Flare buildup in X-rays,UV, microwaves and white light

Coordinated observations using space and ground-based instruments were made of active region complex #2522/2530, 24–30 June, 1980. The 10 largest flares from these regions were of importance M1-M6 in X-rays, and all were observed from satellites, except for one observed from a balloon. Several kinds of buildup signature have been found in the tens of minutes before these flares. Among these signatures are the following: 1) Relative faintness in X-ray lines of the pre-flare pixels, 2) X-ray (5–15 keV) “flashes” at points displaced by 1′–2′ from the flare site, 3) Rising filaments seen in Hα and Ultraviolet 4) Microwave intensification, polarization increase and polarization flip 5) Coronal disturbances above limb flares at or before the impulsive phase.     

1980年11月6日—7日耀斑后冕拱的激活机制

1980年11月6日耀斑后冕拱(Post-flare coronal arch)在母耀斑(AR2779)开始后3小时形成, 并在形成后11小时和25小时两次激活。两次激活均由双带耀斑的增长环系所致。本文提出了激波加热和Petschek重连是该冕拱有效的激活机制。导出并求解了考虑辐射损失、热传导、激波加热和Petschek重连加热的冕拱能量方程。理论计算结果与Svestka根据SMM空间资料所给出的该冕拱的激活曲线基本符合。      

1986年2月4日AR4711拱形双带黑子暗条系激活的分析

根据1986-02-04AR47ll由观测所确定的物理参数和特征值,采用电动力学方法数值计算该活动区中两个拱形黑子暗条在大耀斑爆发前的动力学演化过程.结果表明:(1)以旋涡黑子为标志的光球物质旋转运动和以暗条下方磁力线强剪切为特征的剪切运动引起暗条电流增加和背景磁场变化,电流和磁场的相互作用导致暗条向上运动,大耀斑爆发前暗条的上升速度达26km／S;(2)背景场位形对暗条整体动力学行为有很大影响,AR47ll在7×104km高度范围内场强随高度似乎按指数规律衰减.      

Magnetic field structure changes in the vicinity of solar flares

Changes in the structure of the sunspot group and its magnetic field are studied in Hale Region 17644 (May 1981) in connection with the May 16 3B/X1 flare. The characteristic changes, also found in HR 16850 (May 1980) and HR 17098 (September 1980), are the following: Rapid motions of umbrae of opposite polarity in the vicinity of the magnetic zero line, parallel to this line, but in opposite direction. Appearence of new small spots before the flare, leading to a more complicated field structure. Simplification of the magnetic structure after the flare in some days, i.e. decrease of spot areas in the affected territory and the straightening of the magnetic zero line.     

HALE 17590 活动区的爆发辐射

本文根据1981年HALE 17590 太阳活动区的观测资料,着重分析了它的射电辐射特性后发现:(1)在光学活动区发展的上升阶段,每串射电爆发的强度也有由弱到强的变化,其频谱由单调谱变成不规则谱和U型谱;(2)对大的耀斑爆发而言,射电爆发的先兆相比X射线爆早。在射电先兆相期间常伴有谱斑增亮和暗条激活等现象;(3)大耀斑爆发的脉冲极大时刻在射电8毫米波段到来最早。      

Flare build up: 21 May 1980

The decaying solar active region that crossed the central meridian on May 20, 1980 at latitude S13° produced a major flare (2B/X1) at 2054 on May 21. This region was a target of the international Flare Buildup Study and was well observed. The buildup was characterized by little flare activity during two days prior to the major flare but a great deal of activity in the filament that separated the opposite magnetic polarities of the active region. Large proper motions of sunspots and magnetic fields suggest that the magnetic field was stressed prior to the flare. The immediate trigger of the flare appears to have been an eruption of new magnetic flux in the center of the active region. The new flux erupted in a configuration that decreased the net flux of the active region and contributed to the decay of the region.     

Detection of solar neutrons on a long duration balloon flight

The observation of large solar flares on high altitude balloons requires long duration balloon flights because large flares are infrequent and cannot be predicted with enough reliability and lead time to allow a conventional balloon to be launched and reach altitude before the flare occurs. With the many weeks at float altitude expected for a long duration flight, the probability of “catching” a large flare during solar maximum becomes reasonably high and the study of phenomena which heretofore have required a satellite become accessible to a balloon platform. One example of this type of experiment is the observation of neutrons produced by the interaction of flare accelerated nucleons with the solar atmosphere. Because the neutrons are produced immediately by the flare accelerated particles and are unaffected by their transmission through the upper solar atmosphere and the intervening magnetic fields, their observation at 1 A.U. will provide direct information on the flare acceleration process. Specifically, a measurement of the neutron energy and time spectra will yield the energy spectrum of the charged nucleons in the interval 50 to 500 MeV/amu, the charged particle anisotropy, the height of the acceleration region for limb flares, and information on the two-stage acceleration process. Because the γ-ray spectrum is also sensitive to these factors, a combined neutron and γ-ray measurement will provide a much more stringent test of flare models than either done separately. CWRU and the University of Melbourne have designed the EOSCOR (Extended Observation of Solar and Cosmic Radiation) detector to have the necessary sensitivity to detect neutrons from a flare 0.1 the size of the 4 Aug. 1972 event and to be compatible with the constraints of the long duration balloon system. The detector has been test flown on short duration balloon flights and calibrated at E_n = 38, 58, and 118 MeV. It is planned to launch it on a long duration balloon flight from Australia in December 1982 when simultaneous γ-ray observations will be possible with the SMM and/or HINTORI satellites.     

日面耀斑环中物质的运动

利用云南天文台1980年7月14日3B级双带耀斑的光学观测资料,以及SMM卫星对同一耀斑的X射线观测结果,讨论日面耀斑环中物质的运动规律。先比较耀斑Hα象和X射线象的日面位置,根据投影效应确定耀斑环的高度;然后从理论上估算由于耀斑环中物质下落,所形成的耀斑活动区视向速度的分布。所得结果与观测资料基本相符。      

The 1980 April 12 flare and transient: Report on progress in interpretation

A multidisciplinary study of this solar-interplanetary event is summarized by two main points: this flare was an incident in a process that began days before the flare, and continued after the flare; and the chain of events can be interpreted most simply in terms of energy input over scales of time and space that are large compared to the flare seen in the light of Hα. In support of these points, 5 aspects of the flare are described here: (1) hours before the flare, slow changes in coronal structure were associated with radio continuum emission, suggesting large-scale magnetic-field changes and the presence of energetic electrons; (2) long-lived X-ray loops require sustained energy input for at least an hour after the flare start; (3) interplanetary disturbance near earth is probably related to this limb flare, although the (expected) absence of a shock makes identification uncertain; (4) the coronal mass ejection overlay decaying magnetic field; (5) speed derived from frequency drift of the type II radio burst in the low corona, and from the travel time of the disturbance to 1 a.u., are about twice as great as the observed speed of the coronal mass ejection and of the disturbed solar-wind speed.     

1980年7月14日耀斑和磁流浮现模型

本文利用云南天文台耀斑H_α巡视观测、活动区白光照相及速度场资料,结合SMM的X射线资料和北京天文台的射电观测资料,对1980年7月14日日面3B级大耀斑进行了综合研究。对照耀斑过程的磁流浮现(EMF)模型,我们分析了活动区的形态变化特征,估算了耀斑释放的磁能、耀斑过程的特征时间及耀斑爆发时加速的电子总数和加速电子的平均能量。结果表明:(1)耀斑过程的EMF模型与观测结果基本符合,可以认为EMF模型能够较好地说明耀斑的物理过程。(2)根据对速度场资料及耀斑产生位置的分析,初步认为电流片可能位于速度中性线与磁中性线的交点处及其附近,或速度中性线与暗条的交点处及其附近[3]。(3)观测和计算表明,硬x射线爆是由电流片中加速的高能非热电子所产生,而软X射线爆则由耀斑区的高温等离子体的热轫致辐射所产生。      

Relationships of a growing magnetic flux region to flares

Some sites for solar flares are known to develop where new magnetic flux emerges and becomes abutted against opposite polarity pre-existing magnetic flux (review by Galzauskas/1/). We have identified and analyzed the evolution of such flare sites at the boundaries of a major new and growing magnetic flux region within a complex of active regions, Hale No. 16918. This analysis was done as a part of a continuing study of the circumstances associated with flares in Hale Region 16918, which was designated as an FBS target during the interval 18 – 23 June 1980. We studied the initiation and development of both major and minor flares in Hα images in relation to the identified potential flare sites at the boundaries of the growing flux region and to the general development of the new flux. This study lead to our recognition of a spectrum of possible relationships of growing flux regions to flares as follows: (1) intimate interaction with adjacent old flux — flare sites centered at new/old flux boundary, (2) forced or “intimidated” interaction in which new flux pushes old field having lower flux density towards a neighboring old polarity inversion line where a flare then takes place, (3) “influential” interaction — magnetic lines of force over an old polarity inversion line, typically containing a filament, reconnect to the new emerging flux; a flare occurs with erupting filament when the magnetic field overlying the filament becomes too weak to prevent its eruption, (4) inconsequential interaction — new flux region is too small or has wrong orientation for creating flare conditions, (5) incidental — flare occurs without any significant relationship to new flux regions.     

Direct evidence for chromospheric evaporation in a well-observed compact flare

We have observed the flare of 1980 May 7 1456 UT with several Solar Maximum Mission instruments, in coordination with the Sacramento Peak Observatory Vacuum Tower Telescope. From the X-ray data we determine the total amount of plasma at T > 2 × 10⁶ K, commonly attributed to chromospheric evaporation. From Hα we have determined the amount of plasma that has been evaporated from the chromosphere. We find that enough material has been evaporated from the chromosphere to account for the X-ray plasma. Taken together, the Hα, soft and hard X-ray images suggest that chromospheric evaporation is driven both by flare accelerated electrons, during the impulsive phase, and conduction, during the thermal phase.     

1980年11月5日耀斑的硬、软X射线及微波的象与Hα等光度象的比较

本文对1980年11月5日22点25分开始的1B/M1-M4的Hα耀斑进行了图象处理,绘制了等光度图;与硬、软X射线象,微波象进行了比较.结果表明:1.耀斑的第一次极大,高能电子没有穿透到色球.Hα耀斑主要是由T=107—108K(产生软硬X射线的热区)等离子体向下传导到色球而形成.2.Hα耀斑的第二次极大,是由高能电子轰击色球而形成,Hα耀斑滞后数秒(小于5秒).3.耀斑闪光相,Hα面积与Hα强度同步增长.4.从耀斑前后的横向磁场变化(Hα短纤维的变化),估计磁能释放～1031尔格.      

Two successive partial mini-filament confined ejections

Active region (AR) NOAA 11476 produced a series of confined plasma ejections, mostly accompanied by flares of X-ray class M, from 08 to 10 May 2012. The structure and evolution of the confined ejections resemble that of EUV surges; however, their origin is associated to the destabilization and eruption of a mini-filament, which lay along the photospheric inversion line (PIL) of a large rotating bipole. Our analysis indicate that the bipole rotation and flux cancellation along the PIL have a main role in destabilizing the structure and triggering the ejections. The observed bipole emerged within the main following AR polarity. Previous studies have analyzed and discussed in detail two events of this series in which the mini-filament erupted as a whole, one at 12:23 UT on 09 May and the other at 04:18 UT on 10 May. In this article we present the observations of the confined eruption and M4.1 flare on 09 May 2012 at 21:01 UT (SOL2012-05-09T21:01:00) and the previous activity in which the mini-filament was involved. For the analysis we use data in multiple wavelengths (UV, EUV, X-rays, and magnetograms) from space instruments. In this particular case, the mini-filament is seen to erupt in two different sections. The northern section erupted accompanied by a C1.6 flare and the southern section did it in association with the M4.1 flare. The global structure and direction of both confined ejections and the location of a far flare kernel, to where the plasma is seen to flow, suggest that both ejections and flares follow a similar underlying mechanism.     

MHD simulation of magnetic field configuration above the active region NOAA 10365

The current sheet (CS) creation before a flare in the vicinity of a singular line above the active region NOAA 10365 is shown in numerical experiments. Such a way the possibility of energy accumulation for a solar flare is demonstrated. These data and results of observation confirm the electrodynamical solar flare model that explains solar flares and CME appearance during CS disruption. The model explains also all phenomena observed in flares. For correct reproduction of the real boundary conditions the magnetic flux between spots should be taken into account. The full system of 3D MHD equations are solved using the PERESVET code. For setting the boundary conditions the method of photospheric magnetic maps is used. Such a method permits to take into account all evolution of photospherical magnetic field during several days before the flare.     

The morphology and velocity field of the large flare on the solar disc on July 14, 1980

The active region morphology and the features of solar radio bursts and sight-line velocity distribution of a flare of Importance 3B on the solar disc (AR 2562) on 1980 July 14 are introduced in this article.     

Study of ionospheric D region changes during solar flares using MF radar measurements

During solar flares, the X-ray radiation suddenly increases, resulting in an increase in the electron density of the atmospheric D region and a strong absorption of short-wave radio waves. Based on Langfang medium frequency (MF) radar, this paper analyzed the variation characteristics of D region in the lower ionosphere from 62 km to 82 km. The analysis focused on multiple C-level and M-level solar flare events before and after the large-scale flare event at 11:53 (UT) on September 6, 2017. The results show that it is difficult to detect the electron density over 70 km in Langfang during solar flares, but the electron density value can be obtained as low as 62 km, and the stronger the flare intensity, the lower the detectable electron density height. Besides, the equal electron density height, the received power of X and O waves will also be significantly reduced during the flares, and the reduction of equal electron density height has a weak linear relationship with flare intensity.     

Analysis of the 1980 November 18 limb flare observed by the hard X-ray imaging spectrometer (HXIS)

X-ray images of the 18 November 1980 limb flare taken by the HXIS instrument aboard SMM were analysed. The hard X-rays originated from three spots on the SW limb of the solar disk with different altitudes and time evolution. The locations of the brightest spots in hard and soft X-rays are compared with the predictions of flare models. The X-ray spctra from the pixels with highest count rates can be fitted by power laws. The spatial variation of the spectral index is in agreement with the existence of a non-thermal electron component.     

Structural development of the X-ray limb flare of 30 April 1980

We describe the development of the limb flare of 30 April 1980, 20:20 UT, as observed by the Hard X-ray Imaging Spectrometer (HXIS) aboard the Solar Maximum Mission (SMM). It consisted of a short-lived bright nucleus (FWHM < 10,000 km), just inside the Sun's limb; a longer lasting tongue, extending to a height of 30,000 km, and a more complicated feature, approximately situated at the Sun's limb. The tongue was a pre-existing magnetic structure that started emitting X-rays only a few seconds after the bright nucleus, and which had a slightly higher temperature than the nucleus; its X-ray emission may be caused by electrons escaped from the nucleus.     

Solar maximum mission experiment: Early results of the hard X-ray imaging experiment

We have selected four widely different flares from the early period of operations of the Hard X-Ray Imaging Spectrometer (HXIS) on SMM to illustrate the characteristic imaging properties of this experiment. For the small flare of April 4, 1980, we demonstrate the instrument's capability for locating a compact source. In the weak, but extensive, flare of April 6 we show how well the instrument can display spatial structure, and also the low level of the instrument background. In the 1B flare of April 7 we are able to locate positions of the X-ray emission in the soft and hard channels, and estimate the positional variations of the emission patches. Finally, in the IN flare of April 10, which produced the strongest hard X-ray burst we have seen so far, we repeat some of the studies made for the April 7 event, and also demonstrate the capability of the HXIS instrument to study the development, with high time resolution, of individual 8″ × 8″ elements of the flare.