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211.
《Atmósfera》2014,27(3):227-237
The O+ ion density measured by the SROSS-C2 satellite during solar minima (year 1995, F10.7 = 77) and maxima (year 2000, F10.7 = 181) has been analyzed for studying diurnal, seasonal, latitudinal and geomagnetic variations. The study region covers an area encompassed between 5-3 5° N latitude and 65-95° E longitude over India at a ~500 km altitude (F2 region). The year 2000 shows significant enhancement in the annual average of O+ ion density and attainment of post sunset secondary enhancement compared to 1995. Attributed to photoionization, daytime shows a maximum ionization compared to nighttime. However, attainment of post sunset secondary maxima is attributed to the strong pre-reversal enhancement in the vertical E x B drift. The effect of geomagnetic activity Kp through the E x B drift dynamic movement on O+ ion density distribution studies indicates periodicities of seven and nine days in 1995 and 2000, respectively, and polynomial dependency of the O+ ion density on geomagnetic activity Kp. Further on, stratification of the O+ ion density according to latitude (5-35° N) indicates high density in mid-latitudes (12-24° N) compared to high and low latitudes, except in the winter of 1995, which shows a distinct trend (i.e., density decreases with increasing latitude). 相似文献
212.
"数字开发区"的理念就是把开发区作为一个生态系统,其中的居民、交通、能源、商业、通信、水资源等构成一个整体,各部分相互联系、彼此影响。本文简要介绍了"智慧利民"数字开发区建设及实际应用情况。 相似文献
213.
214.
NNR������ITRF��ȫ�����˶�ģ�� 总被引:1,自引:0,他引:1
????????ITRF2000???????????????????????????ITRF2000??1 mm/a????????????NNR??NUVEL1A?????????????NNR????;??????????????????????????????????ж?ITRF??????????NNR?????? 相似文献
215.
S. Zharikov R. E. Mennickent Yu. Shibanov V. Komarova 《Astrophysics and Space Science》2007,308(1-4):545-549
We have obtained the spectrum of a middle-aged PSR B0656+14 in the 4300–9000 Å range with the ESO/VLT/FORS2. Preliminary results show that at 4600–7000 Å the spectrum is almost featureless and flat with a spectral index α ν ??0.2 that undergoes a change to a positive value at longer wavelengths. Combining with available multiwavelength data suggests two wide, red and blue, flux depressions whose frequency ratio is about 2 and which could be the 1st and 2nd harmonics of electron/positron cyclotron absorption formed at magnetic fields ~108 G in upper magnetosphere of the pulsar. 相似文献
216.
217.
The rapidly oscillating Ap (roAp) stars currently represent the only main sequence stars other than the Sun which exhibit non-radial acoustic pulsations of high overtone. This makes them excellent subjects for asteroseismology, an approach which promises to yield accurate knowledge of the interior structures of stars. Of the 27 known roAp stars, 24 were discovered in Sutherland despite extensive searches conducted elsewhere. This paper reviews the discovery of the roAp phenomenon and describes the factors that contribute to the high discovery rate for these stars at Sutherland. Two long-term observational projects in progress at Sutherland are discussed,viz. the Cape roAp Star Survey and long-term monitoring of frequency variations in roAp stars. 相似文献
218.
The BL Lac-type object 3C 66A was observed at the Crimean Astrophysical Observatory during the international project OJ-94.
Observations were made over 10 nights from February through December 2003 at the Cassegrain focus of the 125-cm AZT-11 telescope
with a photopolarimeter capable of simultaneous measurements in the UBVRI bands. In the course of our measurements the brightness
of the object increased by more than 1 magnitude in all these bands. Its color indices varied and the degree of polarization
decreased from ∼16% in February to ∼3% at the end of our observations. In December 2003 a rapid change in the position angle
from 15° to 40° was noticed. The spectral energy distribution Fn is well described by a power law with a spectral index a (Fν ∝ ν
−α
. The increase in brightness was accompanied by a reduction in the spectral index. The most probable mechanism for the observed
changes in the brightness, degree of polarization, and spectral index may be a decrease in the magnetic field strength or
a change in its configuration owing to a increase in the chaotic component of the field.
__________
Translated from Astrofizika, Vol. 49, No. 1, pp. 41–59 (February 2006). 相似文献
219.
Qi-Rong Yuan Peng-Fei Yan Yan-Bin Yang Xu Zhou Department of Physics Nanjing Normal University Nanjing yuanqirong@njnu. edu. cn National Astronomical Observatories Chinese Academy of Sciences Beijing Department of Mathematics Physics Qingdao University of Science Technology Qingdao 《中国天文和天体物理学报》2005,5(2):126-136
Convincing evidence for a past interaction between the two rich clusters A399 and A401 was recently found in the X-ray imaging observations. We examine the structure and dynamics of this pair of galaxy clusters. A mixture-modeling algorithm was applied to obtain a robust partition into two clusters, which allowed us to discuss the virial mass and velocity distribution of each cluster. Assuming that these two clusters follow a linear orbit and they have once experienced a close encounter, we model the binary cluster as a two-body system. As a result, four gravitationally bound solutions are obtained. The recent X-ray observations seem to favor a scenario in which the two clusters with a true separation of 5.4h-1 Mpc are currently expanding at 583 km s-1 along a direction with a projection angle of 67.5°, and they will reach a maximum extent of 5.65 h-1 Mpc in about 1.0 h-1 Gyr. 相似文献
220.