共查询到20条相似文献，搜索用时 31 毫秒
1.
This paper is devoted to an analysis of brightness temperatures of the polar and low-latitude coronal holes on the Sun in the cm-wave range during periods of minimum solar activity. Data from observations of the polar coronal hole received by the RATAN-600 radio telescope during the solar eclipse of March 29, 2006, and low-latitude observations of coronal holes and quiet Sun received earlier with the RATAN-600 and BPR radio telescopes in the period of minimum solar activity have been used in the paper. The obtained good agreement between the brightness temperatures of cm-wave emission of the polar coronal hole above the North Pole of the Sun and of the low-latitude coronal holes against the background of the quiet Sun reveals the identity of the temperature properties of large coronal holes, irrespective of the mode of their arrangement and location on the Sun during the periods of minimum solar activity. 相似文献
2.
A. A. Melkumyan A. V. Belov M. A. Abunina A. A. Abunin E. A. Eroshenko V. A. Oleneva V. G. Yanke 《Geomagnetism and Aeronomy》2018,58(2):154-168
The IZMIRAN database of Forbush effects and interplanetary disturbances was used to study features of the action of high-speed solar wind streams from coronal holes on cosmic rays. Three hundred and fifty Forbush effects created by coronal holes without other actions were distinguished. The mean values and distributions have been found for different characteristics of events from this group and compared with all Forbush effects and Forbush effects caused by coronal ejections. Despite the great differences in high-speed streams from coronal holes, this group turned out to be more compact and uniform as compared to events related to coronal ejections. Regression dependences and correlation relations between different parameters of events for the studied groups have been obtained. It has been shown that Forbush effects caused by coronal ejections depend considerably more strongly on the characteristics of interplanetary disturbances as compared to Forbush effects related to coronal holes. This suggests a significant difference between the modulation mechanisms of Forbush effects of different types and corroborates earlier conclusions based on indirect data. 相似文献
3.
E. V. Ivanov 《Geomagnetism and Aeronomy》2012,52(8):981-986
This paper investigates the relationship between cyclic variations in the velocity of coronal mass ejections and cyclic changes in the structure of the large-scale solar magnetic field (LSSMF) in solar cycle 23, using the effective solar multipole index as a parameter of the characteristic dimensions of LSSMF structural elements. Cyclic variations in the velocity and frequency of coronal mass ejections are found to resemble cyclic changes in the effective solar multipole index. It is suggested that cyclic changes in the maximum velocity of coronal mass ejections are associated with different conditions for the formation of complexes of active regions connected by coronal arch structures, the energy of which is the main source of energy (velocity) for coronal mass ejections. The study leads to some suggestions about the possible site of initiation of coronal mass ejections. 相似文献
4.
The spectra of the coronal hole radio emission in solar cycles 23 and 24 have been studied based on RATAN-600 data in the 4–16.5 GHz range at frequencies of 5.7 and 17 GHz and 327 MHz. It has been found that bright features of coronal hole microwave emission at 17 GHz and dark features at 5.7 GHz can exist in coronal holes when the spectral index is 1.25–1.5 in the 6.5–16.5 GHz range; the radio spectrum in this range is flat when coronal holes are indiscernible against the background of a quiet Sun. The possible vertical scale of the solar atmosphere over coronal holes is discussed. 相似文献
5.
本文从三个方面探讨了副鼻窦直接冠状扫描影像:(1)检查前病人的准备;(2)CT 技术;(3)数据显示。最佳 CT 技术主要包括采用俯卧位对副鼻窦前部以3mm 层厚薄层扫描,它可使得窦口鼻道综合体得以最佳显示,余部采用5mm 层厚扫描。扫描角度无意义。 相似文献
6.
A new analytical model of a fine singular 3D coronal loop is developed. The loop is a thin curved magnetic flux tube immersed in the potential magnetic arcade. The ambient corona is given by the hydrostatic model of a quiet solar atmosphere (Avrett and Loeser, 2008). The proposed 3D model of a fine coronal loop reproduces well the observed physical properties of coronal structures of this kind. 相似文献
7.
I. A. Bilenko 《Geomagnetism and Aeronomy》2012,52(8):1005-1014
This paper investigates the dependence of the observed coronal mass ejections and their parameters on evolutionary changes in the global solar magnetic field at different phases of solar cycles 23?C24. Four periods in the evolution of the solar cycle are identified, depending on the dominance ratio of the sectoral and zonal magnetic field structures. The parameters of coronal mass ejections observed during these periods are analyzed. The evolving structure in the global magnetic field is identified, and its influence on coronal mass ejections is examined. 相似文献
8.
Melkumyan A. A. Belov A. V. Abunina M. A. Abunin A. A. Eroshenko E. A. Oleneva V. A. Yanke V. G. 《Geomagnetism and Aeronomy》2020,60(5):521-529
Geomagnetism and Aeronomy - Forbush decreases of cosmic rays are caused by two types of solar sources: coronal holes and coronal mass ejections. In some cases, the identification of the solar... 相似文献
9.
环枢椎冠状CT扫描因其受到人体结构及设备的制约，技术难度较大，故很少有单位开展此项检查。我院影像科与北医三院脊柱外科协作，为了临床的需要，解决环枢椎外伤及术前术后的诊断问题，我们对环枢椎的直接冠状CT扫描进行了尝试。结果令人满意，达到了临床的诊断要求。 相似文献
10.
The interrelation between the density inhomogeneity and the magnetic field configuration in the solar corona has been studied. The situation of consistency with the regular cellular magnetic field organization, established by the authors based on polarization data, and helmet-shaped coronal structures has been analyzed. Consistency was found when coronal helmets appeared as projections on the plane of the sky of dense layer folds. It turned out that a dense layer on a regularly deformed neutral surface on a scale of 60° generates coronal shapes typical of solar activity minimum epochs. Threby, a weighty argument for the Molodenskii hypothesis that a dense layer is formed on the neutral surface has been obtained and it has been determined that one can find the 3D geometry of the coronal neutral surface based on modeling the visible shape of coronal helmets. The study of this geometry based on the observed coronal structures in the epoch of minimum and low solar activity indicated that the neutral surface longitudinal deformation scale remains stable and the surface latitudinal amplitude at the corona base reaches 50°–70° latitudes and tends to increase with increasing solar activity. This amplitude decreases as a power function with a variable index close to ?1 with increasing distance from the Sun. In addition, a 10° small-scale deformation of the studied surface with a predominant latitudinal flexure direction has been revealed. 相似文献
11.
The problem of the observed fast damping of longitudinal waves in solar coronal magnetic loops is studied. According to some data, the radiation effect, which plays a key role in the cooling of coronal loops that are observed in the extreme UV wavelength range, is used to explain this phenomenon. The dispersion relation for slow magnetosonic modes of a cylindrical magnetic tube has been obtained with regard to the radiation effect. It has been indicated that the radiation actually results in the fast damping of the slow magnetosonic modes of coronal magnetic loops. 相似文献
12.
Short-lived plasma jets of various scales, from giant X-ray jets more than 300 Mm in extent to numerous small jets with sizes
typical of macrospicules, are the phenomena observed in the solar corona in extreme ultraviolet and X-ray emission. Small
jets are particularly prominent in polar coronal holes. They are close neighbors of tiny bright loops and coincide in time
with their sudden brightening and increase in size. The geometric shape of the jets and their location suggest that they arise
near singular null points of the coronal magnetic field. These points appear in coronal holes due to the emergence of small
bipolar or unipolar magnetic structures within large-scale unipolar cells. Polar jets show a distinct vertical plasma motion
in a coronal hole that introduces significant momentum and mass into the solar wind flow. Investigating the dynamics of polar
jets can elucidate certain details in the problem of fast solar wind acceleration. 相似文献
13.
Correlation between the parameters of coronal mass ejections (CMEs) that are detected on the LASCO coronographs and are associated
with eruptive prominences and the distances of CME axes from the coronal streamer belt has been analyzed. The deviations of
CME trajectories from the radial direction have been investigated. 相似文献
14.
Summary Using a more detailed geomagnetic activity Kp index, the finding in [3] that geomagnetic activity increases after the CMP of coronal holes, was verified; it was shown using individual activity patterns, that coronal holes apparently do not form a homogeneous class of phenomena, which must be respect in considerations of emissions of fast solar wind streams. 相似文献
15.
Abstract A class of exact solutions to the steady, two-dimensional magnetohydrodynamic equations ina cylindrical geometry is presented. These may model both closed and open magnetic structures found in the solar atmosphere. For closed structures, it is found that increasing the flow speed causes the summit of the arcade of closed magnetic fieldlines to rise. Parameter ranges also exist where the solution has regions of open and closed field, and so the solutions may be relevant for modelling flows in solar magnetic structures such as coronal streamers, X-ray bright points coronal plumes and coronal holes. 相似文献
16.
对1970-1980年1AU附近太阳风的观测资料所进行的分析表明,60％的冕旒相关流和40％的CME相关云的流速都不大于350km/s;80％的流速不大于350km/s的低速风起源于冕旒,且除冕旒和CMEs外,看来还存在别的低速风日冕源区.有关冷风的分析表明,近80％的冷风的流速不大于350km/s,80％的冷风起源于冕旒;也有一小部分冷风既非起源于冕旒,也不起源于CMEs.低速风的11年变化显示,在太阳活动各位相,冕旒总是低速风的主要日冕源区.但是,极大位相时的冕旒宽度很可能大于极小和下降位相. 相似文献
17.
We study the annual frequency of occurrence of intense geomagnetic storms (Dst < –100 nT) throughout the solar activity cycle for the last three cycles and find that it shows different structures. In cycles 20 and 22 it peaks during the ascending phase, near sunspot maximum. During cycle 21, however, there is one peak in the ascending phase and a second, higher, peak in the descending phase separated by a minimum of storm occurrence during 1980, the sunspot maximum. We compare the solar cycle distribution of storms with the corresponding evolution of coronal mass ejections and flares. We find that, as the frequency of occurrence of coronal mass ejections seems to follow very closely the evolution of the sunspot number, it does not reproduce the storm profiles. The temporal distribution of flares varies from that of sunspots and is more in agreement with the distribution of intense geomagnetic storms, but flares show a maximum at every sunspot maximum and cannot then explain the small number of intense storms in 1980. In a previous study we demonstrated that, in most cases, the occurrence of intense geomagnetic storms is associated with a flaring event in an active region located near a coronal hole. In this work we study the spatial relationship between active regions and coronal holes for solar cycles 21 and 22 and find that it also shows different temporal evolution in each cycle in accordance with the occurrence of strong geomagnetic storms; although there were many active regions during 1980, most of the time they were far from coronal holes. We analyse in detail the situation for the intense geomagnetic storms in 1980 and show that, in every case, they were associated with a flare in one of the few active regions adjacent to a coronal hole. 相似文献
18.
Geomagnetic disturbances in the Canadian region are compared with their solar and heliospheric sources during the decline phase of solar activity, when recurrent solar wind streams from low-latitude coronal holes were clearly defined. A linear correlation analysis has been performed using the following data: the daily and hourly indices of geomagnetic activity, solar wind velocity, and coronal hole area. The obtained correlation coefficients were rather low between the coronal hole areas and geomagnetic activity (0.17–0.48), intermediate between the coronal hole areas and the solar wind velocity (0.40–0.65), and rather high between the solar wind velocity and geomagnetic activity (0.50–0.70). It has been indicated that the correlation coefficient values can be considerably increased (by tens of percent in the first case and about twice in the second case) if variations in the studied parameters related to changes in the ionosphere (different illumination during a year) and variations in the heliolatitudinal shift of the coordinate system between the Earth, the Sun, and a spacecraft are more accurately taken into account. 相似文献
19.
本文研究了头部冠状位ＣＴ可调角度扫描架的制做和应用。为了解决临床工作中头部冠状位ＣＴ扫描技术中存在的摆位困难，病人体位不舒适而移动所产生的定位不准确、图像不清晰、伪影等问题，着重介绍头部冠状位ＣＴ可调角度扫描架的固定作用和可调角度的研究． 相似文献
20.
I. A. Bilenko 《Geomagnetism and Aeronomy》2017,57(8):952-963
Statistical studies of coronal mass ejections (CMEs) and coronal holes (CHs) are reviewed. The work summarizes the historical and current results of statistical studies of CMEs and CHs and their parameters that have been obtained by various authors who considered these phenomena as independent manifestations of solar activity, as well as their mutual effect on geomagnetic activity, based on both ground and space observations. 相似文献