Superior conjunction of pioneer 6

Spectrograms of the radio signals from Pioneer 6 were taken as the spacecraft was occulted by the sun. The spectral bandwidths increased slowly at first, then very rapidly at 1 degree from the sun. In addition, six solar "events" produced marked increases of bandwidth lasting for several hours. The received signal power seemed unaffected by the solar corona.     

Torsional oscillations of the sun

The sun's differential rotation has a cyclic pattern of change that is tightly correlated with the sunspot, or magnetic activity, cycle. This pattern can be described as a torsional oscillation, in which the solar rotation is periodically sped up or slowed down in certain zones of latitude while elsewhere the rotation remains essentially steady. The zones of anomalous rotation move on the sun in wavelike fashion, keeping pace with and flanking the zones of magnetic activity. It is uncertain whether this torsional oscillation is a globally coherent ringing of the sun or whether it is a local pattern caused by and causing local changes in the magnetic fields. In either case, it may be an important link in the connection between the rotation and the cycle that is widely believed to exist but is not yet understood.     

Anomalous solar rotation in the early 17th century

The character of solar rotation has been examined for two periods in the early 17th century for which detailed sunspot drawings are available: A.D. 1625 through 1626 and 1642 through 1644. The first period occurred 20 years before the start of the Maunder sunspot minimum, 1645 through 1715; the second occurred just at its commencement. Solar rotation in the earlier period was much like that of today. In the later period, the equatorial velocity of the sun was faster by 3 to 5 percent and the differential rotation was enhanced by a factor of 3. The equatorial acceleration with declining solar activity is in the same sense as that found in recent Doppler data. It seems likely that the change in rotation of the solar surface between 1625 and 1645 was associated with the onset of the Maunder Minimum.     

Active polar region on the nucleus of comet halley

The images of the nucleus of comet Halley returned by the Giotto spacecraft reveal a number of active regions on the surface, one of which is near the expected location of the rotation pole. This feature is larger and brighter than other source regions, suggesting that the mechanism that drives this source is also different. At this active region near the rotation pole, the sun was circumpolar for a significant portion of the solar encounter. Continuous insolation heated the nucleus to greater depths than in other areas, producing the broad, active polar region.     

Solar differential rotation and oblateness

An investigation of the time development of differential rotation produced by the solar wind torque indicates that the sun has a rapidly rotating core.     

Seismic images of the far side of the Sun

Images of an active region on the far side of the sun were derived by applying seismic holography to recent helioseismic observations from space. Active regions are the centers of energetic phenomena such as solar flares and coronal mass ejections, whose resulting electromagnetic and particle radiation interfere with telecommunications and power transmissions on Earth and can pose significant hazards to astronauts and spacecraft. Synoptic seismic imaging of far-side solar activity will now allow anticipation of the appearance of large active regions more than a week ahead of their arrival on the east solar limb.     

Stellar Activity and Brightness Variations: A Glimpse at the Sun's History

Radiometric measurements during the past decade from the Solar Maximum Mission and Nimbus 7 satellites have shown that the total solar irradiance varies in step with the sun's 11-year magnetic activity cycle. Stellar observations from the Lowell and Mount Wilson observatories now confirm and elaborate this discovery. These measurements show that older stars similar to the sun tend to become brighter as their magnetic activity level increases, just as the sun does during its 11-year activity cycle. Younger stars, however, tend to become fainter as their magnetic activity level increases. This contrasting behavior suggests that the balance between the competing phenomena that influence solar brightness variability has shifted during the sun's lifetime.     

Turbulent dynamics in the solar convection zone

Observations of the sun reveal highly complex flows and magnetic structures that must result from turbulent convection in the solar envelope. A remarkable degree of large-scale coherence emerges from the small-scale turbulent dynamics, as seen in the cycles of magnetic activity and in the differential rotation profile of this star. High-performance computing now permits numerical simulations of compressible turbulence and magnetohydrodynamics with sufficient resolution to show that compact structures of vorticity and magnetic fields can coexist with larger scales. Such structured turbulence is yielding transport properties for heat and angular momentum at considerable variance with earlier models. These simulations are elucidating the coupling of turbulent fluid motions with rotation and magnetic fields, which must control the interlinked differential rotation and magnetic dynamo action.     

太阳系天体相对地球某点的波动式螺线运动(Ⅰ)——太阳、月球相对地球某点螺线运动方程推导及模拟分析

为研究太阳系天体相对地球某点的运动规律,首先建立了地心黄道坐标系,并将太阳绕地球的圆周运动转换为太阳绕地心的余弦波动,同时将此余弦波动作为标准余弦曲线.将太阳绕地球的运动分解为波动和"自转",并分双波动坐标轴和波动-螺面坐标轴分析,推导出太阳对地球赤道某点的波动式螺线运动轨迹方程,同时进行计算机模拟与分析,得到了太阳对地球某纬度某点的波动式螺线运动轨迹方程.以此类推,推导出月球对地球某点的波动式螺线运动轨迹方程,并分别进行计算机模拟与分析.结果表明,太阳、月球相对于地球某点的运动轨迹为与幅值与角度相关的波     

Rapid rotation of the solar interior

A model proposed for the sun apparently can account for the maintenance of photospheric rotation against deceleration by the solar wind. The rotational period is about half a day near the top of the radiative mass, and 1.6 times shorter at the center.     

Seismology of the sun

Oscillations of the sun make it possible to probe the inside of a star. The frequencies of the oscillations have already provided measures of the sound speed and the rate of rotation throughout much of the solar interior. These quantities are important for understanding the dynamics of the magnetic cycle and have a bearing on testing general relativity by planetary precession. The oscillation frequencies yield a helium abundance that is consistent with cosmology, but they reinforce the severity of the neutrino problem. They should soon provide an important standard by which to calibrate the theory of stellar evolution.     

Dynamic variations at the base of the solar convection zone

We have detected changes in the rotation of the sun near the base of its convective envelope, including a prominent variation with a period of 1.3 years at low latitudes. Such helioseismic probing of the deep solar interior has been enabled by nearly continuous observation of its oscillation modes with two complementary experiments. Inversion of the global-mode frequency splittings reveals that the largest temporal changes in the angular velocity Omega are of the order of 6 nanohertz and occur above and below the tachocline that separates the sun's differentially rotating convection zone (outer 30% by radius) from the nearly uniformly rotating deeper radiative interior beneath. Such changes are most pronounced near the equator and at high latitudes and are a substantial fraction of the average 30-nanohertz difference in Omega with radius across the tachocline at the equator. The results indicate variations of rotation close to the presumed site of the solar dynamo, which may generate the 22-year cycles of magnetic activity.     

基于AT89S52的智能型双精度太阳自动跟踪系统设计

为提高太阳能的利用率,以AT89S52单片机为控制核心,采取极轴式跟踪方式,设计了一套以视日运动轨迹跟踪为主、光电跟踪进行跟踪校正的智能型双精度太阳跟踪系统,该系统通过采集时钟芯片信息计算当前太阳位置,实现视日运动轨迹跟踪;同时利用光电传感器采集的光强偏差控制步进电机,实现光电跟踪,校正轨迹偏差,保证聚光板与太阳光相垂直。试验表明,该太阳跟踪系统能在不同天气状况下对太阳进行较准确跟踪,能量接收效率提高20%以上,达到了充分利用太阳能的目的。     

Galileo ultraviolet spectrometer experiment: initial venus and interplanetary cruise results

The Galileo Extreme Ultraviolet Spectrometer obtained a spectrum of Venus atmospheric emissions in the 55.0- to 125.0-nanometer (nm) wavelength region. Emissions of helium (58.4 nm), ionized atomic oxygen (83.4 nm), and atomic hydrogen (121.6 nm), as well as a blended spectral feature of atomic hydrogen (Lyman-beta) and atomic oxygen (102.5 nm), were observed at 3.5-nm resolution. During the Galileo spacecraft cruise from Venus to Earth, Lyman-alpha emission from solar system atomic hydrogen (121.6 nm) was measured. The dominant source of the Lyman-alpha emission is atomic hydrogen from the interstellar medium. A model of Galileo observations at solar maximum indicates a decrease in the solar Lyman-alpha flux near the solar poles. A strong day-to-day variation also occurs with the 27-day periodicity of the rotation of the sun.     

GONG Observations of Solar Surface Flows

Doppler velocity observations obtained by the Global Oscillation Network Group (GONG) instruments directly measure the nearly steady flows in the solar photosphere. The sun's differential rotation is accurately determined from single observations. The rotation profile with respect to latitude agrees well with previous measures, but it also shows a slight north-south asymmetry. Rotation profiles averaged over 27-day rotations of the sun reveal the torsional oscillation signal-weak, jetlike features, with amplitudes of 5 meters per second, that are associated with the sunspot latitude activity belts. A meridional circulation with a poleward flow of about 20 meters per second is also evident. Several characteristics of the surface flows suggest the presence of large convection cells.     

Solar-Like M-Class X-ray Flares on Proxima Centauri Observed by the ASCA Satellite

Because of instrumental sensitivity limits and stellar distances, the types of x-ray flares observable on stars have been intrinsically much more energetic than those on the sun. Such enormous events are a useful extrapolation of the solar phenomenon if the underlying assumption is correct that they form a continuous sequence involving similar physical processes as on the sun. The Advanced Satellite for Cosmology and Astrophysics (ASCA), with its greater sensitivity and high-energy response, is now able to test this hypothesis. Direct comparison with solar flares measured by the x-ray-monitoring Geostationary Operational Environmental Satellites (GOES) is possible. The detection of flares on Proxima Centauri that correspond to GOES M-class events on the sun are reported.     

海口市太阳总辐射变化特征及其与气候因子的关系

利用海口地面站1971-2008年太阳总辐射和气象资料,对海口市太阳总辐射特征进行分析,结果表明：1971-2008年海口太阳总辐射以-248．467MJ／m^2·a的速度减少,月变化与年变化趋势一致。低云量、水汽压是影响其太阳总辐射的主要气候因子。太阳总辐射与气温关系达到置信度为0．001的极显著水平。     

农村被动式太阳房动态能耗数值模拟与优化研究

对采用附加阳光间的天津某农村被动式太阳房围护结构的全年动态能耗及附加阳光间的全年太阳得热量进行了数值模拟,并比较分析了采用附加阳光间前后该住宅的全年围护结构能耗。同时,利用数值模拟手段,对采用了保温材料的墙体和Low-E玻璃的阳光间的全年动态能耗进行了模拟,并与未采用保温材料和Low-E玻璃的情况进行了对比分析。结果表明采用Low-E玻璃的附加阳光间能耗降低了80%,采用保温材料的围护结构墙体能耗降低了43.5%。通过经济效益比对分析,采用保温材料和Low-E玻璃增加的投资约97 396元,约5年内即可收回。     

太阳系天体相对地球某点的波动式螺线运动(Ⅱ)——太阳系七大行星相对地球某点的螺线运动方程推导及模拟分析

为研究太阳系天体相对地球某点的运动规律,在太阳系天体相对地球某点的波动式螺线运动(I)中推导出太阳和月球对地球赤道某点和纬度某点的波动式螺线运动轨迹方程,并进行了计算机模拟与分析的基础上,推导出太阳系七大行星对地球赤道某点和纬度某点的波动式螺线运动轨迹方程,并分别进行了计算机模拟与分析.结果表明,太阳系七大行星相对于地球某点的运动轨迹为与幅值与角度相关的波动式螺线,向x轴方向等速传播,并且在两种坐标轴下的运动规律与太阳、月亮类似.并且:1在双波动坐标轴下分析,水星运动轨迹在yz平面上的投影出现重波;2金星运动轨迹在yz平面上的投影疏密度与其余星球相反;3在波动-螺面坐标轴下分析,天王星和海王星螺线与太阳的最相近.     

Solar constant: constraints on possible variations derived from solar diameter measurements

Climatically significant variation of the solar constant (the energy output of the sun) implies measurable change in the solar radius. The available data limit variations of the solar radius between 1850 and 1937 to about 0.25 arc second; modeling of the sun indicates that the solar constant did not vary by more than 0.3 percent during that time.