scholarly journals A High Spectral Resolution Observation of the Soft X‐Ray Diffuse Background with Thermal Detectors

2002 ◽  
Vol 576 (1) ◽  
pp. 188-203 ◽  
Author(s):  
D. McCammon ◽  
R. Almy ◽  
E. Apodaca ◽  
W. Bergmann Tiest ◽  
W. Cui ◽  
...  
Keyword(s):  
Spectral Resolution ◽  
High Spectral Resolution ◽  
X Ray ◽  
Thermal Detectors ◽  
Resolution Observation ◽  
Diffuse Background

Thermal Detectors for X-ray Astronomy

1990 ◽  
Vol 115 ◽  
pp. 346-356
Author(s):  
Stephen S. Holt
Keyword(s):  
High Resolution ◽  
Quantum Efficiency ◽  
Spectral Resolution ◽  
High Spectral Resolution ◽  
X Ray ◽  
Thermal Detectors ◽  
The Sacrifice

AbstractSpectroscopy is traditionally characterized by the sacrifice of quantum efficiency for high spectral resolution. Since X-ray astronomy is a photon-limited discipline, the choice between high resolution for very few sources versus much lower resolution for many more has not always been an easy one. The development of new thermal detectors offers the opportunity to “have one’s cake and eat it, too.”

scholarly journals High Spectral Resolution Observations of Coronal X-Ray Emission from the RS CVn Binary Sigma Corona Borealis

1984 ◽  
Vol 86 ◽  
pp. 143-146
Author(s):  
G.R. Riegler ◽  
P.C. Agrawal ◽  
T.H. Markert
Keyword(s):  
Spectral Resolution ◽  
Emission Measure ◽  
High Spectral Resolution ◽  
Loop Model ◽  
X Ray ◽  
Resolution Observation ◽  
Volume Emission ◽  
Best Fit ◽  
Spectral Scan ◽  
Prominent Peak

Results of a high spectral resolution observation of the RS CVn binary σ Cr B, made with the Focal Plane Crystal Spectrometer (FPCS) on the Einstein Observatory, are reported. A spectral scan in the 800–840 eV interval shows clear presence of an X-ray emission line at 826 eV identified with the 1S0 − 1P1 transition of Fe XVII. A prominent peak at 1007 eV in the scan band 987–1013 eV is attributed to a blend of lines due to Fe XVII and Fe XXI. Using the observed line fluxes and the Raymond-Smith model, best fit values of corona temperature and volume emission measure, with associated 90% confidence level uncertainties, are derived to be (6.9 ± 0.8) × 106 K and (1.7 ± 0.7) × 1053 cm−3, respectively. Pressure and density of the X-ray emitting plasma and loop length are deduced by applying a Constant Pressure Coronal Loop Model.

Comparison of solar soft X-ray irradiance from broadband photometers to a high spectral resolution rocket observation

2009 ◽  
Vol 43 (3) ◽  
pp. 349-354 ◽  
Author(s):  
Thomas N. Woods ◽  
Phillip C. Chamberlin
Keyword(s):  
Spectral Resolution ◽  
High Spectral Resolution ◽  
X Ray

scholarly journals High spectral resolution observations of the coronal X-ray emission from the RS CVn binary Sigma Corona Borealis

1985 ◽  
Vol 213 (4) ◽  
pp. 761-771 ◽  
Author(s):  
P. C. Agrawal ◽  
T. H. Markert ◽  
G. R. Riegler
Keyword(s):  
Spectral Resolution ◽  
High Spectral Resolution ◽  
X Ray

scholarly journals Goals for the Application of High-Resolution X-ray Spectroscopy to the Diagnosis of Stellar Coronal Plasmas

1990 ◽  
Vol 115 ◽  
pp. 94-109 ◽  
Author(s):  
Jeffrey L. Linsky
Keyword(s):  
High Resolution ◽  
Spectral Resolution ◽  
Transient Flow ◽  
Emission Measure ◽  
Active Regions ◽  
High Sensitivity ◽  
High Spectral Resolution ◽  
Spectral Features ◽  
Signal To Noise ◽  
X Ray

AbstractI provide examples of how high-resolution x-ray spectra may be used to determine the temperature and emission measure distributions, electron densities, steady and transient flow velocities, and location of active regions in stellar coronae. For each type of measurement I estimate the minimum spectral resolution required to resolve the most useful spectral features. In general, high sensitivity is required to obtain sufficient signal-to-noise to exploit the high spectral resolution. Although difficult, each measurement should be achievable with the instrumentation proposed for AXAF.

scholarly journals About diagnostics of Z-pinches hot points

2000 ◽  
Vol 18 (2) ◽  
pp. 291-296 ◽  
Author(s):  
V.Yu. POLITOV ◽  
A.V. POTAPOV ◽  
L.V. ANTONOVA
Keyword(s):  
Experimental Data ◽  
Theoretical Analysis ◽  
Spectral Resolution ◽  
High Spectral Resolution ◽  
Electrical Discharges ◽  
Maximum Compression ◽  
X Ray ◽  
Average Temperature ◽  
Radiation Spectra ◽  
Spectral Intensities

We present the results of X-ray diagnostics of Z-pinch hot points, formed during fast electrical discharges through exploding Al wires. Experimental data include the pinhole images and X-ray time integrated radiation spectra. These spectra were obtained with high spectral resolution in the range 1.5–2.2 keV, contained the most intensive resonance lines of Al H- and He-like ions. Comparison of the recorded lines width and peak intensities with the corresponding modeled values, enables us to estimate the main hydrodynamical parameters of hot point, such as average temperature and density, being achieved at a moment of its maximum compression. Additionally, on the base of theoretical analysis of the spectral intensities distribution in well-resolved Lyα satellites, the gradient of compression velocities field is concluded. Some features of the investigated lines spectra forming are discussed.

scholarly journals High spectral resolution x-ray optics with highly oriented pyrolytic graphite

2006 ◽  
Vol 14 (10) ◽  
pp. 4570 ◽  
Author(s):  
H. Legall ◽  
H. Stiel ◽  
V. Arkadiev ◽  
A. A. Bjeoumikhov
Keyword(s):  
Spectral Resolution ◽  
Pyrolytic Graphite ◽  
High Spectral Resolution ◽  
Highly Oriented Pyrolytic Graphite ◽  
Ray Optics ◽  
X Ray

scholarly journals High Spatial/Spectral Resolution Studies of Eta Carinae

2005 ◽  
Vol 13 ◽  
pp. 799-801
Author(s):  
Theodore R. Gull ◽  
Keyword(s):  
Spectral Resolution ◽  
Large Scale ◽  
High Spectral Resolution ◽  
Space Telescope ◽  
X Ray ◽  
Eta Carinae ◽  
Imaging Spectrograph

AbstractWe have used the high spatial and high spectral resolution of the Space Telescope Imaging Spectrograph (STIS) to study Eta Carinae and the Homunculus. Since the last minimum in 1998.0, CCD spectral modes have followed changes in the Eta Carinae, and large-scale changes in the Homunculus. Since 2001.7, MAMA echelle-mode observations have followed changes in the Eta Carinae and the very nearby ejecta through the 2003.5 minimum. Very significant changes in the star and nebular occur as the X-Ray drop occurs in the minimum.

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