Two-component temperature analysis of OSO-5 X-ray flare data

Solar Physics ◽  
1973 ◽  
Vol 28 (1) ◽  
pp. 169-174 ◽  
Author(s):  
J. R. H. Herring ◽  
I. J. D. Craig
Keyword(s):  
Temperature Analysis ◽  
X Ray ◽  
Two Component ◽  
Component Temperature

Dimensions de micelles mixtes de p-alkylbenzènesulfonates par diffusion central des rayons X

1977 ◽  
Vol 10 (1) ◽  
pp. 37-44 ◽  
Author(s):  
C. Cabos ◽  
P. Delord ◽  
J. Rouviere
Keyword(s):  
Small Angle ◽  
Small Angle Scattering ◽  
Micellar Solutions ◽  
Probable Structure ◽  
X Ray ◽  
Absolute Scale ◽  
Angle Scattering ◽  
Scattering Measurements ◽  
Two Component ◽  
Most Probable Structure

The structure of micellar solutions is determined from X-ray small-angle scattering measurements on an absolute scale. The most probable structure is chosen by comparison with spherical cylindrical and lamellar models. This method is applied to two-component micelles and it is possible to follow the variation of micellar dimensions when the concentration of each component is varying.

Two-component continuum spectrum X-ray pulsar EXO2030+375

1993 ◽  
Vol 13 (12) ◽  
pp. 383-386
Author(s):  
X.J. Sun ◽  
T.P. Li ◽  
M. Wu ◽  
L.X. Cheng
Keyword(s):  
X Ray ◽  
Continuum Spectrum ◽  
Two Component

A two-component X-ray spectrum from SMC X-1

1983 ◽  
Vol 266 ◽  
pp. 814 ◽  
Author(s):  
F. E. Marshall ◽  
R. H. Becker ◽  
N. E. White
Keyword(s):  
X Ray ◽  
Two Component

scholarly journals The X-ray Spectra of High Redshift Quasars

1989 ◽  
Vol 134 ◽  
pp. 161-166
Author(s):  
Claude R. Canizares ◽  
Julia L. White
Keyword(s):  
High Redshift ◽  
Radio Spectrum ◽  
Clear Correlation ◽  
X Rays ◽  
Spectral Parameters ◽  
X Ray ◽  
Systematic Uncertainties ◽  
Two Component ◽  
X Ray Background ◽  
Single Power

We present mean spectral parameters for various ensembles of quasars observed with the Einstein Observatory Imaging Proportional Counter (IPC). Our sample contains 71 optically or radio selected quasars with 0.1 < z < 3.5, Galactic NH < 1021 cm−2, total counts of 30 −500, and IPC gain < 19. Quasars are grouped into ensembles according to radio properties (Flat Radio Spectrum [FRS], Steep Radio Spectrum [SRS] or Radio Quiet [RQ]), and either redshift or X-ray luminosity, lx. We find a clear correlation between radio properties and α. FRS quasars have α∼0.4, SRS quasars have α∼0.7 and RQ quasars have α ∼1–1.4. There is no evidence for a dependence of α on z nor, for the FRS and SRS ensembles, on lx over nearly three decades. FRS quasars with 2.0 < z < 3.5 have just as flat mean spectra as those with low z, implying that a single power law, which is flatter than the canonical one with α ∼ 0.65, continues into the 1–10 keV band (in which the observed softer X-rays were emitted). Unfortunately, the results for high redshift and high lx RQ quasars are ambiguous because of systematic uncertainties in the ensemble means. Thus we cannot test the two-component spectral hypothesis of Wilkes and Elvis for these objects. SRS X-ray spectra could be steeper than FRS spectra because of the mixing of two components, although a single intrinsically steeper spectrum is easier to reconcile with the absence of z dependence. The uncertainty in a for RQ quasars with high z leaves open the important question of their contribution to the cosmic X-ray background.

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