Nikonov, V.B. და ნიკონოვი, ვ. და Никонов, В.Б. (1938) მზის გვირგვინის სრული გამოსხივების რედიომეტრული განსაზღვრის ცდა 1936 წლის 19 ივნისის მზის სრული დაბნელების დროს / Radiometric determination of the total radiation from the solar corona June 19, 1936. აბასთუმნის ასტროფიზიკური ობსერვატორიის ბიულეტენი / Bulletin of the Abastumani Astrophysical Observatory (3). С. 77-89.
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1938-I-9.pdf Download (2MB) | გადახედვა |
რეზიუმე
The result of an attempt to determine radiometrically the total amount of radiation from the solar corona during the total solar eclipse of June 19, 1936 are discussed below. The corona was observed by means of a special radiometer arranged as shown in Fig.2. A spherical mirror O1 (D=120 mm; F=300 mm) projects the corona image on the front surface of a double fluorite lens O2 (D =9 mm; F=11.5 mm). The angular diameter of the lens field equals 1.71 enabling the measurement of the coronal radiation up to 36' from the sun limb. The image of the mirror, diminished to the size of 5.3 mm and filled uniformly wit light, is thrown from the lens O2 on one of the junctions of the compensating thermocouple T. Thus, a uniform illumination of the thermocouple is obtained independent from the size and from of the measured image and, consequently the direct comparison of the coronal and lunar radiation is made possible. A lamellated bismuth-antimony thermocouple lined with mica and provided with a fluorite window was used. Its resistance equals 3 ohm and sensitivity 0.2 μV/μcal. The termocurrent was measured with a Zernicke Ze galvanometer. The observations were made measuring successively the corona and the background at a distance of 5 from it. The observed mean deflection from the corona was found to bee 7.2 mm. To obtain the energetic magnitude of the total radiation from the solar corona the observations of the full moon were carried out. The reduction for extinction was made on the ground of actinometric observations. The value obtained for the total amount of the coronal radiation seems to be somewhat exaggerated. It is possible that the errors due to the uncertainty of the reduction for atmospheric extinction are involved in the results. Nevertheless, the data obtained indicate clearly enough the excess of infra-red in the outer parts of the corona. We have ground to believe that radiometric observations by the above described method will yield in future reliable value of the total coronal radiation and will definitively solve the problem of the presence of infra-red excess in the corona, provided that the whole apparatus be carefully standardized and the specially determined exact corrections for extinction be used. October, 1937
| ობიექტის ტიპი: | სტატია |
|---|---|
| თემატიკა: | Q Science > QB Astronomy |
| ქვეგანყოფილება: | Institutes > Evgeny Kharadze Abastumani National Astrophysical Observatory |
| განმათავსებელი მომხმარებელი: | თამარ ჭაღიაშვილი |
| განთავსების თარიღი: | 09 ივლისი 2018 10:58 |
| ბოლო ცვლილება: | 09 ივლისი 2018 10:58 |
| URI: | http://eprints.iliauni.edu.ge/id/eprint/8173 |
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