The Solar Limb Intensity Profile.

1961 ◽  
Vol 134 ◽  
pp. 323 ◽  
Author(s):  
John E. Gaustad ◽  
John B., Jr. Rogerson
Keyword(s):  
Solar Limb ◽  
Intensity Profile ◽  
Limb Intensity

The Solar Limb Intensity Profile.

1959 ◽  
Vol 130 ◽  
pp. 985 ◽  
Author(s):  
John B., Jr. Rogerson
Keyword(s):  
Solar Limb ◽  
Intensity Profile ◽  
Limb Intensity

scholarly journals Observation of Global 160-min Infrared (Differential) Intensity Variation of the Sun

1983 ◽  
Vol 66 ◽  
pp. 21-35
Author(s):  
V.A. Kotov ◽  
S. Koutchmy ◽  
O. Koutchmy
Keyword(s):  
Low Frequency ◽  
Intensity Variation ◽  
Solar Limb ◽  
The Sun ◽  
Average Amplitude ◽  
Instrument Analysis ◽  
Limb Intensity ◽  
Limb Darkening ◽  
Global Fluctuations ◽  
Made In

AbstractThe method developed and the instrument designed for detecting variations of the solar limb darkening at the atmospheric transparency window of the solar opacity minimum region of λ 1.65 µ are described. This differential technique proved to be successful in rejecting undesirable low frequency noises due to the atmosphere and to the instrument. Analysis of observations made in 1977, 1978, and 1981 indicates the persistance of global fluctuations of the IR differential, center-to-limb intensity at the wellknown 160 min period with an average amplitude of about ± 2 x 10-4 in units of the ‘average Sun’ intensity near 1.65 µm.

scholarly journals Determination of Temperature in Solar Prominences/Filaments Using FISS Observations

2013 ◽  
Vol 8 (S300) ◽  
pp. 85-89
Author(s):  
Jongchul Chae ◽  
Hyungmin Park ◽  
Donguk Song
Keyword(s):  
Source Function ◽  
Thermal Structure ◽  
Solar Limb ◽  
Intensity Profile ◽  
Fast Imaging ◽  
Background Intensity ◽  
Solar Prominences ◽  
Spectral Profiles ◽  
Constant Source

AbstractUsing the Fast Imaging Solar Spectrograph of the 1.6 meter New Solar Telescope at Big Bear, we simultaneously took the spectral profiles of the Hα line and the Ca ii line at 854.2 nm from prominences beyond the solar limb and filaments on the disk. The spectral data were fitted by the slab model of radiative transfer with constant source function, either with zero background intensity profile (in prominences) or with carefully constructed background intensity profile (in filaments). These observations with different perspectives and different analyses produced consistent results: temperature inside prominences/filaments ranges from 4000 to 20000 K with a mean of about 9500 K. We expect that this kind of observation and analysis with higher spatial resolution and higher temporal resolution will allow us to study in detail the thermal structure and evolution of plasma in prominences.

July 11, 1991 Eclipse Corona Photometry by the Results of Electropolarimetric and CCD-Matrix Observations

1994 ◽  
Vol 144 ◽  
pp. 567-569
Author(s):  
V. Kulidzanishvili ◽  
D. Georgobiani
Keyword(s):  
Solar Corona ◽  
Observational Data ◽  
Solar Limb ◽  
Ccd Matrix

AbstractThe observational data of July 11, 1991 eclipse solar corona obtained by both electropolarimeter (EP) and CCD-matrix were processed. Using these data, the solar corona photometry was carried out. The results of EP data are compared with the ones of CCD data. It must be noted here that the CCD data give us only characteristics of the inner corona, while the EP data show the features of both the inner and middle corona up to 4R⊙. Standard flattening indexϵis evaluated from both data. The dependence of the flattening index on the distance from the solar limb is investigated. The isophotes in Na and Ca lines are plotted. Based on these data some ideas and conclusions on the type of the solar corona are presented.

Synoptic Charts of the Solar Eclipses of 1990 and 1991

1994 ◽  
Vol 144 ◽  
pp. 517-521
Author(s):  
Z. Mouradian ◽  
G. Buchholtz ◽  
G. Zlicaric
Keyword(s):  
Solar Limb ◽  
Active Regions ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractThe synoptic charts of solar rotations 1831 and 1844 have been drawn up, corresponding to the eclipses of 22 July 1990 and 11 July 1991. These charts contain the active regions and the filaments, and show the position of the solar limb, at the time of the eclipse. They are for use in studying the coronal structures observed during these eclipses. The variation of these structures is given in the table. The last section of the article contains a formula for identifying the structures out of the limb.

Effects of the Laser Intensity Profile on Ignition of Hydrogen-Air Mixture

2021 ◽  
Author(s):  
Albina Tropina ◽  
Sagar Pokharel ◽  
Mikhail N. Shneider
Keyword(s):  
Laser Intensity ◽  
Intensity Profile

scholarly journals Solar Irradiance Variability Due to Solar Flares Observed in Lyman-Alpha Emission

Solar Physics ◽  
2021 ◽  
Vol 296 (3) ◽  
Author(s):  
Ryan O. Milligan
Keyword(s):  
Solar Flares ◽  
Solar Spectrum ◽  
Neutral Hydrogen ◽  
Solar Limb ◽  
High Background ◽  
Superposed Epoch Analysis ◽  
Lyman Alpha ◽  
Alpha Emission ◽  
Epoch Analysis ◽  
Very High

AbstractAs the Lyman-alpha (Ly$\upalpha $ α ) line of neutral hydrogen is the brightest emission line in the solar spectrum, detecting increases in irradiance due to solar flares at this wavelength can be challenging due to the very high background. Previous studies that have focused on the largest flares have shown that even these extreme cases generate enhancements in Ly$\upalpha $ α of only a few percent above the background. In this study, a superposed-epoch analysis was performed on ≈8500 flares greater than B1 class to determine the contribution that they make to changes in the solar EUV irradiance. Using the peak of the 1 – 8 Å X-ray emission as a fiducial time, the corresponding time series of 3123 B- and 4972 C-class flares observed in Ly$\upalpha $ α emission by the EUV Sensor on the Geostationary Operational Environmental Satellite 15 (GOES-15) were averaged to reduce background fluctuations and improve the flare signal. The summation of these weaker events showed that they produced a 0.1 – 0.3% enhancement to the solar Ly$\upalpha $ α irradiance on average. For comparison, the same technique was applied to 453 M- and 31 X-class flares, which resulted in a 1 – 4% increase in Ly$\upalpha $ α emission. Flares were also averaged with respect to their heliographic angle to investigate any potential center-to-limb variation. For each GOES class, the relative enhancement in Ly$\upalpha $ α at the flare peak was found to diminish for flares that occurred closer to the solar limb due to the opacity of the line and/or foreshortening of the footpoints. One modest event included in the study, a C6.6 flare, exhibited an unusually high increase in Ly$\upalpha $ α of 7% that may have been attributed to a failed filament eruption. Increases of this magnitude have hitherto only been associated with a small number of X-class flares.

X-ray imaging of a solar limb flare on 1982 January 22

Solar Physics ◽  
1986 ◽  
Vol 107 (1) ◽  
pp. 109-121 ◽  
Author(s):  
T. Takakura ◽  
K. Tanaka ◽  
N. Nitta ◽  
K. Kai ◽  
K. Ohki
Keyword(s):  
Solar Limb ◽  
X Ray ◽  
X Ray Imaging ◽  
Limb Flare

Theoretical explanation of the solar limb effect

1971 ◽  
Vol 19 (6) ◽  
pp. 659-667 ◽  
Author(s):  
Cs. Ferencz ◽  
Gy. Tarcsai
Keyword(s):  
Solar Limb ◽  
Theoretical Explanation ◽  
Limb Effect
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