Slide2:
Miller et al. 2006 Chandra HETG GRO1655-40
Chance for a Serious Model:
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:
Density Measurement Ratio of Fe XXII lines at
11.92 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:
Ionization Parameter (O-Ne and Ca-Fe
Abundances x 2)
Differs from optical
Voigt profile
Unresolved doublets
Inner shell Fe K
ξ ~ 104 (soft spectrum)
Limits on r:
Limits on r Column Density N ~ nr
Ionization parameter ξ from highest and lowest ionization
stages: 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 Wind:
Physics of Wind Not 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 Rates:
Importance of Atomic Rates Hagai Netzer says r=10 10.7 = 0.1 RIC works, so thermally
driven 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