1. X-ray Binaries in the Era of Chandra and XMM High Resolution Spectroscopy Michael A. Nowak MIT Kavli Institute for Astrophysics and Space Research & Chandra X-ray Science Center Michael A. Nowak MIT Kavli Institute for Astrophysics and Space Research & Chandra X-ray Science Center

2. What are We Asking with Spectra? Broad Band X-ray Spectra (RXTE, Suzaku, Swift, INTEGRAL, + multi-wavelength) What are the basic components? Corona: Size, Temperature, Optical Depth? Jet: Does it contribute to the X-rays? Disk: Truncated? Measure of relativity? Surface: Differences with respect to BH? Reflection: Relative geometry of above?

3. Broad-band Spectra keV Photons sec -1 cm -2 keV -1  (Markoff, Nowak, & Wilms 2005) keV Photons sec -1 cm -2 keV -1  (Markoff, Nowak, & Wilms 2005) (Kubota et al.) Cyg X-1: Classic “Hard State”

4. Broad-band Spectra (Nowak et al., in prep.) 4U 1957+11: Classic “Soft State”

5. Broad-band Spectra (Fiocchi et al., 2007) 4U 1705-44

6. What are We Asking with Spectra? High Resolution X-ray Spectra: Chandra & XMM What are the physical properties? Velocities, Temperatures, Densities Inflows? Outflows? Rotation? Compositions? Ionization states? Separation of narrow & broad components: Relativity vs. atomic physics Complex interactions among “continuum” components

7. Outline of Talk Overview of the (Many & Complex) Components of an Accreting Binary System What physics are we studying with each? Examples of Chandra & XMM gratings studies When do we obtain high-resolution features, and when don’t we? (Actually, I don’t really know...) Where do we go from here?

8. Components of X-ray Binaries:

9. Neutron stars have surfaces! Continua: Cooling of interior (nuclear physics), contrast to BH implies existence of horizon? (See, however, Jonker et al. 2007) Hi-res spectra: Redshifted features constrain M/R (nuclear physics; Cottam et al. 2002)

10. (Cottam et al. 2002) EXO 0748-676 Neutron Star Surface: RX J0720.4- 3125 (van Kerwijk et al. 2007) RX J1308.6+2127 EXO 0748-676: Only example so far Low spin (45 Hz; Villarreal & Strohmayer 2004) Low temperature burst If the features are real: M/R consistent with “reasonable” EOS Some exotic EOS ruled out

11. Components of X-ray Binaries: Disks: No intrinsic hi-res features; more via their interaction with their environment (X-ray heating, fluorescence, boundary layers at coronal transition, etc.) Evidence of MHD turbulence driving accretion? Do they truncate? Are models and observations good enough to measure relativity (i.e., spin; Shafee et al. 2007, Davis et al. 2006, etc.)

12. Components of X-ray Binaries: Some (Many? Most?) disks are warped: Her X-1, LMC X-4, SS 433 Most mechanisms (radiative warping - Petterson 1977, Pringle 1996; winds - Schandl & Meyer 1994) rely on X-ray heating - testable by hi-res spectroscopy

13. Her X-1 Observations: (Jimenez-Garate et al. 2002) (Jimenez-Garate et al. 2005) Line velocities and widths are small (<290 km s -1 ) Viewing only the outer region of the disk G = (i+f)/r ratios imply photoionized atmospheres R = f/r ratio is very low, except for higher Z UV radiation coverts f to i, and/or Density leads to collisional depopulation High Z-species occupy much greater volume Consistent story, but not yet “testing” warp theory

14. Components of X-ray Binaries: “Hard States” likely have a corona (or equivalently, base of a jet): Geometry & structure are debated “Transition regions” have been hypothesized as possible source of line emission (Perna et al. 2000) But only applied to sources such as Sgr A* (see M81* talk by A. Young)

15. Components of X-ray Binaries: Both coronae (Magdziarz & Zdziarski 1995) and jets (Markoff & Nowak 1994) yield reflection features Chief benefit of hi-res may lie in disentangling components

16. “Ideal” Reflection: GX 301-2 (Watanabe et al. 2004)

17. Cyg X-1 (Miller et al. 2002) “Hard State” BHC Observations: GX339-4 (Miller et al. 2004) 4U 1705-44 (Di Salvo et al., 2005)

18. Low-res Data Used to Challenge Lines (Young et al. 2005) MCG-6-30-15 (Done & Gierlin´ski 2006) XTE J1650-500

19. Components of X-ray Binaries: Accretion Disk Coronae Distinct from Inner Corona/Jet Ionized Disk Atmospheres “Dipping Sources”

20. ADC Sources Show Orbital Modulation X1822-371: HETG Lightcurve (Heinz & Nowak 2001)

21. HETG Observations of X1822-371 (Cottam et al. 2001)

22. Going a Little Away from the Disk Plane: EXO 0748-676 (Garate et al. 2001) * Continuum consistent with absorbed, point source * Line emission consistent with unabsorbed, extended region, 500 km s -1 < velocity broadening < 1200 km s - 1 * Absorbers have neutral and ionized components

23. Ionized Absorption in Many “Dippers” Models to XMM (both PN and RGS data) have been successfully applied to many dipper sources X 1323-619, X 1916-053, X 1254-690, MXB 1659- 298, X 1624-490 (Boirin et al. 2004, 2005; Díaz Trigo et al. 2006) Fe XXV & Fe XXVI absorption commonly detected Chandra studies of X 1916-053 show rather narrow features (Juett et al. 2006, Iaria et al. 2006) 4U 1916-05 (Juett & Chakrabarty 2006)

24. Components of X-ray Binaries: Winds!

25. Seen in Both Neutron Stars & Black Holes P Cygni profiles in Cir X-1 with V = 200-2000 km s -1 (Brandt & Schulz 2000, Schulz & Brandt 2002) Blue shifted Fe XXVI line in GRS 1915+105 with V = 770±400 km s -1, (Lee et al. 2002) Blue-shifted absorption in GRO J1655-40, seen by both XMM (Díaz Trigo et al. 2006) and Chandra (Miller et al. 2006), with V = 300-1600 km s -1

26. Wind Examples: Cir X-1 (Schulz & Brandt 2002) GRS 1915+105 (Lee et al. 2002) GRO J1655-40 (Díaz Trigo et al. 2006)

27. Extreme Example of Absorption Lines: GRO J1655-40 (Miller et al. 2006) Disk-dominated, 4% L Edd state 90 significant absorption lines, 76 identified (32 charge states), blue shifted 300-1600 km s -1, FWHM 300 km s -1, no emission lines Modeled with a highly ionized wind at R = 400 GM/c 2 Too close to be thermal, too ionized to be line driven Hypothesized to be magnetically driven Netzer (2006) instead modeled the spectrum with R = 10 5 GM/c 2, with But not a true “fit” to the data

28. Components of X-ray Binaries: Accretion Streams & Secondary Winds

29. Winds & Flows from the Secondary Most relevant to High Mass X-ray Binaries (HMXB) Examples of both Neutron Star and Black Hole sources Vela X-1 (Schulz et al. 2002, Goldstein et al. 2004, Watanabe et al. 2006) Cyg X-3 (Paerels et al. 2000) Example of Cyg X-1 at Phase 0 (Hanke et al., in prep.)

30. Dipping in Cyg X-1 3×10 4 10 4 Rate (cps) 2 2×10 4 4×10 4 Time (sec) 4 6 (Hanke et al., in prep.)

31. Why We Need Con-X (Simulations by Manfred Hanke)

32. Components of X-ray Binaries: Not intrinsic to the X-ray Binary But important to understand to determine what is intrinsic ‘Warm Absorber’ or ‘WHIM’? * Absorption from Cold & Warm Phases of ISM (Juett et al. 2004, 2006; Yao et al. 2006, 2007; Wang et al. 2005, etc.) * Dust Scattering Halos & ‘Solid State Astrophysics’ (Predehl & Schmitt 1995, Lee & Ravel 2005, Xiang et al. 2005, Smith et al. 2006, etc.) * Absorption also depends upon direction of view -in the plane, or through the halo (see Daniel Wang’s talk)

33. Multi-phase ISM GX 339-4 (Miller et al. 2004) (Juett et al. 2004, 2006) 4U 1957+11 (Nowak et al, in prep.) There are clear cold & warm components of the ISM There are also examples of “warm absorbers” GX 339-4 Ne IX line (Miller et al. 2004) is perhaps 5% due to ISM (Juett et al. 2006) 4U 1957+11 Ne IX is consistent with ISM (halo), and agrees with Mkn 421 (Yao et al., in prep.) Why doesn’t 4U 1957+11 show intrinsic lines??? Very similar L Edd and inclination to GRO J1655-40

34. Summary X-ray binaries have many components, interacting in complex, interesting ways High resolution X-ray spectroscopy is addressing all of them Continuum spectroscopy is perhaps “ahead” in that we’ve had time for multiple observations: States, orbital phases, inclinations, etc. But that means there is lots to do with Chandra, XMM, and on into Constellation X