Quasistationary outflow of gases from solar active regions

The author's finding that active regions are sources of relatively slow and approximately radial quasistationary corpuscular streams is confirmed by using the fact that active regions are closely connected with coronal holes. Furthermore, attention is paid to numerous papers according to which the active regions characterized by enhanced and prolonged chromospheric (flare) activity are also sources of quasistationary corpuscular streams. Velocities of gases in these streams are higher than velocities of gases in streams from “quiet” active regions.On the basis of all these studies it is suggested that the origin of outflow of plasma from “quiet” active regions and from active regions with enhanced flare activity is the same and is due to some continuous non-stationary processes in the active regions. The velocity of gases in all these streams grows with increasing continuous flare activity in the active regions.It is concluded that quasistationary corpuscular streams from active regions with enhanced flare activity are important sources of cosmic rays from the sun.     

The radial velocity of the sun as a star and the solar cycle

Radial velocity measurements of the sun as a star using a resonant scattering spectrometer have been obtained at Izaña (Tenerife) during long observing seasons from 1976 to 1985. Its analysis shows that except for the global oscillations with periods shorter than one day there are stable signals with longer periods: at ∼13 days with mean amplitude of ∼ 3 m/s (it changes with the solar cycle) and another one of ∼ 15 m/s amplitude which shows a temporal variation of various years related to the solar cycle. The first signal has a partial explanation as an effect produced by the passage of active regions through the visible surface of the sun but it does not completely explain the observed signal. The second one, related to the limb shift, is probably due to changes in the convection zone in connection with the solar cycle.     

New ultra-violet filtergrams and results from the transition region camera rocket experiment

The rocket-borne solar ultra-violet telescope named Transition Region Camera (T.R.C.) was launched successfully for the fourth time on 25th october 1985. Calibrated photographic images of the sun were obtained at Lyman alpha and in two adjacent bands at 156 nm and 169 nm. The angular resolution achieved was equivalent to 0.7 arcsec. Fine structures in Lyman alpha were observed in the network and above supergranular cells. From the 156 nm filtergram (including a strong C IV contribution) and the 169 nm filtergram, we study the differential contribution of the C IV lines and of the continuum emission, from the quiet sun, an active region and at the limb.     

Solar radio emissions

In this paper, we present a tutorial review which was presented at the first Advanced School on Space Environment (ASSE 2004). We first describe the basics of radioastronomy definitions, and discuss radiation processes relevant to solar radio emissions like plasma emission, free–free bremsstrählung and gyromagnetic emissions. We illustrate these fundamentals by describing recent solar radio observations and the constraints they bring on different solar physical parameters. We focus on solar radio emissions from the quiet sun, active regions and during explosive events known as solar flares, and how the latter can bring quantitative informations on the particles responsible for the emission. Finally, particular attention is paid to new radio diagnostics obtained at very high frequencies in the millimeter/submillimeter range, as well as to radio emissions relevant to Space Weather studies.     

Evolution of the solar corona from solar maximum to minimum

A study on solar coronal activities related to the 11-year activity cycle is presented from the Yohkoh soft X-ray observations. Yohkoh was launched in August 1991, just after the solar maximum of the cycle 22 and continues to observe the Sun in the declining phase of the magnetic activity cycle toward the solar minimum. The soft X-ray flux from the whole Sun in the declining phase essentially decreases with the size of active regions. The X-ray intensity in quiet regions in the declining phase decreases with the magnetic flux observed at the photosphere. The whole-Sun soft X-ray flux does not monotonically decrease, but there are periodic enhancements of the flux with about a one-year interval. The activity appears as bright clusters in the butterfly diagram of the soft X-ray intensity and corresponds to the emergence of complexes of activity in the sunspot zones. The high-latitude activity is also studied, and we find that the X-ray intensity of high-latitude regions fluctuates with time scale of about one year.     

The structure of the solar corona as observed by the Solar Extreme ultraviolet Rocket Telescope and Spectrograph

Data from the Solar Extreme-ultraviolet Rocket Telescope and Spectrograph (SERTS) have been used to address a number of important scientific problems. The primary strength of the SERTS data is the fact that this spectral range is rich with emission lines. Over 270 lines are seen in the SERTS active Sun spectrum, from 57 different ions. For example, multiple (≥4) lines are observed for all ionization states of iron from Fe IX to Fe XVII. Temperatures and densities have been derived for a number of active and quiet Sun regions, the coronal magnetic field strength has been estimated for both a plage region and an active region.     

CME影响下L1点附近等离子体及共生微波爆发的射电辐射机制研究

CME在产生和发展过程中与日冕和行星际介质相互作用并发出不同波长的射电辐射．在研究了无CME时空间等离子体的各种辐射机制基础上,统计分析了1999年2月至1999年8月期间有较大的CME发生情况下,在CME影响下L1拉格朗日点附近等离子体参数发生变化后的射电辐射机制．分析结果表明,其射电辐射机制主要是轫致辐射、微量的回旋辐射和更加微弱的复合辐射．此外,分析讨论了1999年2月至1999年8月期间与CME共生的太阳微波爆发．分析结果表明,与CME共生的是微波逐渐型爆发、尖峰爆发,其辐射机制主要是轫致辐射、回旋共振辐射、等离子体辐射及电子回旋脉泽辐射．     

基于活动区面积统计的F10.7指数预报方法

太阳10.7cm射电流量（F_10.7）是反映太阳整体活动的重要指标,其主要源头是日面活动区.F_10.7指数与日面活动区具有显著的相关性,且不同面积的活动区与F_10.7并不遵循相同的线性关系.为进一步提高F_10.7预报的准确性,利用日面活动区面积与F_10.7的相关性,依据面积大小分类,提出F_10.7的预报公式并进行验证.采用2008-2018年SWPC （Space Weather Prediction Center）公布的活动区面积数据和CSWFC （Canadan Space Weather Forecast Center）公布的F_10.7实测数据计算预报公式系数,利用高年（2003年）和低年（1997年）的F_10.7预报验证其结果.研究结果表明,预报结果与实测值的相关系数分别为0.9318和0.9295,二者皆优于SWPC同时期的预报结果（相关系数分别为0.9186和0.8771）.本研究首次基于活动区的变化预测了F_10.7,提高了F_10.7预测的准确性.      

The variability of the sun's ultraviolet radiation

The intensity of continua and emission lines which form the solar UV spectrum below 2100 Å is variable. Continua and emission lines originating from different layers in the solar atmosphere show a different degree of variability. Coronal emission lines at short wavelengths are much more variable than continua at longer wavelengths which originate in lower layers of the solar atmosphere. Typical time-scales of solar UV variability are minutes (flare induced), days (birth of active regions), 27 days (solar rotation), 11 years (solar cycle) and perhaps centuries, caused by long-term changes of the solar activity. UV intensity variations have been determined by either absolute irradiance measurements or by contrast measurements of plages vs. the quiet sun. Plages are the main contributor to the solar UV variability. Typical values for the solar UV variability over a solar cycle are: <1% at wavelengths longer than 2100 Å, 8% at 2080 Å (continuum), 20% at 1900 Å (continuum), 70% at H Lyα, 200% in certain emission lines 1200 < λ < 1800 Å and more than a factor of 4 in coronal lines λ < 1000 Å. Plage models predict the variable component of the solar UV radiation within ±50%. Absolute fluxes are known within ±30%. Several efforts are underway to monitor the solar UV irradiance with a precision better than a few percent over a solar activity cycle.     

快变分量观测与基本分量特性

本文对太阳２２周峰年期云南天文台日冕射电频谱仪观测到的６０个快速事件作了分析。从中获得了尖峰辐射、增强噪暴、快速起伏、类尖峰、叠加脉冲五种快变型别，对它们的亮温度、叠加特性、特征时间、辐射源尺度、偏振特性以及辐射机制六个方面作了分析研究后，对射电爆发、缓变分量和宁静太阳的辐射特征参量也作了研究，从而得出基本分量特性。     

A summary of significant solar-initiated events during STIP interval XII

Using data available at the present time, a summary of the significant solar-terrestrial events of STIP Interval XII (April 10–July 1, 1981) has been prepared. The first half of the interval was extremely active, several of the largest X-ray flares, particle events, and shocks of the present solar cycle took place during April and the first half of May. The second half of the interval, on the other hand, was characterized by relatively quiet conditions. Several large events which occurred on 10, 24 and 27 April and on 8 and 16 May are discussed in some detail. It is suggested that one of the most interesting subjects of future study could be the comparison and statistical analysis of the numerous events for which excellent observations are available, e.g. on what causes a type II burst to propagate in the interplanetary medium.     

磁扰和磁静期间海南扩展F起始时间出现率研究

利用2002年2月至2007年12月(第23太阳活动周的下降段)近6年的海南DPS-4型电离层测高仪探测数据, 对磁扰和磁静夜晚期间扩展F起始时间出现率进行统计研究. 结合海南电离层观测站所观测到的扩展F类型, 将扩展F区分为频率型、区域型、混合型和强区域型, 分别进行统计分析. 结果表明, 无论磁扰还是磁静夜晚, 混合型扩展F起始时间总出现率最高, 最为活跃, 其次为频率型和强区域型扩展F, 最不活跃的是区域型扩展F; 无论在磁扰还是在磁静夜晚条件下, 混合扩展F起始时间主要围绕在午夜前后, 且磁静时更多地起始于午夜前, 而磁扰时则倾向于延至午夜后, 频率型扩展F在午夜后较高, 而强区域型扩展F则在午夜前较高. 在本次太阳活动下降阶段, 强区域型与区域型扩展F的起始时间出现率逐年与太阳活动呈现一定的相关性. 所得结果有助于分析不同类型扩展F在形态和机制方面的差异.      

Reorganization of the solar corona following a C4.7 flare

Yohkoh X-ray images, multifrequency two-dimentional observations of the Nancay Radioheliograph, Kitt Peak and Mees magnetograms provide a unique set of data with which to study a C4.7 long-duration flare that was observed close to the equator (S07, W11) on 25 Oct. 1994 at 09:49 UT. Linear force-free field extrapolations indicate a very high degree of non-potentiality in the active region. The X-ray flare started with the expansion of spectacular twisted loops. Fifteen minutes after the flare onset sporadic radio (type III) bursts were observed spreading over an area of almost 1/3 of the solar disc and two remote X-ray brightenings appeared over quiet regions of opposite magnetic polarity located in on opposite hemispheres of the Sun. In the close vicinity of these remote brightenings two coronal holes formed. The timing and location of these events combined with the overall magnetic configuration provide evidence for a large-scale magnetic reconnection occurring between the expanding twisted loops and the overlying huge loops which inter-connect quiet solar regions.     

A balloon-borne sun-tracking multichannel photometer for atmospheric aerosol measurements

A balloon borne multichannel photometer for measurement of atmospheric scattering in the near ultraviolet and the visible wavelength regions has been developed at the Physical Research Laboratory, Ahmedabad for study of the size distribution and number density of aerosols at tropospheric and lower stratospheric altitudes. The instrumentation involves tracking the sun in elevation and scanning in azimuth. The payload was recently flown on a 100 kg. balloon from the Hyderabad Balloon Facility on 18 April 1984. The balloon reached a float altitude of 35 km and good quality data has been obtained from an altitude of 6 km upto float altitude. Data analysis is still in progress. The present paper details the instrument design and presents a few illustrations of the instrument performance from this flight.     

Effect of “Noisy” sun conditions on aircrew radiation exposure

In computer codes used to estimate the aircrew radiation exposure from galactic cosmic radiation, a quiet sun model is usually assumed. A revised computer code (PCAIRE ver. 8.0f) is used to calculate the impact of noisy sun conditions on aircrew radiation exposure. The revised code incorporates the effect of solar storm activity, which can perturb the geomagnetic field lines, altering cutoff rigidities and hence the shielding capability of the Earth’s magnetic field. The effect of typical solar storm conditions on aircrew radiation exposure is shown to be minimal justifying the usual assumptions.     

太阳宁静及耀斑期间1AU附近等离子体轫致辐射研究

在太空等离子体中，尤其在等离子体内部磁场较弱时，轫致辐射是等离子体能量损失的主要机制．本文对太阳宁静及耀斑期间1AU处等离子体轫致辐射计算表明，等离子体辐射强度If的变化与辐射的电磁波频率有直接的关系．当辐射频率，接近于等离子体频率，fpe时，辐射强度显著增大．随着电磁波辐射频率的增大，辐射强度随频率增大作缓慢对数下降．辐射亮温Tb与等离子体电子温度Te、介质光深成正比．Tb与If随辐射频率变化的整体趋势一致．在相同的辐射频率情况下，太阳宁静期间If值、Tb值低于太阳耀斑期间If值、Tb值．     

Balloon observation of the 1983 solar eclipse in Indonesia

A balloon observation of the total solar eclipse on 11 June 1983 was carried out as a cooperative work between Japanese and Indonesian teams. The observation was a photo-polarimetry of the F corona in both visual and near-infrared regions.The balloon of 15,000-m³ with a payload of 150-kg was launched at 7^h13^m on 11 June from Watukosek Balloon Base in East Java. Observation at an altitude of 30.5-km was successfully made during the totality (11^h28～32^m) at a position of ～40-km east-south-east from Jogjakarta.As a preliminary result, an excess in infrared brightness has been found near the position of 3.8R_⊙ west from the sun, which may be due to thermal emission from a high-temperature dust cloud located around the sun.     

Angular distributions of energetic charged particles observed with HELIOS-1 and -2 between 0.3 amd 1 AU and their relevance to manned interplanetary space missions.

The University of Kiel Cosmic Ray Instrument on board the solar probes HELIOS-1 and -2 measured angular distributions of electrons, protons, and heavier nuclei between 0.3 and 1 AU over one complete solar cycle between 1974 and 1986. Anisotropies are observed mainly during the rising phase of solar particle events or close to the passage of certain interplanetary shocks. The anisotropies are presented as proton data of energies between 27 and 37 MeV. The dependence of the anisotropies on particle energy and distance from the sun is provided based on diffusive propagation in interplanetary space. Strong anisotropies could provide a chance of efficient shielding of the passenger compartment by moving heavier parts of the spacecraft structure into the direction of the highest flux. A reduction of the total radiation dose by less than a factor of 2 might be achievable, however, selection of quiet times for the mission reduces the radiation hazard much more.     

Reconstruction of the solar UV irradiance back to 1974

The variability of the solar UV irradiance has strong effects on the terrestrial atmosphere. In order to study the solar influence for times when no UV observations are available, it is necessary to reconstruct the variation of the UV irradiance with time on the basis of proxies. We present reconstructions of the solar UV irradiance based on the analysis of space-based and ground-based magnetograms of the solar disk going back to 1974. With COde for Solar Irradiance (COSI) we calculate solar intensity spectra for the quiet Sun and different active regions and combine them according to their fractional area on the solar disk, whereby their time-dependent contributions over the solar cycle lead to a variability in radiation. COSI calculates the continuum and line formation under conditions which are out of local thermodynamic equilibrium (non-LTE). The applied temperature and density structures include the chromosphere and transition region, which is particularly important for the UV. The reconstructions are compared with observations.     

用极区双雷达研究高纬电离层电场——对观测结果的物理讨论

本文以极区双雷达STARE系统观测到的高纬E区电场(65°—70°范围内)之形态为基础,用简单模式法对其中部分有趣现象进行了讨论。静日(1≤K_p≤3)形态与Vasyliunas模式符合较好。其晨一昏不对称性可部分地由电导率日一夜不均匀性解释,同时也说明在磁层中亦应有晨-昏不对称因素。本文还提出了两个简单模式,以讨论扰日对流圈的西向旋转。其一讨论了场向电流一、二区的相对强度产生之效果;其二考虑了Hall和Pederson电导率之比的作用,并对此两模式进行了比较。为了进一步搞清这个问题,需对磁层过程有更多的了解,也需要对电场和场向电流进行同时性的观测。