Accurate Atomic Rates for Black Hole Accretion Disks

John Raymond

Disk winds have been know in AGN for years andsuspected in Galactic Black Hole Binaries

Miller et al. 2006 Chandra HETG GRO1655-40

Chance for a Serious Model

90 Absorption lines, blueshift ~ 500 – 1000 km/s

Usual elements + P, Cl, K, Ti, Cr, Mn, Co

Fe XXIV lines up to 2s – 10p or more

Limits on emission lines (4p-3s) imply small covering fraction

Photoionization model using measured X-ray continuum

Density, r and Abundances are the unknowns

Density Measurement

Ratio of Fe XXII lines at11.92 and 11.77 gives n2/n1

Mauche et al. emission lines

Depends on A value qelectron

qproton

cascades

13.6 < Log ne < 14.1

Ionization Parameter

(O-Ne and Ca-Fe Abundances x 2)

Differs from optical

Voigt profileUnresolved doubletsInner shell Fe K

ξ ~ 104 (soft spectrum)

Limits on rColumn Density N ~ nr

Ionization parameter ξ from highest and lowest ionizationstages: Fe XXVI vs Fe XXII and Model

ξ = L/4πnr2

For known L and ξ, N drops off with r, giving upper limit,

For known L, ξ and n, r is known

Physics of WindNot Radiation-Pressure driven; measure lines and no UV

Miller et al. find r < 10 9.5 < 0.1 RIC = 10 10.7

Implies not thermally driven (Begelman, McKee, Shields), leaving magnetically driven wind

Importance of Atomic RatesHagai Netzer says r=10 10.7 = 0.1 RIC works, so thermallydriven wind is OK, but with ne only 10 13. Higher ne

requires r < 10 10.4 even for his ionization parameter.

XSTAR, CLOUDY seem to fall in between

Woods et al require 0.2 RIC and density is < 10 12

σphot(E)

f values αrec (DR rates for high ions, low T) Δn=0 cooling transitions Fe XXII fine structure transition