A, 470, 317 www. g-vo. org The X-ray Universe 2011

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H 1504+65: CHANDRA Spectrum Werner et al. 2004 www. g-vo. org The X-ray Universe 2011

H 1504+65: Iron group www. g-vo. org The X-ray Universe 2011

KPD 0005+5106 Teff = 200 000 K instead of Teff = 120 000 K www. g-vo. org The X-ray Universe 2011

SSS Spectra: Teff = 0. 7 MK www. g-vo. org The X-ray Universe 2011

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SEDs for Extremely Hot Stars www. g-vo. org The X-ray Universe 2011

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Teff = 0. 7 MK www. g-vo. org The X-ray Universe 2011

Nova V 4743 Sgr • outburst Sep 20, 2002, m. V = 5 • Mar 2003: brightest super-soft source in the sky • CHANDRA spectrum – C V, C VI, N VII, O VII absorptions – Teff 1 – 2 MK (Ness et al. 2003) • XMM-RGS spectrum (Apr 4, 2003) – Teff 610 k. K (Rauch, Werner & Orio 2005) www. g-vo. org The X-ray Universe 2011

V 4743 Sgr www. g-vo. org The X-ray Universe 2011

Teff Determination: N VI / N VII Ionization Equilibrium www. g-vo. org

Effective Temperature of Nova V 4743 Sgr after Burst www. g-vo. org

[X] = log ( abundance / solar abundance) of species X www. g-vo. org

SSS SEDs • Teff = 550 – 1050 k. K • log g = 9 • “V 4743 Sgr” abundance pattern – C/N abundance ratio from [C] = -1. 5, [N] = 1. 8 to [C] = -0. 4, [N] = 0. 2 • http: //astro. uni-tuebingen. de/~rauch/ – atables (in FITS format) for XSPEC www. g-vo. org The X-ray Universe 2011

www. g-vo. org The X-ray Universe 2011

VO Service Theo. SSA • based on the Tübingen NLTE Model Atmosphere Package TMAP, the GAVO Service Theo. SSA provides – Spectral Energy Distributions (SEDs) • Theo. SSA (http: //dc. g-vo. de/theossa) – Simulation Software • TMAW (http: //astro. uni-tuebingen. de/~TMAW/TMAW. shtml) – Atomic Data • TMAD (http: //astro. uni-tuebingen. de/~TMAD/TMAD. html) www. g-vo. org The X-ray Universe 2011

www. g-vo. org The X-ray Universe 2011