scholarly journals The X-Ray Flare of π UMA : Temperature and Emission Measure

1989 ◽  
Vol 104 (2) ◽  
pp. 127-130
Author(s):  
M. Landini ◽  
B.C. Monsignori Fossi
Keyword(s):  
Temperature Gradient ◽  
Power Supply ◽  
Emission Measure ◽  
Low Energy ◽  
Loop Model ◽  
Medium Energy ◽  
Differential Emission Measure ◽  
X Ray ◽  
Spectral Bands

AbstractAn X-ray flare from the star π UMA has been observed by EXOSAT on January 31, 1984. The data were collected using the-Low Energy Experiment and the Medium Energy Experiment, sensitive to the spectral bands 0.04 - 2 Kev and 1-20 Kev (Landini et al. 1986).The temperature and emission measure variations during the flare are deduced under the isothermal assumption. Using a parametrized profile of the differential emission measure, wich is controlled by the conductive flux via the temperature gradient, the comparison with the observed data gives some insight on a “mean loop” model and its power supply.

Exosat Observations of H2252−035: Pulse Phase and Orbital Phase Dependent Low Energy Absorption and Iron Line Emission

1987 ◽  
Vol 93 ◽  
pp. 281-292
Author(s):  
W. Pietsch ◽  
W. Voges ◽  
E. Kendziorra ◽  
M. Pakull
Keyword(s):  
Energy Absorption ◽  
Line Emission ◽  
Low Energy ◽  
Gas Absorption ◽  
X Rays ◽  
Medium Energy ◽  
Iron Line ◽  
X Ray ◽  
Low Energies ◽  
Optical Light Curve

AbstractThe 805 sec pulsing X-ray source H2252−035 has been observed for 7 h on September 14/15 and on September 17, 1983 in X-rays with the low energy telescope and the medium energy detectors of EXOSAT. While below 2 keV the semiamplitude of the 805 s pulses is ~ 100% in the 2.3–7.9 keV band it is only ~ 40%. X-ray dips that are more pronounced in low energies occur simultaneously with the orbital minimum of the optical light curve. The medium energy spectra during dips with respect to the non dip spectrum can be explained by just enhanced cold gas absorption of an additional absorbing column of 2 1022 cm−2. Model spectra for the 805 s minimum have to include a strong iron emission line at 6.55 keV with an equivalent width of 3 keV in addition to a reduced continuum intensity (radiating area) and enhanced low energy absorption.

scholarly journals First Determinations of Differential Emission Measure Distribution from RESIK X-ray Spectra

2004 ◽  
Vol 2004 (IAUS223) ◽  
pp. 461-462 ◽  
Author(s):  
A. K[ecedilla]pa ◽  
J. Sylwester ◽  
B. Sylwester ◽  
M. Siarkowski
Keyword(s):  
Emission Measure ◽  
Differential Emission Measure ◽  
X Ray ◽  
Measure Distribution

scholarly journals X-ray bursting activity in the BL Lacertae object PKS 2155-304

1986 ◽  
Vol 119 ◽  
pp. 267-268
Author(s):  
D. Maccagni ◽  
L. Chiappetti ◽  
L. Maraschi ◽  
D. Molteni ◽  
M. Morini ◽  
...  
Keyword(s):  
Exposure Time ◽  
Low Energy ◽  
Medium Energy ◽  
X Ray ◽  
Bl Lacertae ◽  
Bl Lac ◽  
Proportional Counters ◽  
Bursting Activity

The bright BL Lac object PKS 2155-304 (mv=13; z=0.117) was observed with EXOSAT at five epochs (1983 Oct. 31, Nov. 30, 1984 Nov. 6, 7 and 11), for a total of about 30 hours of exposure time. Here we present data and results obtained with the Low Energy (LE) telescopes, in the band 0.05–2. keV, and with the Medium Energy (ME) argon proportional counters in the range 1.–6. keV.

scholarly journals Overview of XRT performance and first results

2007 ◽  
Vol 3 (S247) ◽  
pp. 326-336
Author(s):  
Antonia Savcheva ◽  
Keyword(s):  
Fine Structure ◽  
Coronal Holes ◽  
Emission Measure ◽  
Active Regions ◽  
Potential Fields ◽  
Differential Emission Measure ◽  
Short Introduction ◽  
X Ray ◽  
First Results ◽  
Measure Analysis

AbstractIn this review we present a short introduction to the X-ray Telescope on Hinode. We discuss its capabilities and new features and compare it with Yohkoh SXT. We also discuss some of the first results that include observations of X-ray jets in coronal holes, shear change in flares, sigmoid eruptions and evolution, application of filter ratios and differential emission measure analysis, structure of active regions, fine structure of X-ray bright points, and modeling non-potential fields around filaments. Finally, we describe how XRT works with other ground and space-based instrumentation, in particular with TRACE, EIS, SOT, and SOLIS.

Determination of differential emission measure from X-ray solar spectra registered by RESIK aboard CORONAS-F

2006 ◽  
Vol 40 (4) ◽  
pp. 294-301 ◽  
Author(s):  
A. Kepa ◽  
J. Sylwester ◽  
B. Sylwester ◽  
M. Siarkowski ◽  
A. I. Stepanov
Keyword(s):  
Emission Measure ◽  
Differential Emission Measure ◽  
X Ray

scholarly journals Differential emission measure analysis of hot-flare plasma from solar-maximum mission X-ray data

1984 ◽  
Vol 4 (7) ◽  
pp. 203-207 ◽  
Author(s):  
J. Jakimiec ◽  
J. Sylwester ◽  
J.R. Lemen ◽  
R. Mewe ◽  
R.D. Bentley ◽  
...  
Keyword(s):  
Solar Maximum ◽  
Emission Measure ◽  
Differential Emission Measure ◽  
Solar Maximum Mission ◽  
X Ray ◽  
Measure Analysis ◽  
Flare Plasma
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