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Recent results of zebra patterns in solar radio bursts

Research in Astronomy and Astrophysics 2010年第9期10卷 821-866页

作者： Gennady P.chernov Key Laboratory of Solar Activity National Astronomical ObservatoryChinese Academy of Science Pushkov Institute of Terrestrial Magnetism Ionosphere and Radio Wave PropagationRussian Academy of Sciences (IZMIRAN)

This review covers the most recent experimental results and theoretical research on zebra patterns （ZPs） in solar radio bursts. The basic attention is given to events with new peculiar elements of zebra patterns received over the last few years. All new properties are considered in light of both what was known earlier and new theoretical models. Large-scale ZPs consisting of small-scale fiber bursts could be explained by simultaneous inclusion of two mechanisms when whistler waves ＂high- light＂ the levels of double plasma resonance （DPR）. A unique fine structure was observed in the event on 2006 December 13： spikes in absorption formed dark ZP stripes against the absorptive type Ⅲ-like bursts. The spikes in absorption can appear in accordance with well known mechanisms of absorptive bursts. The additional injection of fast particles filled the loss-cone （breaking the loss-cone distribution）, and the generation of the continuum was quenched at these moments. The maximum absorptive effect occurs at the DPR levels. The parameters of millisecond spikes are determined by small dimensions of the particle beams and local scale heights in the radio source. Thus, the DPR model helps to understand severai aspects of unusual elements of ZPs. However, the simultaneous existence of several tens of the DPR levels in the corona is impossible for any realistic profile of the plasma density and magnetic field. Three new theories of ZPs are examined. The formation of eigenmodes of transparency and opac- ity during the propagation of radio waves through regular coronal inhomogeneities is the most natural and promising mechanism. Two other models （nonlinear periodic space - charge waves and scattering of fast protons on ion-sound harmonics） could happen in large radio bursts.

关键词： Sun general -- Sun flare -- Sun radio radiation

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Envelope Soliton in Solar Radio Emission

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Chinese Physics Letters 2000年第5期17卷 355-357页

作者： WANG De-Yu G.P.chernov Purple Mountain Observatory Chinese Academy of SciencesNanjing 210008 National Astronomical Observatories Chinese Academy of Sciences IZMIRAN 142092 TroitaskMoscow RegionRussia

Several envelope soliton fine structures have been observed in solar radio metric-wave *** a model of longitudinal modulational instability to explain these fine *** is found that this instability can only occur in the condition of sound velocity being larger than Alfvin velocity in ***,the envelope soliton fine structures should display in the coronal region with high temperature and low magnetic 6eld,which corresponds to the solar radio emission in the region of meter and decameter wavelength.

关键词： soliton envelope Soliton

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Multi-scale hydrological system-of-systems realized through WHOS:the brokering framework

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International Journal of Digital Earth 2022年第1期15卷 1259-1289页

作者： Enrico Boldrini Stefano Nativi Silvano Pecora Igor chernov Paolo Mazzetti Institute of Atmospheric Pollution Research (CNR-IIA) National Research Council of ItalySesto Fiorentino (FI)Italy World Meteorological Organization (WMO) GenevaSwitzerland Ministero della Transizione Ecologica (MITE) RomaItaly

Global Change challenges are now systematically recognized and tackled in a growingly coordinated manner by intergovernmental organizations such as the United *** observing networks provide the founded data sources to assess the Earth environmental status and take sound decisions to achieve a sustainable *** Hydrological Observing System(WHOS)allows to discover and access historical and near real time hydrological *** represents the hydrological contribution to the wider WIGOS-WIS system of *** is a digital ecosystems framework contributed by a set of data providers and technical support *** this framework,three regional pilots were successfully *** WHOS architecture applies the services brokering style,implemented through the Discovery and Access Broker technology.A brokering approach makes a global system of systems possible and sustainable,where the different enterprise systems are enabled to interoperate,despite they implement heterogeneous communication interfaces and data *** this manuscript,the WHOS brokering solution is detailed by recurring to the definition of a set of transversal viewpoints to describe the important aspects of the complex ecosystem–namely:enterprise,information,computational,engineering,and technological ***,the three regional pilot ecosystems are described as successful cases of WHOS implementation.

关键词： Data brokering hydrology system-of-systems interoperability

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The importance of source positions during radio fine structure observations

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Research in Astronomy and Astrophysics 2014年第7期14卷 831-842页

作者： Guennadi P.chernov Yi-Hua Yan Qi-Jun Fu Key Laboratory of Solar Activity National Astronomical ObservatoryChinese Academy of Sciences Pushkov Institute of Terrestrial Magnetism Ionosphere and Radio Wave PropagationRussian Academy of Sciences (IZMIRAN)TroitskMoscow region142190Russia

The measurement of positions and sizes of radio sources in the observations of the fine structure of solar radio bursts is a determining factor for the selection of the radio emission mechanism. The identical parameters describing the radio sources for zebra structures（ZSs） and fiber bursts confirm there is a common mechanism for both structures. It is very important to measure the size of the source in the corona to determine if it is distributed along the height or if it is point-like. In both models of ZSs（the double plasma resonance（DPR） and the whistler model） the source must be distributed along the height, but by contrast to the stationary source in the DPR model, in the whistler model the source should be moving. Moreover, the direction of the space drift of the radio source must correlate with the frequency drift of stripes in the dynamic spectrum. Some models of ZSs require a local source, for example,the models based on the Bernstein modes, or on explosive instability. The selection of the radio emission mechanism for fast broadband pulsations with millisecond duration also depends on the parameters of their radio sources.

关键词： solar flare -- radio emission -- zebra-pattern -- spike-bursts

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On the Zebra Structure in the Frequency Range near 3 GHz

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Chinese Journal of Astronomy and Astrophysics 2001年第6期1卷 525-536页

作者： G.P.chernov L.V.Yasnov~ Yi-HuaYan Qi-JunFu NationalAstronomicalObservatories ChineseAcademyofSciencesBeijing100012 St.PetersbourgUniversity St.PetersbourgRussia

We present 19 cases of zebra pattern structure (ZPS) and fiber bursts (FB) in radio bursts in frequency range around 3 GHz, and one such case in the range 5.2-7.6 GHz, using the new microwave spectrometer of NAOC between 2.6-3.8 and 5.2-7.6 GHz (China, Huairou station) with high resolution (10 MHz and 8 ms). The FB and ZPS have about the same spectral parameters: the frequency bandwidth of emission stripes △f-20MHz, the frequency separation between the emission and the neighboring low frequency absorption -△fea-30MHz and the frequency separation between emission stripes (when a periodic structure persists) △fs -60-70 MHz. Therefore we consider both these fine structures to be whistler manifestations, i.e., interactions of plasma electrostatic waves with whistler waves (generated by the same fast particles with loss-cone anisotropy) l + w → t. The duration of the fiber bursts of about 2 s corresponds to whistler waves propagating undamped at about 2s, which requires a whistler increment < 0.5 s-1. In the frequency range 3-7 GHz the relation between the ratios of plasma to cyclotron frequencies and whistler to cyclotron frequencies is almost independent of the decrement of whistler electron damping. This finding is used to obtain the magnetic field strength in the region of generation. For a reasonable value of electron temperature (2-20 MK), we find B = 125-190 G when the electron density is (8-18) × 1010 cm-3 and B = 520 - 610 G when the electron density is (35-60) × 1010 cm-3. In two remarkable events, 1998-04-15 and 2000-10-29, the right-hand polarization is strong for all the fine structures and corresponds to ordinary wave.

关键词： Sun: radio radiation - Sun: activity

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Concerning spikes in emission and absorption in the microwave range

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Research in Astronomy and Astrophysics 2013年第1期13卷 115-128页

作者： Gennady P.chernov Robert A.Sych Guang-Li Huang Hai-Sheng Ji Yi-Hua Yan Cheng-Ming Tan Key Laboratory of Solar Activity National Astronomical ObservatoryChinese Academy of Sciences Pushkov Institute of Terrestrial Magnetism Ionosphere and Radio Wave PropagationRussian Academy of Sciences (IZMIRAN) Institute of Solar-Terrestrial Physics Purple Mountain Observatory Chinese Academy of Sciences

In some events, weak fast solar bursts （near the level of the quiet Sun） were observed in the background of numerous spikes in emission and absorption. In such a case, the background contains the noise signals of the receiver. In events on 2005 September 16 and 2002 April 14, the solar origin of fast bursts was confirmed by simultaneous recording of the bursts at several remote observatories. The noisy background pixels in emission and absorption can be excluded by subtracting a higher level of continuum when constructing the spectra. The wavelet spectrum, noisy pro- files in different polarization channels and a spectrum with continuum level greater than zero demonstrates the noisy character of pixels with the lowest levels of emission and absorption. Thus, in each case, in order to judge the solar origin of all spikes, it is necessary to determine the level of continuum against the background of which the solar bursts are observed. Several models of microwave spikes are discussed. The electron cyclotron maser emission mechanism runs into serious problems with the in- terpretation of microwave millisecond spikes： the main obstacles are too high values of the magnetic field strength in the source （Pe 〈 uB）. The probable mechanism is the interaction of plasma Langmuir waves with ion-sound waves （l ＋ s → t） in a source related to shock fronts in the reconnection region.

关键词： solar flare -- radio emission -- spike-bursts

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Flare evolution and polarization changes in fine structures of solar radio emission in the 2013 April 11 event

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Research in Astronomy and Astrophysics 2016年第2期16卷 69-80页

作者： Gennady chernov Robert Sych Bao-Lin Tan Yi-Hua Yan Cheng-Ming Tan Qi-Jun Fu Marian Karlicky Valery Fomichev Key Laboratory of Solar Activity National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100012China Pushkov Institute of Terrestrial Magnetism Ionosphere and Radio Wave PropagationRussian Academy of Sciences(IZMIRAN)TroitskMoscow region142190Russia Yunnan Observatories Chinese Academy of SciencesKunming 650011China Institute of Solar-Terrestrial Physics Russian Academy of SciencesSiberian BranchIrkutsk 664033Russia Astronomical Institute of the Academy of Sciences of the Czech Republic Ondrejov 15165Czech Republic

The measurement of positions and sizes of radio sources in observations is important for un- derstanding of the flare evolution. For the first time, solar radio spectral fine structures in an M6.5 flare that occurred on 2013 April 11 were observed simultaneously by several radio instruments at four different observatories： Chinese Solar Broadband Radio Spectrometer at Huairou （SBRS/Huairou）, Ondrejov Radio Spectrograph in the Czech Republic （ORSC/Ondrejov）, Badary Broadband Microwave Spectropolarimeter （BMS/Irkutsk）, and spectrograph/IZMIRAN （Moscow, Troitsk）. The fine structures included microwave zebra patterns （ZPs）, fast pulsations and fiber bursts. They were observed during the flare brightening lo- cated at the tops of a loop arcade as shown in images taken by the extreme ultraviolet （EUV） telescope onboard NASA＇s satellite Solar Dynamics Observatory （SDO）. The flare occurred at 06：58-07：26 UT in solar active region NOAA 11719 located close to the solar disk center. ZPs appeared near high frequency boundaries of the pulsations, and their spectra observed in Huairou and Ondrejov agreed with each other in terms of details. At the beginning of the flare＇s impulsive phase, a strong narrowband ZP burst occurred with a moderate left-handed circular polarization. Then a series of pulsations and ZPs were observed in almost unpolarized emission. After 07：00 UT a ZP appeared with a moderate right-handed polarization. In the flare decay phase （at about 07：25 UT）, ZPs and fiber bursts become strongly right-hand polarized. BMS/Irkutsk spectral observations indicated that the background emission showed a left-handed circular polarization （similar to SBRS/Huairou spectra around 3 GHz）. However, the fine structure appeared in the right-handed polarization. The dynamics of the polarization was associated with the motion of the flare ex- citer, which was observed in EUV images at 171 A and 131 A by the SDO Atmospheric Imaging Assembly （AIA）. Combining magnetograms observed by t

关键词： Sun activity -- Sun flares -- Sun particle emission -- Sun radio radiation -- zebra-pattern

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The Strength of Intermolecular Contact in Protein Crystals

The Strength of Intermolecular Contact in Protein Crystals

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5th China-Japan Workshop on Microgravity Sciences

作者： Y.MATSUURA A.a.chernov Institute for Protein Research Osaka University Suita Osaka 565-0871 Japan MSFC/NASA Huntsville AL 35812 USA Institute for Protein Research Osaka University Suita Osaka 565-0871 Japan MSFC/NASA Huntsville AL 35812 USA

＜正＞ In protein crystals, which usually contain 30 to 70 % volume of water, protein molecules form intermolecular contacts of various strengths depending on the nature of the molecules and crystal systems. The intermolecular contact （macrobond） is composed of characteristic combination of various intermolecular interactions consisting of several types of elementary non-covalent bonds, such as hydrogen bond （frequently involving water molecules）, ionic, and van der Waals. We have been studying the correlation between morphology and macrobond strengths essentially in an approach similar to the periodic-bond-chain （PBC） analyses [1,2].

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软土地基上地表建筑系统的强震反应(英文)

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西北地震学报 2005年第1期27卷 30-35页

作者： POTAPOV V.A. chernov E.A 俄罗斯科学院西伯利亚分院地壳研究所伊尔库茨克格勃64033俄罗斯

本文导出了一种给出相对烈度在lg R^0之间的收敛解(忽略震级)的小震方程式。结合在贝加尔地区岩石抗震特性调查与文字资料和统一理论,使人们可对震源等势面进行评估。确定了在震源区边界处的地震烈度稳定性和弹性波在地壳中的传播,使得... 详细信息

本文导出了一种给出相对烈度在lg R^0之间的收敛解(忽略震级)的小震方程式。结合在贝加尔地区岩石抗震特性调查与文字资料和统一理论,使人们可对震源等势面进行评估。确定了在震源区边界处的地震烈度稳定性和弹性波在地壳中的传播,使得推导出从地震主要参数震级向随震中距不同的烈度定量计算的转换成为可能。获得了烈度(能通量的密度)对距离的双线性相关,给出了能通量密度和相对烈度之间的关系。求出了取决于地表建筑地基的物理特性的振动载荷烈度。在地震学角度,这种强震的定量预测方法是一种提供详细地震区划和场地小区划的可能手段之一。

关键词：地震烈度地震反应抗震

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The comparison of intravenous and lymphotropic routes of <sup>99m</sup>Tc ciprofloxacin in experimental pulmonary suppuration

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Health 2011年第11期3卷 663-667页

作者： Yuriy Lishmanov Svetlana Sazonova Yevgeny Sokolovich Vladimir chernov 不详

Intravenously injected “99mTc-ciprofloxacin” is rapidly accumulated and washed from the septic focus. Lymphotropic injections provide targeted and long-lasting effect of antibiotics. After injection into the interspinous ligament the drug slowly enters the inflammation area (by-passing the urinary organs and liver), where it is maximally accumulated only after 24 h, which allows to reduce the number of injections and the total dose of the antibiotic.

关键词： Pulmonary Suppuration Lymphotropic Route 99mTc Ciprofloxacin

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