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The HETGS view of themicro-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
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
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
Prominent Neutral Photoelectric K edges
in GRS 1915 + 105
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)
*
*
IR show heated dust in surroundings (Mirabel et al. 1996, Marti et al. 2000)
3 x 1022 cm-2
}
Ionizing Absorption from a Hot Disk Atmosphere
(also CaXX Ly ; W > 1.2 mA, Nca > 3.6x1016 cm-2)
Lee et al.
Consider this …
What if the ionized absorber is associated with material flowing out from the X-ray source ?
(1) Assume vwind ~ 100 km s-1 ( = solid angle of outflow)
(2) Efficiency ~ 0.1 & Lbol ~ Lx (lower limit on Lbol)
Mass flux in disk ~ mass flux in wind when /4 ~ 1material in ~ material out for slow isotropic wind Le
e e
t al. 2
00
2
Ionizing flux & density changes ?
If R ~ 1011 cm and vwind~ 100 km/s tflow = 10 ks
(10-8
erg
cm
-2 s
-1)
Lee et al.