排序方式： 共有24条查询结果，搜索用时 31 毫秒
1.
Photographs of the corona in the continuum spectrum (580–700 nm) have been obtained with a doublet camera (F=4m) through rotating sector polarizers with the vibrational directions oriented radially and tangentially to the solar limb. Isophotes of the total emission and its polarized component, as well as diagrams giving the degree of polarization for the (K+F)-corona and the electron corona proper (P
K), have been plotted up to the distance of 1R
from the limb. In some inner regions the polarizationP
K exceeds the highest value possible for Thomson scattering under the given conditions. The reality of this anomally is dubious; systematic photometrical errors may account for it. Three-dimensional forms of 15 different coronal rays have been ascertained by comparing the course of polarization along the rays to the family of Baumach curves. The rays are found to deflect substantially from the radial directions out of the plane of the sky. Mean values of the coronal brightness and polarization versus the distance from the Sun have been determined. Contrary to well-known models (Van de Hulst) the mean polarization of the electron corona (P
K) decreases with distance after reaching the maximum (50%) at (1.4–1.6)R
from the Sun's centre. This decrease can be explained by deflection of the streamers from radial directions. 相似文献
2.
G. M. Nikolsky 《Solar physics》1969,6(3):399-409
This paper is a result of the evolution of researches on the prediction and identification of the solar EUV spectrum by Ivanov-Holodny and the author.An absolute calibration of the solar EUV spectrum is given. The corresponding energy distribution is shown in Figure 2. During the minimum solar activity the radiation flux in the range below 1027 Å near the earth is 2.6 erg/cm2 sec, in the maximum it is 8 erg/cm2 sec.Abundances of fifteen elements in the solar atmosphere were deduced (Table III) from a comparison of predicted and observed intensities of more than 300 lines in the spectral region below 1215 Å. 相似文献
3.
K. Y. Kondratiev I. Y. Badinov G. N. Gaevskaya G. A. Nikolsky M. P. Fedorova 《Pure and Applied Geophysics》1964,58(1):187-203
Summary The present research considers the vertical profiles of the radiation balance and its components for summer and autumn seasons measured by standard actinometric instruments fixed on free balloons and gives the values of radiational temperature changes in the layers of 1000 to 500 and 1000 to 20 mb. 相似文献
4.
The new Lyot-coronagraph with 53 cm objective is described. The coronagraph has a grating spectrograph. The solar disk image on the slit of the spectrograph is 12.6 cm. The dispersion is 1 Å/mm in the second order. The coronagraph is situated at the Kislovodsk Station of Pulkovo Observatory, 2050 m above sea level. 相似文献
5.
Golionko B. G. Basilyan A. E. Nikolsky P. A. Kostyleva V. V. Malyshev N. A. Verzhbitsky V. E. Obmetko V. V. Borodulin A. A. 《Geotectonics》2019,53(6):675-699
Geotectonics - Detailed lithological, stratigraphic, and structural studies of the fold-thrust structures were conducted on New Siberia Island. We have established that the jointly deformed... 相似文献
6.
Yudintsev S. V. Malkovsky V. I. Nikolsky M. S. Nikonov B. S. 《Doklady Earth Sciences》2019,485(1):303-307
Doklady Earth Sciences - It is suggested to dispose of radioactive wastes of nuclear energetics with long-lived actinides in the form of titanates and zirconates in boreholes up to 5 km deep. The... 相似文献
7.
Slit spectrograms of a quiescent prominence and the inner corona (h2.5 arc min) in the range 3400–7000 Å (dispersion 6–10 Å/mm) were obtained. From an analysis of the Stark effect on the Balmer lines (up to number 36) the electron density in the prominence n
e = (7 ± 3) × 1010 cm–3 was deduced. The kinetic temperature T
k and the non-thermal velocities
t, found from a simultaneous consideration of the Balmer and metal lines, are T
k 10 000 K and v
t6 km/s. Also the emission measure of the prominence along the line-of-sight was found: ME = 1031 cm–5.In the coronal spectrum 24 coronal lines were found. Thirteen of these lines were identified and measured photometrically to get their absolute intensities, profiles and halfwidths. For nine lines the intensities as a function of the height were studied and on this basis the coronal lines were divided into a few groups. The line-of-sight and non-thermal velocities are
r 10 km/s and
t 25 km/s. The coronal lines originate in at least three types of regions with different temperatures. The emission measure as a function of the ionization temperature was determined. The abundances of four elements of the iron group (V, Cr, Mn, Co) were estimated. The abundances of the other elements of the same group (A, Ca, Fe, Ni), found from EUV-data, are in a good agreement with our observations. The degree of inhomogeneity in the corona was estimated:
. 相似文献
8.
A series of H-spectrograms obtained with the 21 in. Lyot coronagraph has been examined. Measurements of relative distances between spicules (nearly 50 features) embrace the time interval of about 21 min (38 pictures). It is found out that spicules oscillate along the limb with a characteristic time interval (period) about 1 min, characteristic amplitude of 1 arc sec and velocities about 10–15 km/s. The oscillations show no correlation for distant spicules. 相似文献
9.
A new type of magnetograph has been built capable to measure weak magnetic fields in the chromosphere and corona. Measurements of magnetic field in two prominences are demonstrated as examples. 相似文献
10.
K. Ya. Kondratyev G. A. Nikolsky E. O. Shultz 《Meteorology and Atmospheric Physics》1996,61(3-4):119-126
Summary The most significant solar spectral radiation bursts that occurred during more than twelve-years observation period at an high altitude station are analyzed. It is shown that the number and amplitudes of solar spectral bursts increase when the solar activity (SA) maximum is approaching. A plausible mechanism of short-term variations of extra-atmospheric solar spectral irradiance (ETSSI) is discussed. It appears that a burst of ETSSI arises when the Earth is sporadically irradiated by a strong flux of induced violet-blue high coming out of magnetic flux tubes in the active region (AR) of the Sun. We confirm earlier conclusions that on the time-scale of decades there is a close relationship between variations in the areas of faculae, the solar constant, and surface air temperature. On the basis of these results we suggest that at the end of the 1930s, when the Sun was very active, its effective output was about 0.4%, and the surface temperature in the Northern hemisphere about 0.4°C, higher than in the first decade of the 20th century.With 5 Figures 相似文献