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The HETGS view of the micro-quasar GRS 1915+105

The HETGS view of the micro-quasar GRS 1915+105. Lee et al. 2002, ApJ., 567, 1102. COLLABORATORS : C.S. Reynolds (U. Maryland) R.A Remillard (MIT) N.S. Schulz (MIT) A.C. Fabian (IoA – Cambridge) E.G. Blackman (U. Rochester). Julia Lee : Chandra symposium 2002.

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The HETGS view of the micro-quasar GRS 1915+105

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  1. The HETGS view of the micro-quasar GRS 1915+105 Lee et al. 2002, ApJ., 567, 1102 COLLABORATORS : C.S. Reynolds (U. Maryland) R.A Remillard (MIT) N.S. Schulz (MIT) A.C. Fabian (IoA – Cambridge) E.G. Blackman (U. Rochester) Julia Lee : Chandra symposium 2002

  2. The micro-quasar GRS 1915+105 • Discovery with WATCH All Sky Monitor on GRANAT (Castro-Tirado et al. 1992) • LMXB with K-M III companion (Greiner et al. 2001) • Radial velocity curves : 14 Msun; ~ 33 day period • Galactic jet source with superluminal motion in radio • vjet ~ 0.92c; incl = 70 deg.(e.g. Mirabel & Rodriquez 1999) • ballastic AND steady jets (e.g. Fender 1999, Dhawan et al. 2000) • ASCA during soft state (Kotani et al., 2000) • Ca XX, Fe (XXV, XXVI), and blends of H- and He-like Ni & Fe • Highly variable : repeated flares, then periods of quiescence • L ~ few x 1037 to few x 1039 erg s-1

  3. Chandra HETGS & RXTE PCA 2000 April 24 : Phase ~ 0.8 ASM 21-28 April : ~ 0.4 Crab (2-12 keV) Lx > 6.4 x 1038 erg/s

  4. GRS 1915 + 105 : Low Hard State Lee et al.

  5. Prominent Neutral Photoelectric K edges * * } 3 x 1022 cm-2 Lee et al.

  6. Prominent Neutral Photoelectric K edges in GRS 1915 + 105 IR show heated dust in surroundings (Mirabel et al. 1996, Marti et al. 2000) • OTHER BINARIES ? • Overabund : S, O • (companion stars) • GRO1655; V4641 Sgr • (Orosz et al. 2001, , Brown et al. 2001, • Israelian et al. 1999) • No Fe, Si overabund • SS 433(Marshall et al. 2002) • Cyg X1(Schulz et al. 2002) • X0614 + 091(Paerels et al. 2001) * * } 3 x 1022 cm-2

  7. Solid State Astrophysics ? Extract grain properties via compound’s inner structure ! Lee et al. 2002

  8. Ionizing Absorption from a Hot Disk Atmosphere (also CaXX Ly a; W > 1.2 mA, Nca > 3.6x1016 cm-2) Lee et al.

  9. The iron complexaHOTdisk atmosphere (lower limit) Lee et al.

  10. Consider this … a a a What if the ionized absorber is associated with material flowing out from the X-ray source ? (1) Assume vwind ~ 100 km s-1 (W = solid angle of outflow) (2) Efficiency h~ 0.1 & Lbol ~ Lx (lower limit on Lbol) Lee et al. 2002 • Mass flux in disk ~ mass flux in wind when W/4p ~ 1 • material in ~ material out for slow isotropic wind

  11. Ionizing flux & density changes ? (10-8 erg cm-2 s-1) If R ~ 1011 cm and vwind~ 100 km/s Dtflow = 10 ks Lee et al.

  12. LOW HARD STATE : • COLD : anomalous Fe, Si • HOT disk atm. (H, He-like Fe) • DUST : XAFS ? • VARIABILITY : flow ? COLD Clouds HOT atm / corona Lee et al. 2002

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