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

GRS 1915 + 105 : Low Hard State

Lee et al.

Prominent Neutral Photoelectric K edges

**

3 x 1022 cm-2}

Lee et al.

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

}

Solid State Astrophysics ?

Extract grain propertiesvia compound’s inner structure !

Lee et al. 2002

Ionizing Absorption from a Hot Disk Atmosphere

(also CaXX Ly ; W > 1.2 mA, Nca > 3.6x1016 cm-2)

Lee et al.

The iron complexa HOT disk atmosphere

(lower limit)

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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 et

al.

2002

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.

COLD Clouds

LOW HARD STATE :

• COLD : anomalous Fe, Si

• HOT disk atm. (H, He-like Fe)

• DUST : XAFS ?

• VARIABILITY : flow ?

HOT atm / corona

Lee et al. 2002