ELF emission generated by the HAARP HF-heater using varying frequency and polarization

We present first observations of the ELF emission generated by the modulated ionospheric HF-heating using the HAARP facility. We focus primarily on the dependence of the polarization and of the amplitude of the ELF wave upon the frequency and polarization of the heating radio wave. A simple 1D computational model of the ELF generation based on the earlier developed model of a horizontal magnetic dipole caused by the HF ionospheric heating [1] is presented. The model develops a qualitative understanding of the changes in the ELF amplitude and polarization due to variations of the heating frequency. The obtained results imply that polarization of the ELF emission generated by the ionospheric HF-heating can be controlled by changing the frequency or polarization of the radio wave. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 42, No. 8, pp. 728–735, August 1999.     

The moon as a cosmic source of linearly polarized radio emission

We analyze parameters of the partially linearly polarized thermal radio emission from the Moon taking the effects of radiative heat transfer and surface roughness into account. The distributions of the Stokes parameters I, Q, and U over the visible lunar disk are considered. The polarization parameters of the integral radio emission as functions of the frequency and the Moon phase are obtained by integrating the Q and U distributions. We consider the possibility of using the Moon as a reference source of partially linearly polarized radiation for space-borne and ground-based projects aimed at studying polarization of the Galactic radio emission and the cosmic microwave background. __________ Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 50, No. 7, pp. 593–606, July 2007.     

Electron acceleration and type II radio emission at quasi-parallel shock waves

Solar type II radio bursts are interpreted as the radio signature of shock waves travelling through the solar corona. Some of these shock waves are able to enter into the interplanetary medium and are observed as interplanetary type II bursts. The nonthermal radio emission of these bursts indicates that electrons are accelerated up to superthermal and/or relativistic velocities at the corresponding shocks. Plasma wave measurements at interplanetary shock waves support the assumption that the fundamental type II radio emission is generated by wave-wave interactions of electron plasma waves and ion acoustic waves and that the source region is located near the transition region of the shock. Therefore, the instantaneous bandwidth of type II bursts should reflect the density jump across the shock. Comparing the theoretically predicted density jump of coronal shock waves (Rankine-Hugoniot relations) and the measured instantaneous bandwidth of solar type II radio bursts it is appropriate to assume that these bursts are generated by weak supercritical quasi-parallel shock waves. Two different mechanisms for the accelaration of electrons at this kind of shock waves are investigated in the form of test particle calculations in given magnetic and electric fields. These fields have been extracted from in-situ measurements at the quasi-parallel region at Earth’s bow shock, which showed large amplitude magnetic field fluctuations (so-called SLAMS: Short Large Amplitude Magnetic Field Structures) as constituent parts. The first mechanism treats these structures as strong magnetic mirrors, at which charged particles are reflected and accelerated. Thus, thermal electrons gain energy due to multiple reflections between two approaching SLAMS. The second mechanism shows that it is possible to accelerate electrons inside a single SLAMS due to a noncoplanar component of the magnetic field in these structures. Both mechanism are described in the form of test particle calculations, which are supplemented by calculations according to adiabatic theory. The results are discussed for circumstances in the solar corona and in interplanetary space. Astrophysikalisches Institut, Observatorium für solare Radioastronomie, Potsdam, Germany. Published from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 41, No. 1, pp. 84–104, January, 1998.     

Electron acceleration and type II radio emission at quasi-parallel shock waves

Solar type II radio bursts are interpreted as the radio signature of shock waves travelling through the solar corona. Some of these shock waves are able to enter into the interplanetary medium and are observed as interplanetary type II bursts. The nonthermal radio emission of these bursts indicates that electrons are accelerated up to superthermal and/or relativistic velocities at the corresponding shocks. Plasma wave measurements at interplanetary shock waves support the assumption that the fundamental type II radio emission is generated by wave-wave interactions of electron plasma waves and ion acoustic waves and that the source region is located near the transition region of the shock. Therefore, the instantaneous bandwidth of type II bursts should reflect the density jump across the shock. Comparing the theoretically predicted density jump of coronal shock waves (Rankine-Hugoniot relations) and the measured instantaneous bandwidth of solar type II radio bursts it is appropriate to assume that these bursts are generated by weak supercritical quasi-parallel shock waves. Two different mechanisms for the accelaration of electrons at this kind of shock waves are investigated in the form of test particle calculations in given magnetic and electric fields. These fields have been extracted from in-situ measurements at the quasi-parallel region at Earth’s bow shock, which showed large amplitude magnetic field fluctuations (so-called SLAMS: Short Large Amplitude Magnetic Field Structures) as constituent parts. The first mechanism treats these structures as strong magnetic mirrors, at which charged particles are reflected and accelerated. Thus, thermal electrons gain energy due to multiple reflections between two approaching SLAMS. The second mechanism shows that it is possible to accelerate electrons inside a single SLAMS due to a noncoplanar component of the magnetic field in these structures. Both mechanism are described in the form of test particle calculations, which are supplemented by calculations according to adiabatic theory. The results are discussed for circumstances in the solar corona and in interplanetary space.     

Spectral peculiarities of high energy X-ray radiation,gamma radiation,and Submillimeter radio emission in the impulsive phase of a solar flare

We analyze experimental data on the temporal behavior of fluxes and energy spectra of hard solar X-ray and gamma radiation in the energy range of 0.015 to 300 MeV, obtained onboard the CORONAS-F satellite during a solar flare on August 25, 2001. These data are compared with measurements of the radio emission fluxes over the wide frequency range of 1–405 GHz. For our analysis, we use data obtained onboard the YOHKOH, TRACE and GOES satellites, along with ground-based observations of this solar event using the Solar Submillimeter Telescope (SST; Argentina). For the first time, we find nearly simultaneous changes in the energy spectra of gamma radiation over the range 10–150 MeV and the frequency spectrum of radio emission at the beginning and during a impulsive phase of this event (whose duration did not exceed three minutes).     

Radio emission structure of cloud-to-ground lightning discharge

Cloud-to-ground lightning discharge radio frequency emission is analysed on the base of measurements with high temporal resolution allowed to fully resolve its structure. Discharge radio emission mainly consists of independent random bi-polar pulses. Pulse length, amplitude and interpulse period distributions are studied at different stages of lightning discharge. The significant change of radio frequency emission structure during discharge development is demonstrated.     

Spatial-frequency characteristics of radio emission induced by interaction of an extensive air shower with the Earth’s surface

The spatial directional pattern of the radio emission induced by interaction of the excess electrons of an extensive air shower with the Earth’s surface was found in the approximation of perfect soil conductance. The results made it possible to determine the frequency range (≈0.2–1 MHz), within which the radio emission of the shower is maximum, provided that this emission mechanism is valid. In addition, it became possible to explain the previously observed lack of direct proportionality between the shower energy and the radio signal amplitude. It was found that this disproportionality is caused mainly by the high directivity of low-frequency (0.2–3 MHz) radiation patterns within a wide range of the values of the axial tilt.     

电子束驱动的回旋激射不稳定性进一步的数值研究

鉴于近来发现的弱相对论性电子束驱动的回旋激射(maser)不稳定性在太阳射电发射中的重 要应用，在Chen等的理论模型的基础上，对回旋激射不稳定性主要特征在更广泛的参数范围 内进行了进一步的深入研究，丰富了此类等离子体不稳定性的基本内容，而且预期在天体射 电发射机理的研究中也将得到更广泛的应用. 关键词： 回旋激射不稳定性 弱相对论性电子束 增长率     

Manifestations of the 5-Min Photospheric Oscillations in the Solar Microwave Emission

Dynamic spectra of low-frequency (LF) modulation of microwave emission during solar flares are obtained. Observation data for five radio bursts at frequency 37 GHz recorded by a 14-m Metsäahovi observatory (Finland) radiotelescope in the period from 1990 to 1993 were used. Frequency modulation of the radio emission intensity with the average period 296±37 (1) s, which is close to the period of well-known photospheric oscillations, was observed. Possible mechanisms of photospheric oscillation influence on the regions of radio burst generation are discussed.     

Features of Short-Period Oscillations of Microwave Emission from the Solar Active Region before the Flare

The radiation of microwave sources above sunspots at a frequency of 17 GHz gives information about the parameters of solar plasma in the regions where the magneti-field strength is B ~ 2000 G in the transition region between the chromosphere and corona. Short-period oscillations (with a period of several minutes) of microwave emission from solar active regions (ARs) reflect wave processes in magnetic flux tubes of sunspots. Short-period oscillations of microwave emission from AR NOAA 12242 before two flares on December 17, 2014 are analyzed. This analysis is based on solar radio images obtained by means of the Nobeyama Radio Heliograph with a 10″?15″ two-dimensional spatial resolution. The radio maps of the whole solar disk were synthesized in a nonstandard mode with a cadence of 10 s and an averaging time of 10 s. An increase in the power of about ten-minute oscillations of microwave radiation approximately 40 to 50 min before the M1.5 flare (01: 00 UT) is found. On the same day, an increase in the power of ten-minute oscillations is observed about 60 min before the M8.7 flare (04: 42 UT). This effect is similar to the effect found earlier by two groups of authors independently for three-minute oscillations—namely, they observed a sharp increase in three-minute oscillations 15 to 20 min before the radio burst accompanying the flare. The effect in question may be interpreted as an relationship ofMHD waves propagating along the magnetic flux tube of a sunspot and the onset of the solar flare.     

Electromagnetically Induced Transparency and Absorption of A Monochromatic Light Controlled by a Radio Frequency Field

Electromagnetically induced transparency and absorption of a monochromatic light controlled by a radio frequency field in the cold multi-Zeeman-sublevel atoms are theoretically investigated. These Zeeman sublevels are coupled by a radio frequency(RF) field. Both electromagnetically induced transparency and electromagnetically induced absorption can be obtained by tuning the frequency of RF field for both the linear polarization and elliptical polarization monochromatic lights. When the transfer of coherence via spontaneous emission from the excited state to the ground state is considered, electromagnetically induced absorption can be changed into electromagnetically induced transparency with the change of intensity of radio field. The transparency windows controlled by the RF field can have potential applications in the magnetic-field measurement and quantum information processing.     

Effect of limiting polarization in the Jovian inner magnetosphere

Jovian decameter emission is known to exhibit almost total polarization. We consider the elliptical polarization to be a consequence of linear-mode coupling in the Jovian magnetosphere outside the source region. We determine conditions of emission propagation along the ray path that are necessary for self-consistent explanatation of the polarization observations and show that the ellipticity (axial ratio of the polarization ellipse) is determined by the magnetospheric plasma density n_e in a small region a distance of about half the Jovian radius from the radiation source. The plasma density in the region is quite low, n_e<0.4 cm⁻³, and the geometrical-optics approximation of emssion propagation in front of the region converts to the vacuum approximation behind it. The latter means that the linear-mode coupling in the Jovian inner magnetosphere is manifested as the effect of limiting polarization. Sources of decameter emission emitting at different frequencies f are located at heights corresponding to gyrofrequency levels f _Be ≅f and at magnetic-force lines that belong to L-shells passing through the satellite Io. The location of the transitional region in the Jovian magnetosphere varies depending on the emission frequency and the time. For each given decameter radio emission storm occupying some region in frequencytime space, we have a number of transitional regions located in a certain region of the Jovian magnetosphere—the interaction region of the magnetosphere (IRM) for the given emission storm. The distribution of magnetospheric plasma in an IRM is found from data of observations of the polarization ellipiicity of the given decameter radio emission storm. By matching the calculated ellipticity of emission with the observed ellipticity at every point of frequency-time space of the emission dynamic spectrum one finds a recurrent relation between the local values of the magnetospheric plasma density N_c and the planetary magnetic field B in the IRM, which allows evaluation of the distribution of plasma density if a definite model of the Jovian magnetic field has been adopted. Institute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod, Russia; Space Research Institute, Austrian Academy of Sciences, Austria. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 41, No. 2, pp. 177–193, February, 1998.     

RT-2 radio telescope of the Ussuriysk Astrophysical Observatory: current state and observation data

An RT-2 radio telescope of the Ussuriysk Astrophysical Observatory (UAO) is intended for measuring the total flux of solar radio emission at a frequency of 2.804 GHz. Regular observations have been carried out in the UAO since 1990. The current state of the instrument and the data survey for the observation years are presented. The emphasis is on the transition to digital registration of the radio flux in 2002, which offers new opportunities of the data analysis. Digital recording allows us to improve the accuracy of the daily radio-flux measurements, ensures their comparison with the data of the integral radio emission at other frequencies, and provides for reconstruction of the time profiles of powerful radio bursts. Possible problems which can be solved using the UAO radiometer data are outlined. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 51, No. 12, pp. 1005–1010, December 2008.     

Prevalence of the Ordinary Mode in Microwave Radio Emission from Solar Active Regions

We propose an interpretation of some observations of the ordinary (o) mode in the microwave emission of slowly-varying (s) radio sources associated with active regions in the solar atmosphere. As a rule, the extraordinary (e) mode dominates in the s-component, which is fully explained by the generally accepted theory of its origin. This theory is based on the cyclotron and bremsstrahlung mechanisms of radiation of thermal electrons in an inhomogeneous plasma of the solar atmosphere above sunspots, where the magnetic field decreases and the kinetic temperature increases with height. It is shown in this work that the prevalence of the ordinary mode is due most probably to the presence of a region with a negative gradient of the kinetic temperature in the atmosphere above the sunspot. We analyze the qualitative frequency dependences of the brightness temperature and polarization of the radiation of a hot and cold (compared to the ambient plasma) filament in the s-component source, as well as the possible reasons for the polarization reversal at a certain frequency. Special attention is paid to the active region NOAA 4741 with the unipolar sunspot described in [1, 2]. Criteria permitting one to judge which of two effects (linear wave coupling or presence of a region with a negative temperature gradient) is responsible for the o-mode in the s-component are discussed.     

射频场控制的磁子能级中单色激光吸收抑制

理论上研究了射频场作用下多塞曼能级系统中单色激光的吸收抑制现象.一束单色线偏振或者椭圆偏振的激光作用于铷原子两能级间,线或椭圆偏振矢量方向与磁场方向垂直.在磁场中冷铷原子能级发生分裂,通过一个射频场将这些磁子能级耦合起来.当扫描射频场频率时,计算表明原子对单色光的吸收谱中出现了透射峰,类似于电磁诱导透明现象,光吸收减弱,光场透射增强.对于线性偏振或者椭圆偏振的单色光均能得到透射增强的结果 .这种现象完全不同于通常光泵磁共振实验中射频场与磁子能级谐振时光被吸收最多的现象.这种扫描射频场频率时单色光的透射增强现象来自于磁子能级间的相干效应.计算表明在扫描射频场频率时单色光吸收谱中出现的透射峰与射频场的拉比频率和椭圆偏振光的左旋和右旋圆偏振成分相关.这种射频场控制的单色光透射增强效应在磁场测量,光信息处理等领域有潜在的应用价值.     

射频场控制的磁子能级中单色激光吸收抑制

理论上研究了射频场作用下多塞曼能级系统中单色激光的吸收抑制现象.一束单色线偏振或者椭圆偏振的激光作用于铷原子两能级间,线或椭圆偏振矢量方向与磁场方向垂直.在磁场中冷铷原子能级发生分裂,通过一个射频场将这些磁子能级耦合起来.当扫描射频场频率时,计算表明原子对单色光的吸收谱中出现了透射峰,类似于电磁诱导透明现象,光吸收减弱,光场透射增强.对于线性偏振或者椭圆偏振的单色光均能得到透射增强的结果.这种现象完全不同于通常光泵磁共振实验中射频场与磁子能级谐振时光被吸收最多的现象.这种扫描射频场频率时单色光的透射增强现象来自于磁子能级间的相干效应.计算表明在扫描射频场频率时单色光吸收谱中出现的透射峰与射频场的拉比频率和椭圆偏振光的左旋和右旋圆偏振成分相关.这种射频场控制的单色光透射增强效应在磁场测量,光信息处理等领域有潜在的应用价值.     

Electroluminescence study of polarization changes in lead magnoniobate crystals in pulsed electric fields

Electroluminescence is used to study changes in the polarization of crystals of a model ferroelectric relaxor, lead magnoniobate (PMN), in pulsed electric fields. The amplitude of the electoluminescence pulses produced during polarization and depolarization of PMN crystals is found to depend on the duration of the applied electric field pulses if this duration is shorter than the most probable time for polarization buildup. These data provide evidence of rapid changes in the polarization through realignment of the domain and heterophase structure at temperatures above the temperature for destruction of the induced macrodomain ferroelectric phase and evidence of an “excited” polarization state for short-lived pulses whose decay is accompanied by an enhancement in the amplitude of the depolarizing luminescence pulse and by a reduction in the time delay of its emission following the end of the field pulse. Fiz. Tverd. Tela (St. Petersburg) 39, 341–343 (February 1997)     

Numerical simulations of type-III solar radio bursts

The first numerical simulations are presented for type-III solar radio bursts in the inhomogeneous solar corona and interplanetary space, that include microscale quasilinear and nonlinear processes, intermediate-scale driven ambient density fluctuations, and large scale evolution of electron beams, Langmuir and ion sound waves, and fundamental and harmonic electromagnetic emission. Bidirectional coronal emission is asymmetric between the upward and downward directions, and harmonic emission dominates fundamental emission. In interplanetary space, fundamental and/or harmonic emission can be important. Langmuir and ion sound waves are bursty and the statistics of Langmuir wave energy agree well with the predictions of stochastic growth theory.     

Calibration of the solar radio spectrometer

This paper shows some improvements and new results of calibration of Chinese solar radio spectrometer by analyzing the daily calibration data recorded in the period of 1997–2007. First, the calibration coefficient is fitted for three bands (1.0–2.0 GHz, 2.6–3.8 GHz, 5.2–7.6 GHz) of the spectrometer by using the moving-average method confined by the property of the daily calibration data. By this calibration coefficient, the standard deviation of the calibration result was less than 10 sfu for 95% frequencies of 2.6–3.8 GHz band in 2003. This result is better than that calibrated with the constant coefficient. Second, the calibration coefficient is found in good correlation with local air temperature for most frequencies of 2.6–3.8 GHz band. Moreover, these results are helpful in the research of the quiet solar radio emission.     

The line emissions and polarization in blazars

The correlations between broad-line emission,polarization,and core-dominance parameters are investigated for a sample of 148 blazars(BL Lacertae objects-BLs and flat spectrum radio quasars-FSRQs). An anti-correlation between the broad-line luminosity and the linear polarization is found. The broad-line and polarization relation can be explained by using a relativistic beaming model,which perhaps suggests that BL Lacs and FSRQs are a single class. We also investigated the relation between the ratio of the broad-line luminosity to the Eddington luminosity and linear polarization,and that between the ratio of the broad-line luminosity to the Eddington luminosity and the core-dominance parameter.