1 / 18

T ransient NS X -ray binaries with S imbol- X

T ransient NS X -ray binaries with S imbol- X. Sergio Campana Osservatorio astronomico di Brera campana@merate.mi.astro.it. Bologna, May 2007. Outline. A brief history: what we discovered and what we know now, focusing of hard X-ray emission The future: Simbol-X.

cade
Download Presentation

T ransient NS X -ray binaries with S imbol- X

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. Transient NSX-ray binaries with Simbol-X Sergio Campana Osservatorio astronomico di Brera campana@merate.mi.astro.it Bologna, May 2007

  2. Outline • A brief history: what we discovered and what we know now, focusing of hard X-ray emission • The future: Simbol-X RXTE/ASM light curve

  3. X-ray binaries: variable

  4. State transitions: SIGMA Barret & Vedrenne 1994 Limiting luminosity for all LMXRBs (NS+BH) at 4x1036 erg/s Maccarone 2003

  5. Hard tails: INTEGRAL Paizis et al. 2006 4U 1820-30 Campana et al. 1998 Tarana et al. 2007

  6. State transitions: jets BH XRB Belloni 2007 NS XRB Homan et al. 2007

  7. Very hard tails: PDS/XTE Occasional detection of very hard tails (BMC) GX 17+2 Di Salvo et al. 2000 Farinelli et al. 2007 Campana et al. 1998

  8. From outburst to quiescence Campana et al. 1998 FAST ! e-folding time changing from ~20 d to ~1 d at transition BeppoSAX data

  9. NStransients in quiescence ExN(E) ExN(E) • Canonical spectrum: • Soft component (NS atmosphere, kT~0.1-0.3 keV; ≥50% of the flux) • Hard component (Power law, photon index ~1-2; ≤50% of the flux) Lx=1032-1033 erg/s

  10. NStransients in quiescence: variability Aql X-1 Campana et al. 2003 Rutledge et al. 2001 Campana &Stella 2004

  11. Transient X-ray pulsars SAX J1808.4-3658 mcrab Wijnands 2005 Campana et al. 2007

  12. SAX J1808.4-3658 in quiescence NS atmosphere model can account less than 10% of the total flux and it is not required by the fit Campana et al. 2002 XMM-Newton data Heinke et al. 2007

  13. Simbol-X strenghts (for XRBs) • Broad-band capabilities (0.5-80 keV) • Large effective area at low and high energies • Good timing capabilities • Focusing instrument and thus low background (e.g. wrt RXTE)

  14. Simbol-X: atoll spectrum Fx=10-9 erg/s/cm2 Lx=4x1036 erg/s @ 5 kpc 3σ Monitoring of parameters variations: study the physics 100 ks  kTC

  15. Simbol-X: very hard tails CONT: Fx=2x10-9 erg/s/cm2 TAIL: Fx=6x10-12 erg/s/cm2 Tail/Cont(0.5-20)= 0.1% kTc=5 keV 40 ks Tau=3

  16. NS transient in quiescence 100 ks Diagnostic of the power law tail and of its variability

  17. SAXJ1808.4-3658 in quiescence 100 ks XMM

  18. Summary • Simbol-X is the first observatory able to disclose the high energy part of the spectrum at very high S/N and for persistent and transient sources, making possible a thorough study of the emission mechanisms through monitoring the variability • Different mechanisms for explaining the transition to and the quiescent emission of NS XRTs approach the problem from the point of view of physics

More Related