Accretion Phenomena in Accreting Neutron Stars From atol to Z-sources Norbert S. Schulz, L. Ji, M. Nowak Claude R. Canizares MIT Kavli Institute for Astrophysics & Space Research Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Accretion Disk Processes with Chandra HETG T. Kallman GSFC, Greenbelt MD

Atoll-, Banana- and Z-sources Schulz, Hasinger&Truemper 1989, Hasinger & van der Klis 1989 Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010

Atoll-, Banana- and Z-sources Schulz, Hasinger&Truemper 1989 Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 sub-L Eddington accretion rates super-L Eddington accretion rates Spectral States of XTE J : Link Between Z and Atoll Sources (Lin et al. 2010)

Atoll-sources with Chandra HETG Chandra Accretion Workschop— Cambridge, MA. July 13-15, S ks 1 4U ks 4 4U ks 1 4U ks 1 4U ks 1 4U ,8 ks 1 4U ,8 ks 1 4U ks 1 4U ks 1 4U ks 4 4U ks 3 4U ks 4 4U ks 3 4U ks 1 4U ks 1 4U ks 5 4U ks 1 4U ks 3 4U ks 1 EXO ks 3 GS ks 3 GR ks 11 Her X ks 10 4U ks 1 Ser X ks 1 XB ks 1 26 Atoll sources for 2.3 Msec in 69 observations M. Linares PhD Thesis 2009

Accretion of Matter in X-ray Binaries ~ log r [cm] Photo-emission and absorption line spectra for log L x > 37 [erg/s] Spectral continua Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010

Accretion Disk Morphologies Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 OpticaLthick cool reflection surface Thin & hot ionization layer Accretion disk atmosphere Accretion disk atmosphere/ Accretion Disk Corona *ADC)

Accretion Disk Atmospheres Assumptions: - energy balance between heating by incident radiation and cooling by recombining emission. - uniform static corona in thermal equi- librium. Compare: - the deduced emission measure n 2 V from the measured line luminosity L line =n 2 Va atom E line A ion with the expected one from an X-ray heated ADC d EM/d  = 2.5x10 65  -3 L 38 2 f(R,T) yellow:measured quantities blue atomic data and ADC models green: quantities to compare log L x = 38 = 37 Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010

Accretion Disk Coronae 4U (Schulz et al. 2002) Her X-1 (Ji et al. 2008) 2S (Kallman et al. 2003) Cir X-1 (Schulz et al. 2008) Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010

Atoll Sources: 4U with Einstein Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 White & Holt 1982

Atoll Sources: 4U with RXTE Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Heinz & Nowak 2001 White & Holt 1982

Atoll Sources: 4U with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Cottam et al. 2001

Atoll Sources: 4U with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Ji et al. 2010

Atoll Sources: 4U with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Heinz & Nowak 2001

Atoll Sources: 4U with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010

Atoll Sources: 4U with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010

Atoll Sources: 4U with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010

Atoll Sources: 4U with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Schulz 1999, Piraino et al. 1999, Migliari et al. 2010, Schulz et al. 2010

Atoll Sources: 4U with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Madej et al Schulz et al. 2010

Atoll Sources: 4U with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010

Banana-sources with Chandra HETG Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 GX ks 1 GX ks 1 GX ks 1 GX ks 5 GX ks 3 3 Banana sources for 85.3 ksec in 4 observations

Banana Sources: GX 13+1 with Chandra Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 GX 13+1 (4U ) is a persistently bright (F x = 9x10 -9 erg cm -2 s -1, N H = cm -2 ) LMXB with a K5 III companion at distance of 7+/-1 kpc.

Z-sources with Chandra HETG Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Cir X ks 9 Cyg X ks 5 GX ks 3 GX ks 4 GX ks 4 GX ks 5 Sco X ks 1 GX ks 4 7 Z -sources for ksec in 31 observations

7th Microquasar Workshop, Foca, Sept. 1-6, 2008 Z-source and Microquasar: Cir X-1 Possibly ultra-relativistic jet Neutron star binary Low/Intermediate mass companion Accretion disk wind of km/s Variable cool & hot absorbers Suggested soft ionized absorber (Parkingson et al. 2003) Fender et al. 2004

Z-sources with Chandra HETG Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Cyg X-2 like Z-tracks Sco X-1 like Z-tracks Church&Church 2001, 2004 Church et al. 2006, 2010 Jackson et L Extended ADC model

Interpretation of Z-tracks with ExADCs Fe XXVI Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 Church, Jackson, & Church 2009

Z-sources: Cyg X-2 Low-mass X-ray Binary: Z-source prototype Distance: 8-12 kpc Luminosity: >> erg/s Companion: A9III evolved, 0.6 M Sun Binary period: 9.84 days Compact Object: Neutron star (type I bursts) Spectral Properties (DiSalvo et al. 2002) : Column Density: 2x10 21 cm -2 Diskbb/bbody : 0.8 keV / 1.7 keV Electron Temperature: > 3 keV Comptoniztation (seed): 1-2 keV Fe-K line: 6.7 keV, 42 eV EW Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010

Extended ADCs in Z-sources: Cyg X-2 Chandra Accretion Workschop— Cambridge, MA. July 13-15, 2010 r disk = [ ] x10 10 cm n Z = < cm -3 n fexxv ~ cm -3 log  2.8 (HB) --> 3.4 (FB) L x : 0.6 L Edd --> 1.4 L Edd

Summary Chandra HETG has observed 36 LMXBs (identified Atoll, Banana, and Z-Sources) for ~ 3.2 Msec in 104 observations. The Atoll source 4U shows a thin ionization layer of ionization parameter log  < 2.6 inferring L x ~ erg/s; Highly ionized Fe XXVI emission from central corona The Atoll source 4U is likely of ultra-compact nature with an accretion disk radius of a few 10 9 cm, probable higher Ne abundance. It exhibits a highly variable and moderately relativistic O VIII line from it inner disk The Z-source Cyg X-2 exhibits broad line emission indicating the presence of an extended (r~10 10 cm) ADC. Line fluxes indicate ADC heating from HB --> NB --> FB from sub- to super Eddington luminosities,