scholarly journals Transit of the Sun across constellation Libra and variation of secondary gamma radiation flux in the month of October and November, 2020 at Udaipur, India

2021 ◽  
Vol 14 (8) ◽  
pp. 718-724
Author(s):  
Devendra Pareek ◽  
◽  
Prajesh Purohit
2020 ◽  
Vol 60 (8) ◽  
pp. 1087-1092
Author(s):  
A. G. Tlatov ◽  
V. M. Bogod ◽  
O. Pons ◽  
M. Rodriges ◽  
R. Estrada ◽  
...  

1991 ◽  
Vol 2 (2-3) ◽  
pp. 199-208
Author(s):  
Guy A. Letteer ◽  
John A. Jungerman ◽  
Carlos M. Castaneda

Radiocarbon ◽  
1992 ◽  
Vol 34 (3) ◽  
pp. 428-430 ◽  
Author(s):  
Páll Theodórsson ◽  
Lauri Kaihola ◽  
H. H. Loosli ◽  
José M. Rodríguez

An informal collaborative group of radiocarbon dating laboratories, the Low-Level Club, has been established to measure the gamma radiation flux and to test the efficiency of the anticoincidence counting system in laboratories with a NaI detector unit. The detector will record gamma radiation from cosmogenic nuclides, muons and secondary γ radiation formed in the passive shield by charged cosmic-ray particles. We present here the first phase of this work.


2012 ◽  
Vol 30 (8) ◽  
pp. 1129-1141 ◽  
Author(s):  
S. Krauss ◽  
B. Fichtinger ◽  
H. Lammer ◽  
W. Hausleitner ◽  
Yu. N. Kulikov ◽  
...  

Abstract. We analyzed the measured thermospheric response of an extreme solar X17.2 flare that irradiated the Earth's upper atmosphere during the so-called Halloween events in late October/early November 2003. We suggest that such events can serve as proxies for the intense electromagnetic and corpuscular radiation environment of the Sun or other stars during their early phases of evolution. We applied and compared empirical thermosphere models with satellite drag measurements from the GRACE satellites and found that the Jacchia-Bowman 2008 model can reproduce the drag measurements very well during undisturbed solar conditions but gets worse during extreme solar events. By analyzing the peak of the X17.2 flare spectra and comparing it with spectra of young solar proxies, our results indicate that the peak flare radiation flux corresponds to a hypothetical Sun-like star or the Sun at the age of approximately 2.3 Gyr. This implies that the peak extreme ultraviolet (EUV) radiation is enhanced by a factor of about 2.5 times compared to today's Sun. On the assumption that the Sun emitted an EUV flux of that magnitude and by modifying the activity indices in the Jacchia-Bowman 2008 model, we obtain an average exobase temperature of 1950 K, which corresponds with previous theoretical studies related to thermospheric heating and expansion caused by the solar EUV flux.


1991 ◽  
Vol 113 (2) ◽  
pp. 112-116 ◽  
Author(s):  
M. Schubnell ◽  
J. Keller ◽  
A. Imhof

In high temperature solar energy applications highly concentrating optical systems, such as, e.g., parabolic dishes, achieve typical radiation flux densities >2 MW/m2. In order to investigate thermo and photochemical reactions at temperatures >1500 K and radiation flux densities >2 MW/m2 a solar furnace was built at Paul Scherrer Institute (PSI). This furnace is a two-stage concentrator. The first stage is a prefocusing glass heliostat with a focal length of 100 m. The second stage is a highly concentrating parabolic dish with a focal length of 1.93 m. To design experiments to be carried out in the focal region of the parabolic dish, the radiation flux as well as its density distribution have to be known. This distribution is usually measured by radiometric methods. However, these methods are generally rather troublesome because of the high temperatures involved. In this paper we present a simple method to estimate the characteristic features of the radiation flux density distribution in the focal region of a concentrator system. It is well known from solar eclipses that the mean angular diameter of the moon is almost equal to that of the sun (9.1 mrad versus 9.3 mrad). Hence, the lunar disk is well suited to be used as a light source to investigate the flux distribution in a solar furnace. Compared to the sun the flux density is reduced by 4·105 and the flux density distribution can be inspected on a sheet of paper located in the plane of interest, e.g., the focal plane. This distribution was photographed and analyzed by means of an image processing system. The density distribution was also simulated using a Monte Carlo ray tracing program. Based on this comparison, and on further ray tracing computations, we show that the peak flux density decreases from 8.9 MW/m2 in December to values below 4 MW/m2 in June and the net radiation flux from 25 kW to 15 kW, respectively.


Atomic Energy ◽  
1961 ◽  
Vol 8 (1) ◽  
pp. 42-43 ◽  
Author(s):  
D. L. Broder ◽  
A. P. Kondrashov ◽  
A. A. Kutuzov ◽  
A. I. Lashuk

1970 ◽  
Vol 18 (6) ◽  
pp. 939-943 ◽  
Author(s):  
E.L. Chupp ◽  
D.J. Forrest ◽  
A.A. Sarkady ◽  
P.J. Lavakare

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