Solar microwave precursors and coronal mass ejection: Possible connection

Radiophysical Research Institute (NIRFI), Nizhny Novgorod (Gorky), Russia. Published in Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 37, No. 7, pp. 883–886, July, 1994.     

太阳日冕物质抛射的磁流体力学性质

太阳是离地球最近的一颗恒星,太阳日冕物质抛射是太阳大气中最剧烈的一种活动现象.当日冕物质抛射爆发时,大量的等离子体物质从接近太阳日面的低日冕被抛出,瞬时释放出巨大的能量.当一部分这些物质和能量传播到地球附近时,可以造成短波通讯中断、卫星工作失常等破坏性现象.文章作者认为,是缠绕的太阳磁场提供了足够的能量,使这些日冕物质可以克服恒星的重力以及周边磁场的束缚抛射出来;而磁螺度在日冕中的不断积累,不仅为日冕物质抛射提供了能量基础,而且使爆发在一定程度上成为一种日冕演化的必然.     

Cluster of solar active regions and onset of coronal mass ejections

round-the-clock solar observations with full-disk coverage of vector magnetograms and multi-wavelength images demonstrate that solar active regions(ARs) are ultimately connected with magnetic field. Often two or more ARs are clustered, creating a favorable magnetic environment for the onset of coronal mass ejections(CMEs). In this work, we describe a new type of magnetic complex: cluster of solar ARs. An AR cluster is referred to as the close connection of two or more ARs which are located in nearly the same latitude and a narrow span of longitude. We illustrate three examples of AR clusters, each of which has two ARs connected and formed a common dome of magnetic flux system. They are clusters of NOAA(i.e., National Oceanic and Atmospheric Administration) ARs 11226 11227, 11429 11430, and 11525 11524. In these AR clusters, CME initiations were often tied to the instability of the magnetic structures connecting two partner ARs, in the form of inter-connecting loops and/or channeling filaments between the two ARs. We show the evidence that, at least, some of the flare/CMEs in an AR cluster are not a phenomenon of a single AR, but the result of magnetic interaction in the whole AR cluster. The observations shed new light on understanding the mechanism(s) of solar activity. Instead of the simple bipolar topology as suggested by the so-called standard flare model, a multi-bipolar magnetic topology is more common to host the violent solar activity in solar atmosphere.     

Study of the relationship between coronal mass ejections and energetic electrons in interplanetary space

We consider time characteristics of energetic electron events in the interplanetary space after solar flares associated with coronal mass ejections (CME). Analysis of electron intensity-time profiles shows that independently of flare duration, times to electron event maximum from flare onset and from electron event onset increase with increasing of CME velocity. A possible interpretation of this effect is electron acceleration by CME associated with a shock wave.Published from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 39, No. 1, pp. 46–52, January, 1996.This work was supported by the Russian Foundation for Fundamental Research (grant 94-02-04453) and by a Contract with EOARD (grant SPC-94-4071).     

On the relationship between solar flares,coronal mass ejections,and post-eruption energy release

We present and illustrate a concept that involves two basic statements: (a) solar pulse flares and coronal mass ejections (CME) are physically similar, but, generally speaking, independent phenomena, which can occur both individually and jointly, initiating each other in different cause and- effect combinations; (b) in the analysis of the relationship between the flares and CMEs one must take into account that the latter result in significant post-eruption flare-like energy release in the corona, which can be accompanied by many important phenomena including the prolonged acceleration of particles.     

Modulation of galactic cosmic ray intensities by coronal mass ejections into interplanetary space

The data on the measurements of the intensities of galactic cosmic rays with proton energies greater than 30 MeV are compared with the data on the solar wind and interplanetary magnetic field measured on board the Vega-1 and Vega-2 automated interplanetary stations. Modulation structures with characteristic shapes and durations, namely quasi-symmetric (“bays”) short-term Forbush decreases of intensity, are revealed. It is shown that these Forbush decreases were recorded due to the stations flying through coronal mass-ejection regions. Original Russian Text ? E.A. Chuchkov, V.I. Tulupov, V.P. Okhlopkov, G.P. Lyubimov, 2009, published in Vestnik Moskovskogo Universiteta. Fizika, 2009, No. 3, pp. 90–93.     

Causal explanation for observed superluminal behavior of microwave propagation in free space

In this Letter we present a theoretical analysis of an experiment by Mugnai and collaborators where superluminal behavior was observed in the propagation of microwaves. We suggest that what was observed can be well approximated by the motion of a superluminal X wave. Furthermore, the experimental results are also explained by the so called scissor effect which occurs with the convergence of pairs of signals coming from opposite points of an annular region of the mirror and forming an interference peak on the intersection axis traveling at superluminal speed. We clarify some misunderstandings concerning this kind of electromagnetic wave propagation in vacuum.     

Interfacial phenomena on the graphite-lithium electrode during the formation process and thermal aging

Slow scan voltammery (SSV), electrochemical impedance spectroscopy (EIS) and galvanostatic cycling (GC) were used to characterize the formation of the Solid Electrolyte Interphase (SEI) on a graphite electrode during lithiation and delithiation and during thermal aging. The SSV and GC results show the irreversible character of the first reduction peak/semi-plateau at 0.8 V. After aging, a new irreversible plateau appears in the GC curves. Concomitantly the interfacial resistances as determined from the Nyquist plots increased then decreased as the signature of SEI transformation. We suggest the SEI is subjected to precipitation/dissolution processes. Paper presented at the 8th EuroConference on Ionics, Carvoeiro, Algarve, Portugal, Sept. 16–22, 2001.     

Near infrared spectral and polarization imaging observation of coronal emission lines during the 2008 total solar eclipse

During the 2008 total solar eclipse, the coronal emission lines were observed by using optical fibre spectrometric and polarization imaging system in near infrared waveband. The profiles of the coronal emission lines including Fe XIII 10747 ?, 10798 ? and He I 10830 ? were obtained with dispersion of 0.5 ? /pix. The intensity of Fe XIII 10747 ? remained unchanged in the two different coronal regions while the intensity of He I 10830 ? varied considerably in the two coronal locations no matter whether the prominence appeared or not. The coronal polarization images were observed at Fe XI 7892 ? with a bandpass of 30 ? in a series of exposure times.     

Acoustic emission during the formation and breakdown of a dislocation cluster

We construct a model for the formation of a dislocation cluster and its evolution after the detachment of the head dislocation. The results obtained with the help of this model are used for calculating the acoustic emission signal accompanying the stages of cluster formation and breakdown. The elastic stresses in the signal under investigation are estimated. The data on relaxation of elastic stresses in the sample containing the cluster are reported.     

Constructive and destructive interference in acoustic emission during fatigue crack propagation

Fatigue crack propagation monitoring with acoustic emission reveals the presence of maxima and minima in the curve of the count rate as a function of the stress intensity factor. This is explained in terms of constructive and destructive interference due to specimen geometry. A theoretical model is developed and experimental proof of the validity of the model is presented.     

Abrupt buckling transition observed during the plectoneme formation of individual DNA molecules

The response of single DNA molecules to externally applied forces and torques was directly measured using an angular optical trap. Upon overwinding, DNA buckled abruptly as revealed by a sharp extension drop followed by a torque plateau. When the DNA was held at the buckling transition, its extension hopped rapidly between two distinct states. Furthermore, the initial plectonemic loop absorbed approximately twice as much extension as was absorbed into the plectoneme upon each additional turn. The observed extension change after buckling and the postbuckling torque support a recent DNA elasticity model.     

Effect of the electromagnetic field of an eruptive prominence on coronal and chromospheric plasmas (CME and Hα emission formation)

The frozen- in chromospheric and coronal plasma motions during an eruption of a filament with a magnetic field configuration described by the inverse polarity model are considered. At the initial stage of the filament motion the magnetic field compresses the chromospheric gas within two strips located symmetrically about the inversion line. The compression is accompanied by plasma heating and emission enhancement in the lineH _α. The distance between the strips increases with filament altitude above the photosphere. This mechanism is sufficient to describe the dynamics ofH _α emission kernels in two- ribbon flares. In the corona region in which the magnetic pressure of the filament field is greater than the gas pressure, plasma rarefaction and cavity formation occur. Near the boundary β=1the plasma is decelerated and its density increases, which corresponds to the formation of an outer shell of the CME.     

The big problems in star formation: The star formation rate,stellar clustering,and the initial mass function

Star formation lies at the center of a web of processes that drive cosmic evolution: generation of radiant energy, synthesis of elements, formation of planets, and development of life. Decades of observations have yielded a variety of empirical rules about how it operates, but at present we have no comprehensive, quantitative theory. In this review I discuss the current state of the field of star formation, focusing on three central questions: What controls the rate at which gas in a galaxy converts to stars? What determines how those stars are clustered, and what fraction of the stellar population ends up in gravitationally-bound structures? What determines the stellar initial mass function, and does it vary with star-forming environment? I use these three questions as a lens to introduce the basics of star formation, beginning with a review of the observational phenomenology and the basic physical processes. I then review the status of current theories that attempt to solve each of the three problems, pointing out links between them and opportunities for theoretical and numerical work that crosses the scale between them. I conclude with a discussion of prospects for theoretical progress in the coming years.     

Double-peak droplet mass distribution observed during sub-ps laser ablation of Si targets

The angular distribution of the ablated material was studied during sub-ps Si laser ablation deposition using a special hemicylindrical substrate holder and different laser fluences ranging between 0.4 and 1.7 J/cm². Scanning electron microscopy analysis of the deposited films showed that, independent of the fluence, the distribution of the deposited droplets presents two maxima. The first maximum corresponds to the average plume deflection angle value due to the local surface orientation produced by the preferential etching process. The second maximum is observed approximately at 45° with respect to the normal of the target surface, and is related to the phase explosion products that expand along the incident laser beam direction. The investigation of the twofold distribution of the sub-μm size deposited droplets is important to improve the quality of the deposited coatings. PACS 81.15.Fg; 68.55.Jk; 79.20.Ds