共查询到20条相似文献，搜索用时 15 毫秒
1.
《天文研究与技术》1990,(4)
Using the Solar Magnetic Field Telescope of Huairou Solar Station,we observed theflare loop occuring on the west limb of the sun on Aug.17,1989.The loops were causedby AR5629(S17,L74).At that time,this active region had already gone to the back ofthe sun,about 10°.From UT0132 to UT0911,we got the data of the flare images 相似文献
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《中国天文和天体物理学报》1982,(2)
We put forth three modes of black hole formation, i.e. (1) A black hole kern forms initially inside the collapsing star. (2) The different mass shells of the collapsing star fulfils the Schwarzschild condition simultaneously. (3) Only the outmost mass shell of the collapsing star fulfils the Schwarzschild condition. We then calculate the entropy of the collapsing star for modes (1) and (3) and find that they are only 10-19 times the entropy of black hole. Modes (1) may be occure during the supernova explosions or galaxy explosions. Mode (3) may be occur in the formation of galactic black hole. 相似文献
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《天文研究与技术》1990,(4)
Using the 18 cm Hα-Photoheliograph at Yunnan Observatory,we obtained theAR5629(S17,L75)data.The AR existed at the southern hemisphere of solar disk duringthe days from Aug.4 to 16.Except Aug.16th when the AR partly moved away from thedisk,sunspot group type was HRX,the AR kept its complex type in McIntoshclassfication on the other 12 days and there were 8 days,spot group areas over 1,000 相似文献
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Measurements of linear polarization in hydrogen H and H lines, made with the Large Solar Vacuum Telescope of Baikal Astrophysical Observatory and Automated Solar Telescope of Sayan Solar Observatory, affiliated with the Russian Institute of Solar and Terrestrial Physics, are reported in this paper. Short-term polarization associated with solar flares is found to be present in active regions. There is a significant tendency for the H polarization vector to be radial, i.e., in the flare-to-disk-center direction. This polarization may be due to atmospheric bombardment by hecta keV protons. On the other hand, the polarization vector is found to be perpendicular to the radial direction at some locations where the line profile has a typical mustache shape suggesting a bombardment by energetic electrons. The H line is also linearly polarized. However, no preferential direction of polarization is found in this line, which is formed more deeply in the solar atmosphere. 相似文献
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Fine structure of brightness inhomogeneities with I r.m.s. = 2.9% was discovered on the extreme limb of the Sun on the best quality white-light photographs obtained at the Soviet Stratospheric Solar Observatory. The concept is that temperature inhomogeneities are responsible for the limb structure. The real value T r.m.s. = 109K is required to explain our observations. Another possible explanation is that small-scale magnetic flux tubes with the realistic filling factor f* = 1% are the source of the limb brightness fluctuations. 相似文献
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《天文研究与技术》1990,(4)
The research on‘Rapid Fluctuation in Solar Flares’is paid great attention becauseof its important position in the solar flare physics,and it is also one of the importantparts in the project“22 MAX GLOBAL CHARACTER RESEARCH OFSOLAR—TERRESTRIAL SYSTEM”.The Solar Radio High Time Resolution 相似文献
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This paper determines what should be the difference between the colour of the solar disc centre and the integrated light of the corona at different heights. We define the colour as the ratio of the spectral intensity at = 640 nm and = 490 nm. The optical radiation of the corona is assumed to be caused by a contribution of photospheric light scattered on free electrons in K-corona and by a contribution of the photospheric light scattered on solid dust particles in F-corona. The limb-darkening law was taken from Pierce and Slaughter (1977). The distribution of electron density and brightness of the F-corona was taken from van de Hulst (1950). We indicate that the solar corona should be already close to the limb, more reddish than the centre of the solar disc, where reddening increases with the height due to the increase of the contribution of the F-corona. 相似文献
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The excitation equilibrium of Fexxv in the solar corona for electron power distributions is presented. A parametric form of the distribution function is used to demonstrate the changes in the excitation equilibrium due to the shape of the distribution. A pseudo-temperature is used for better understanding of the changes in the excitation equilibrium. The Fexxv line intensities depend on the shape of the electron distribution and unusual Fe line ratios can be observed for non-thermal distribution. The results can be used in specific applications in the solar corona, especially in diagnostics of the impulsive phase of solar flares, where the deviations from the Maxwellian distribution can be large. 相似文献
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《天文研究与技术》1990,(4)
The fast rotation of sunspot group 5395 ( first, it exhibited inverse clockwise rotation, then clockwise rotation, the rotative angle was the lagrest 1-2 days before proton flare.) the stronger emission of SVC and the spectral maximun (near 8800MHz) of both the SVC and peak fluxes of the bursts et al are close correlated with occurrence of proton flares. Flares often generated in the regions of emerging or disappearing of new magnetic flux with opposite polarity, of the faster and more complex variation of the gradient and configuration of magnetic field, and of the neck and tail of magnetic gulf. 相似文献
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《天文研究与技术》1990,(4)
1 Introduction In the 1970s, it had been known that two kinds of flares may be existed. One isthe "Compact flare", in EUV and X-ray, it is appeared as static brightenning coronalloop arches preexisted in lower level. Another kind of flare is the "two-ribbon flare", it isinitiated from the collapse of filament and characterized by the continued increasing of 相似文献
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《天文研究与技术》1990,(4)
In Order to study the Global Characteristics of Solar-terrestrial System in the 22th Solar Cycle, our Institute has built up a few geomagnetic observatories recently years at Mohe, Beijing (Ming Toms), Sanya (Hainan Insland) in the torritorg of China. These stations together with some old stations close to 120° E meridian and form the East Asia Meridian Chain of Geomagnetic Observatories. In the meantime we were set up also a observatory of the Chinese Great Wall Station in Antarctica. According to theather character of different area we designed and built the house with different structural style.The magnetic recording house is the under ground in Mohe, the semi-under ground in Beijing, the ground in sanya of China.The recording and the absolute houses are all built on stilts in the Chinese Great Wall Station of Antarctica. All buildins are made of non magnetic materials, Such as limestone, sun-dried mud brick, wood, copper and Aluminum etc.Therefore there are not affects of the magnetic materiat arou 相似文献
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《紫金山天文台台刊》1998,(2)
On the basis of photogravitational theory, the influence of solar photogravitation on the motion of comet tail is discussed in this paper. It is shown that for plasma tail and some of the dust tail, there are two coplaner libration points L6, L7, and three collinear points L21, L22,L3 at most. The regions in which the dust grain of comet tail can move are also obtained. 相似文献
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《天文研究与技术》1990,(4)
It has been found for a long time, with analysing the variation of the relative number of sunspot, that there exist the periodicity of 11 years in solar activity. With the deepening research of the varied solar active phenomena, a series of periodicities with different periods have been also found in solar activity. For example, there is the periodicity of about 80 days for the occurrence, rate of proton flares for solar activity cycles 19 and 20 found by Ai and Fan ci:i at 1974. Recently a periodicity of about 152 days of the occurrence rate of solar flares has been proposed by some authors. a3'5>7:i The existence of this periodicity hsa been proved in the various solar flares. In this paper using the data of solar microwave bursts from January 1986 to December 1988, a Fourier analysis of the occurrence rate of solar microwave bursts has been made. There was no periodicity for the occurrence rate of solar microwave bursts of about 152 days found. This is a new result for solar cycle 22 in the first thr 相似文献
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《天文研究与技术》1990,(4)
The solar-terrestrial sciences studies not only the processes in the regions ofsolar-terrestrial system such as the solar convection region and atmosphere, theinterplanetary space, the earth megnetosphere and ionosphere, the earth atmosphere andsurface, but emphasyzes the coupling processes between the regions, that is the globalcharacters of the solar-terrestrial system. There are important progresses of solar-terres- 相似文献
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《中国天文和天体物理学报》1982,(3)
These two grand gatherhags were attended by 147 representatives of more than 40 unitswhich are of astronomical observatories,stations,factories,planetarium,research institutes,universities,colleges and military departments concerned etc.Among the representatives,thereare the senior astronomers who have made significant contributions to the development ofChinese astronomy,the backbone of astronomica research of middle age who are in their prime 相似文献