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Novae in outbursts!

Novae in outbursts!. What are we learning from X-rays?. Marina Orio INAF-Padova And U Wisconsin. How do we learn and what do we want to learn from “supersoft” novae?. Only way to probe the WD! Need frequent monitoring but also want to “go deep” and obtain high resolution spectra.

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Novae in outbursts!

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  1. Novae in outbursts! What are we learning from X-rays? Marina Orio INAF-Padova And U Wisconsin

  2. How do we learn and what do we want to learn from “supersoft” novae? • Only way to probe the WD! • Need frequent monitoring but also want to “go deep” and obtain high resolution spectra. • Swift has been exceptionally useful extending nova coverage to many more objects for longer times (frequent snapshot observations) • Long exposures are also necessary to monitor time variability - typical of novae on time scales ranging from minute to hour- periodic and aperiodic • High resolution spectra offer unique insight into atmospheric layer close to H-burning shell.

  3. Turn-on and turn-off times Turn on: delayed by self absorption in the wind/shell, depends on the mass/chemistry of the ejecta. Generally nova is “on” when mass loss ceases. Turn off: IF the abundances are those of CNO ashes, long t(off) implies mass increase on secular time scales. Also indicates quantity of accreted mass before outburst.

  4. M31 M31 novae seem to be X-ray sources for longer. Selection effect? Probably not. MW

  5. Other M31 (temptative, partial Chandra HRC-I results)

  6. A new picture of the outburst is emerging • We are beginning to obtain statistical correlations with different physical parameters. • Nova outbursts do not seem to have a unique, continuous mass loss mechanism (not discussed in present talk) • There are 3 possibilities for the burning material composition: re-accreted, WD erosion, CNO-ashes: at least in RS Oph and V4743 Sgr we “see” old CNO ashes • Periodic variations of the SSS with the orbital/rotational period, pointing out at an important role of the magnetic field.

  7. Figure includes GQ Mus, N LMC 2005, V4743 Sgr, V5116 Sgr, V1974 Cyg, RS Oph V2491 Cyg. V723 Cas and “Catalina nova” confirm picture with lower limits (not plotted).

  8. Relationship between t(3) and T(X-ray turnoff) exists but is not perfectly linear. The nova physics is just a little too complex (dust, secondary embedded in the nebula, new episodes of mass loss?)

  9. V5116 Sgr “Stunted” flare lasting about 1000 s, with rise time ~200 s, seen once in (almost) every orbital phase => was it the same phenomenon driving the “flare” on V1494 Aql? Only lower emission measure during minimum (T, N(H) same?)

  10. Large polar cap with “spongy” atmosphere” in a polar system. “Craters” form in the atmosphere in the area where accretion stream touches/touched surface (UV emitting surface, large area subtended)

  11. Cartoon model for V5116 Sgr interpreted as a polar.

  12. Orbital modulations P ~1.8 days

  13. We need IXO to resolve grating spectra over the orbital phase for a significant number of novae, and to probe abundances, temperature and effective gravity of almost any nova in the Galaxy and in the MC. CSS 081007: spectrum obtained only at maximum right after the peak. T~720,000 K, some emission lines on WD continuum

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