1 / 17

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

tait
Download Presentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related