XMM-Newton                                Chandra      Application of X-ray Plasma      Diagnostics to Nova Winds         ...
The RS Oph system Recurrent Nova with 6 recorded outbursts since 1898
outburst                      Accreted                      material:                       H-rich!      Nuclear      burn...
outburst                             Accreted                             material:                              H-rich!  ...
Radiatively driven expansion                                          Pseudo                                          Stel...
Pseudo                                                  Stellar Nuclear                                        Atmosphere ...
Pseudo                                                 Stellar Nuclear                                       Atmosphere bu...
Pseudo                                                 StellarNuclear                                        Atmospherebur...
Constant Bolometric Luminosity phase                              Lbol=1038 erg/s          WD         WD         WDoptical...
 Novae are powered by nuclear burning The pressure is not high enough on a WD  surface to produce any elements heavier  ...
Shock with                 stellar windSSS Emissionfrom hot whitedwarf            + giant in                   Symbiotic N...
Swift observations of RS Oph   Osborne et al. (2011)  shock phase   SSS phase      nebular phase                          ...
Swift observations of RS Oph                                                  Osborne et al. (2008)  shock phase          ...
Swift spectra
grating spectra
RS Oph: 13.8 days after outburst   H-like ions                                   He-like ions                             ...
Ness & Jordan (2008) MNRAS 385, 1691
3-T APEC model reproduces              the observations==>       Assumption of collisionalequilibrium may not be too bad  ...
fG T 
N         Mg                   S                       Fe              SiO   Ne
fG T 
fG T 
FeN       Ne                       S             Mg   Si    O
0.46 x solar      solar      abundance
N high=>CNO-cycledmaterial
RS Oph secondary has   [N/Fe]=0.9:(Pavlenko et al. 2008)=> 20-40% of N fromoutburst or companion
Sample of M giants bySmith & Lambert (1985/86)     RS Oph secondary has        [N/Fe]=0.9:     (Pavlenko et al. 2008)     ...
Sample of M giants by Rich et al. (2007)Mg, Si not produced in outburst=> must come from WD or companion
SummaryThe companion in Symbiotic Novae is a  giant star that has similar abundance ano-  malies as those expected in no...
Application of X-ray plasma diagnostics to nova winds
Application of X-ray plasma diagnostics to nova winds
Application of X-ray plasma diagnostics to nova winds
Application of X-ray plasma diagnostics to nova winds
Application of X-ray plasma diagnostics to nova winds
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Application of X-ray plasma diagnostics to nova winds

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Talk presented by Jan-Uwe Ness (XMM-Newton Science Operations Centre) at the symposium "From atoms to stars: the impact of spectroscopy on astrophysics", Oxford, UK, 28-28 July 2011.

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Application of X-ray plasma diagnostics to nova winds

  1. 1. XMM-Newton Chandra Application of X-ray Plasma Diagnostics to Nova Winds Jan-Uwe Ness XMM-Newton Science Operations Centre SwiftEuropean Space Astronomy Centre (ESAC)
  2. 2. The RS Oph system Recurrent Nova with 6 recorded outbursts since 1898
  3. 3. outburst Accreted material: H-rich! Nuclear burning ignites WD
  4. 4. outburst Accreted material: H-rich! Nuclear burning ignites WD enough radiative energy is produced to drive a wind with v ≈ 1500 km s-1
  5. 5. Radiatively driven expansion Pseudo Stellar Nuclear Atmosphere burning equivalent to a stellar radiation zone 6 m WD 0 x10 k R=10 ay aft er 1 d Photospherebrightest in optical -> discovery
  6. 6. Pseudo Stellar Nuclear Atmosphere burning WD PhotosphereDensity drops, outer layers go optically thin=> Radius of Photosphere recedes to inner, hotter, layers
  7. 7. Pseudo Stellar Nuclear Atmosphere burning WD Photosphere=> fades in optical but Lbol constant => spectrum shifts to higher energies ...
  8. 8. Pseudo StellarNuclear Atmosphereburning Super-Soft-Source X-ray spectrum WD ⇒ SSS phase Photosphere.... until the peak of the spectrum reaches soft X-rays--> direct observations of nuclear burning
  9. 9. Constant Bolometric Luminosity phase Lbol=1038 erg/s WD WD WDoptical UV X-ray
  10. 10.  Novae are powered by nuclear burning The pressure is not high enough on a WD surface to produce any elements heavier than Helium The CNO cycle changes the relative abundances of C, N, and O If the nova ejecta show any other anomalies in composition, then either - WD material has been dredged up - The companion is anomalous
  11. 11. Shock with stellar windSSS Emissionfrom hot whitedwarf + giant in Symbiotic Novae + MS star in Classical Novae
  12. 12. Swift observations of RS Oph Osborne et al. (2011) shock phase SSS phase nebular phase optical
  13. 13. Swift observations of RS Oph Osborne et al. (2008) shock phase SSS phase nebular phase XMM-Newton------------ Chandra Chandra Chandra/XMM XMM-Newton Chandra
  14. 14. Swift spectra
  15. 15. grating spectra
  16. 16. RS Oph: 13.8 days after outburst H-like ions He-like ions other lines (FeXVII - FeXXV) simultaneous Chandra and XMM spectra
  17. 17. Ness & Jordan (2008) MNRAS 385, 1691
  18. 18. 3-T APEC model reproduces the observations==> Assumption of collisionalequilibrium may not be too bad proper EMD analysis
  19. 19. fG T 
  20. 20. N Mg S Fe SiO Ne
  21. 21. fG T 
  22. 22. fG T 
  23. 23. FeN Ne S Mg Si O
  24. 24. 0.46 x solar solar abundance
  25. 25. N high=>CNO-cycledmaterial
  26. 26. RS Oph secondary has [N/Fe]=0.9:(Pavlenko et al. 2008)=> 20-40% of N fromoutburst or companion
  27. 27. Sample of M giants bySmith & Lambert (1985/86) RS Oph secondary has [N/Fe]=0.9: (Pavlenko et al. 2008) => 20-40% of N from outburst or companion
  28. 28. Sample of M giants by Rich et al. (2007)Mg, Si not produced in outburst=> must come from WD or companion
  29. 29. SummaryThe companion in Symbiotic Novae is a giant star that has similar abundance ano- malies as those expected in nova ejecta The abundances for RS Oph appear more anomalous than for typical stars of the same spectral type as the companion We might be seeing WD material => too many heavy elements for SN Ia But: The companion in symbiotics is stripped off the outer layers, exposing layers with different abundances.

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