共查询到20条相似文献，搜索用时 46 毫秒
1.
Observations of coronal holes, solar wind streams, and geomagnetic disturbances during 1973–1976 are compared in a 27-day pictorial format which shows their long-term evolution. The results leave little doubt that coronal holes are related to the high-speed streams and their associated recurrent geomagnetic disturbances. In particular, these observations strongly support the hypothesis that coronal holes are the solar origin of the high-speed streams observed in the solar wind near the ecliptic plane.Visiting Scientist, Kitt Peak National Observatory, Tucson, Arizona.Operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation. 相似文献
2.
Observations of solar radio emission at 3 cm wavelength have been made at Japal-Rangapur Observatory for 1980–1981, the solar maximum year using the 3 m radio telescope. The correlation between microwave solar emissions and the sunspot activity on monthly basis has been found to be high during the maximum phase and in the high cm wavelength band. The basic component has been estimated statistically for successive solar rotations using the data obtained at Japal-Rangapur Observatory. Further, this was compared with the data obtained at other cm wavelengths during 1980–1981 and the solar minimum period 1975–1976 of the 21st cycle. The comparison showed pronounced dips in flux levels at different wavelengths during the summer months of the solar maximum year which may be attributed to the presence of coronal holes in the various levels of the solar atmosphere. The computed basic component values showed pronounced variation at high cm wavelengths for the solar maximum period with dissimilar variations at different wavelengths. During the solar minimum period the variations were negligibly small and showed more or less constant level of activity.Paper presented at the IAU Third Asian-Pacific Regional Meeting, held in Kyoto, Japan, between 30 September–6 October, 1984. 相似文献
3.
Jerome T. Nolte Michel Gerassimenko Allen S. Krieger Craig V. Solodyna 《Solar physics》1978,56(1):153-159
We have compared sudden shifts in coronal hole boundaries observed by the S-054 X-ray telescope on Skylab between May and November, 1973, within 1 day of CMP of the holes, at latitudes 40 °, with the long-term evolution of coronal hole area. We find that large-scale shifts in boundary locations can account for most if not all of the evolution of coronal holes. The temporal and spatial scales of these large-scale changes imply that they are the results of a physical process occurring in the corona. We conclude that coronal holes evolve by magnetic field lines opening when the holes are growing, and by fields closing as the holes shrink.Skylab Solar Workshop post-doctoral appointee 1975–1976. The Skylab Solar Workshops are sponsored by NASA and NSF and managed by the High Altitude Observatory, National Center for Atmospheric Research. 相似文献
4.
Byurakan Astrophysical Observatory and Geneva Observatory. Translated from Astrofizika, Vol. 36, No. 1, pp. 35–54, January–Feburary, 1993. 相似文献
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6.
Byurakan Astrophysical Observatory; Geneva Observatory. Translated from Astrofizika, Vol. 34, No. 3, pp. 301–314, May–June, 1991. 相似文献
7.
Byurakan Astrophysical Observatory; Armagh Observatory (Northern Ireland). Translated from Astrofizika, Vol. 34, No. 3, pp. 327–332, May–June, 1991. 相似文献
8.
Stepanyan Dzh A. Lipovetskii V. A. Chavushyan V. O. Erastova L. K. Shapovalova A. I. 《Astrophysics》1991,34(1):1-6
Byurakan Astrophysical Observatory; Special Astrophysical Observatory, USSR Academy of Sciences. Translated from Astrofizika, Vol. 34, No. 1, pp. 5–12, January–February, 1991. 相似文献
9.
Byurakan Astrophysical Observatory and Special Astrophysical Observatory, Academy of Sciences. Translated fromAstrofizika, Vol. 35, No. 1, pp. 67–75, July–August, 1991. 相似文献
10.
N. R. Sheeley Jr. 《Solar physics》1980,65(2):229-235
He i 10830 Å synoptic maps, obtained at the Kitt Peak National Observatory during 1974–1979, show that the Sun's polar coronal holes have contracted significantly during 1977–1978. Prior to the accelerated increase of sunspot activity in mid-1977, the area of each polar cap was on the order of 8% of the Sun's total surface area (4R
2), whereas toward the end of 1978 these areas fell below 2% of 4R
2. Synoptic polar plots show that the vestigual holes had irregular shapes and were often well removed from the poles themselves. These results are consistent with the changes that one would expect when the polar magnetic fields are weakening just prior to sunspot maximum. 相似文献
11.
The night-to-night and short-term variations inUBV light curves of EW Lac which were made during 1982–1984 at Yonsei University Observatory are discussed. The long-term variability in the photometric behaviour of the star is examined with our own data as well as those of Harmanecet al. (1980).Paper presented at the IAU Third Asian-Pacific Regional Meeting, held in Kyoto, Japan, between 30 September–6 October, 1984.Yonsei University Observatory Contribution No. 23. 相似文献
12.
Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 34, No. 3, pp. 449–457, May–June, 1991. 相似文献
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Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 36, No. 1, pp. 5–13, January–February, 1993. 相似文献
14.
N. A. Volchkova 《Astrophysics》1993,36(1):34-36
Crimean Astrophysical Observatory. Translated from Astrofizika, Vol. 36, No. 1, pp. 61–65, January–February, 1993. 相似文献
15.
The behavior of the symbiotic nova RT Ser from 1940 to 1994 from photographic observations made at the Gissar Observatory (1940–1978) and BVR-band observations at the Crimean Observatory (1983–1994) is analyzed. The outburst lightcurve shows a linear decline at a rate of 0m.06 per year. It appears from the nature of the outburst attenuation that the fading, having already lasted about 80 yr, is still continuing. Judging from the color indices, the principal contribution to the visible light from the system is made by a cool, late-type red giant and hot gas the source of which is, as yet, unknown. The photometric variability observed in the BVR bands with a characteristic time of 10 yr is confirmed by photographic observations of 1928–1978. The period determined from all the data is 9.6 yr and is most likely orbital.Translated fromAstrofizika, Vol. 39, No. 1, pp. 31–40, January–March, 1996. 相似文献
16.
During the summer of 1985, the CIGALE Perot-Fabry scanning interferometer of Marseilles Observatory was installed at the prime focus of the 2.6 m telescope of Byurakan Observatory. The long run (two new moons) was successful and gave matereial for numerous publications.Published in Astrofizika, Vol. 38, No. 4, pp. 619–624, October–December, 1995. 相似文献
17.
Leningrad State University; Crimean Astrophysical Observatory. Translated from Astrofizika, Vol. 34, No. 2, pp. 181–198, March–April, 1991. 相似文献
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Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 34, No. 3, pp. 357–378, May–June, 1991. 相似文献
19.
Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 34, No. 2, pp. 199–204, March–April, 1991. 相似文献
20.
Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 36, No. 3, pp. 315–332, July–September, 1993. 相似文献