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The complex and variable X-ray spectra of the super-soft source RXJ0513.9-6951

The complex and variable X-ray spectra of the super-soft source RXJ0513.9-6951. Vadim Burwitz (MPE) X-ray Grating Spectroscopy Workshop Cambridge MA, July 12, 2007. S uper S oft X -Ray B inaries (SSXBs) RXJ0513.9-6951 Observations of RXJ0513.9-6951 LETGS observations

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The complex and variable X-ray spectra of the super-soft source RXJ0513.9-6951

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  1. The complex and variable X-ray spectra of the super-soft source RXJ0513.9-6951 Vadim Burwitz (MPE) X-ray Grating Spectroscopy Workshop Cambridge MA, July 12, 2007

  2. Super Soft X-Ray Binaries (SSXBs) RXJ0513.9-6951 Observations of RXJ0513.9-6951 LETGS observations XMM RGS / EPIC Comparison with other SSXBs Talk Overview

  3. White dwarfs at high accretion rates  Eddington rate Red Giant configuration Steady H-burn. non-mass ejecting outbursts (recurrent sources)  Novae Cassisi et al. 1998 SSXBs

  4. Discovery of SSXBs in LMC • X-ray survey of LMC by Einstein •  Cal 83 & Cal 87 discovered 1st SSXBs • Long, Helfand Grabelsky 1981, Columbia Astrophysics Laboratory • ROSAT  RX J0513.9-6951 among a total 12 sources • XMM-Newton  Four new super-soft X-ray sources Kahabka, Haberl et al. 2006, 2007

  5. SSXBs as accreting binaries mB = 16.2 mag Porb=0.76 days I ~ edge on mB = 16.2-16.9mag Porb= 1.04 days i = 25deg RX J0513-69 CAL 83 mB = 19 mag Porb=10.6 hours I ~ edge on CAL 87 Our Sun for comparison van Teeseling, Kube

  6. RXJ0513-69: long term optical lightcurve Southwell et al. 1996

  7. RXJ0513-69: X-ray and optical variability Reinsch et al. 2000

  8. RX J0513-69: long-term variation model Hachiso & Kato 2003

  9. RX J0513-69: SMARTS monitoring 2005

  10. Blackbody model (30-40 eV, L~1038 erg/s) RX J0513-69: fits to LETGS data Planckian model + 4 and more Gaussians ... Single LTE WD model Two LTE WD models Burwitz et al. 2007

  11. RX J0513-69 LETGS spectra Burwitz et al. in prep.

  12. RGS-Spectra of RXJ0513.9-6951 McGowan et al. 2005

  13. Comparison with the Hachisu and Kato Models

  14. RX J0513-69 vs. other Super-soft sources Fλ (erg / cm2 / s / Å) λ (Å)

  15. O VII Resonance line O VIII Ly a red shifted & double peaked  Wind outflow 2200 km/s Fe XVII  recombination emm. LETGS eclipse spectrum of Cal 87 Greiner et al. 2004 • resonant scattering • recombination • recombination continua

  16. Paerels et al. 2001 XMM-Newton and Chandra observations of Cal 83 Lanz et al. 2005 - RGS - LETGS

  17. Optical Monitoring (SMARTS) For triggering TOOs (Chandra/XMM) To study the long-term behavior of these objects X-ray observations of SSXBs Needed to study the nature of the outbursts RXJ0513.9-6951 evolution during X-ray bright state WD Atmosphere modeling Possibly more atomic transitions need to be included NLTE vs. LTE Comparison with theoretical Models Summary

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