Salyut-4 Observations of Active Regions on the Sun

1977 ◽  
Vol 36 ◽  
pp. 333-367 ◽  
Author(s):  
A.V. Bruns ◽  
G.M. Grechko ◽  
A.A. Gubarev ◽  
P.I. Klimuk ◽  
V.I. Sevastyanov ◽  
...  
Keyword(s):  
Fine Structure ◽  
Spatial Resolution ◽  
Physical State ◽  
High Spatial Resolution ◽  
Solar Spectrum ◽  
Active Regions ◽  
Spectral Lines ◽  
The Sun ◽  
Solar Image ◽  
Solar Plasma

We believe that the examination of the ultraviolet solar spectrum is the most informative tool for the diagnostic of the physical state of the solar plasma. But the well known phenomenon of fine structure of active regions (A.R.), as well as of quiet ones, making spectral lines to be wavy and patchy (across dispersion) demandsa) high spatial resolution on the solar image and b) stigmatic spectra.

Magnetospheres of Solar Active Regions Inferred from Spectral-Polarization Observations with High Spatial Resolution

1993 ◽  
Vol 419 ◽  
pp. 398 ◽  
Author(s):  
K. R. Lang ◽  
R. F. Willson ◽  
J. N. Kile ◽  
J. Lemen ◽  
K. T. Strong ◽  
...  
Keyword(s):  
Spatial Resolution ◽  
High Spatial Resolution ◽  
Active Regions ◽  
Solar Active Regions

scholarly journals WHY IS NON-THERMAL LINE BROADENING OF SPECTRAL LINES IN THE LOWER TRANSITION REGION OF THE SUN INDEPENDENT OF SPATIAL RESOLUTION?

2015 ◽  
Vol 799 (1) ◽  
pp. L12 ◽  
Author(s):  
B. De Pontieu ◽  
S. McIntosh ◽  
J. Martinez-Sykora ◽  
H. Peter ◽  
T. M. D. Pereira
Keyword(s):  
Transition Region ◽  
Spatial Resolution ◽  
Spectral Lines ◽  
The Sun ◽  
Line Broadening ◽  
Lower Transition ◽  
Thermal Line

A sub-micrometer resolution hard X-ray microprobe system of BL8C at Pohang Light Source

2015 ◽  
Vol 22 (5) ◽  
pp. 1306-1311 ◽  
Author(s):  
Nark-Eon Sung ◽  
Ik-Jae Lee ◽  
Kug-Seong Lee ◽  
Seong-Hun Jeong ◽  
Seen-Woong Kang ◽  
...  
Keyword(s):  
Trace Elements ◽  
Fine Structure ◽  
South Korea ◽  
Spatial Resolution ◽  
High Spatial Resolution ◽  
Structural Information ◽  
Complex Materials ◽  
X Ray ◽  
Pohang Light Source ◽  
X Ray Absorption

A microprobe system has been installed on the nanoprobe/XAFS beamline (BL8C) at PLS-II, South Korea. Owing to the reproducible switch of the gap of the in-vacuum undulator (IVU), the intense and brilliant hard X-ray beam of an IVU can be used in X-ray fluorescence (XRF) and X-ray absorption fine-structure (XAFS) experiments. For high-spatial-resolution microprobe experiments a Kirkpatrick–Baez mirror system has been used to focus the millimeter-sized X-ray beam to a micrometer-sized beam. The performance of this system was examined by a combination of micro-XRF imaging and micro-XAFS of a beetle wing. These results indicate that the microprobe system of the BL8C can be used to obtain the distributions of trace elements and chemical and structural information of complex materials.

High Resolution Balloon-Borne Spectrograph for the Near Solar Ultraviolet

1971 ◽  
Vol 41 ◽  
pp. 263-270 ◽  
Author(s):  
P. Lemaire
Keyword(s):  
Spatial Resolution ◽  
Focal Length ◽  
Solar Spectrum ◽  
Image Plane ◽  
Solar Image ◽  
Balloon Flight ◽  
Aperture Ratio ◽  
Cassegrain Telescope ◽  
Solar Ultraviolet ◽  
Better Than

In order to obtain the solar spectrum of the Mgii lines at 2795.5 Å and 2802.7 Å, we built a balloon instrument which consisted of a Cassegrain telescope, with an aperture ratio of F/20 and a focal length of 300 cm to give a solar image on the slit of a spectrograph. The theoretical spectral resolution is better than 10 mÅ. In the laboratory, we measured a spatial resolution of 10 μ in the image plane of the spectrograph, which corresponds to 1 arc sec in this mounting. During a balloon flight of 1969, April 30, which used a biaxial pointing system, we obtained a spatial resolution better than 10 arc sec, limited by the accuracy of the pointing system. Lastly, on 1970 June 24, the same instrument with a servosystem inside the telescope, was launched and spectral and spatial resolutions of 25 mÅ and about 3 arc sec, respectively, were obtained.

scholarly journals Variation of the generalized Compton red shift in the Sun

1988 ◽  
Vol 123 ◽  
pp. 447-450
Author(s):  
M. Missana
Keyword(s):  
Solar Spectrum ◽  
Systematic Difference ◽  
Compton Effect ◽  
Point Of View ◽  
Red Shift ◽  
Spectral Lines ◽  
The Sun ◽  
Average Depth ◽  
Made In

The most accurate measurements of red shifts in the solar spectrum, made in different epochs by different astronomers, show a systematic difference, in the average 2 mA° (0.2 pm), that seems quite independent on the wavelengths. Such a result can be explained, at least from a qualitative point of view, by the Compton effect. Indeed a variation of the normalized width U of the spectral lines causes a consequent variation of the Compton red shift: increasing U of the 50%, also the red shift increases of about 0.1 pm. Besides that a variation of the average depth h for the formation of the spectral lines in the reversing layer, may cause, in some model atmospheres a change of the red shift: an increase of about 90 Km for h may induce an increase of about 0.4 pm in the Compton red shift.

X-Ray Emission Associated with Filament Activity

1979 ◽  
Vol 44 ◽  
pp. 269-271 ◽  
Author(s):  
L.W. Acton ◽  
J.M. Mosher
Keyword(s):  
Spatial Resolution ◽  
Time Resolution ◽  
Active Regions ◽  
Spatial Relationships ◽  
Solar Plasma ◽  
X Ray ◽  
Small X ◽  
Temporal And Spatial

The purpose of this research is to investigate the temporal and spatial relationships of activated filaments, soft X-ray production, and Ha flares. The X-ray data are from the Lockheed Mapping X-Ray Heliometer (MXRH) on 0S0-8 (Wolfson et al., 1975, 1977). This instrument has been operating continuously since July 1975. It responds to radiation from solar plasma above about 2 × 106K, provides a time resolution of 20 sec, a spatial resolution of 2-3 arc min and has a basic sensitivity roughly equivalent to the 1-8 Å full disc monitors of, e.g., the SOLRAD and SMS/GOES satellites (threshold ≈ 2 × 10-9W/m2). However, because of its spatial resolution the MXRH permits study of small X-ray events in individual active regions even when the integrated solar X-ray emission is high.

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