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本文采用等离子体动力学方法，研究了日冕条件下磁化非相对论热等离子体对太阳射电辐射产生的电子回旋共振吸收，并在辐射频率等于电子回旋谐波频率时求得ｎ≥２谐波吸收率的近似表示式，以及其对等离子体温度，出射角度和谐波数的变化规律，在应用部分，讨论了电子回旋共振吸收对于太阳射电尖峰爆发的影响，认为目前观测到的尖峰爆，大多数高能电子束来自日冕的内层。 相似文献
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射电观测是太阳物理和日地空间科学的重要探测手段,尤其是对于太阳爆发过程中的太阳非热粒子加速、发射和传播等过程.迄今,世界各地研制建成了上百台太阳射电望远镜,包括射电流量计、射电动态频谱仪和射电日像仪等.基于技术进步和新的科学设想,人们还在不断提出新的太阳射电望远镜计划.研制新的太阳射电望远镜时,需要考虑观测频率、带宽、时间分辨率、频率分辨率、空间分辨率、偏振精度等设计参数.事实上,过度追求高参数往往会无法实现期望的科学目标.如何合理地选择太阳射电望远镜的参数呢?长期的观测研究发现太阳射电爆发常常可分成一系列从长到短不同时标的爆发过程,其中,尖峰爆发是最小时间尺度的爆发现象,同时也是太阳上目前发现的最小空间尺度上的爆发过程,可看成一种元爆发过程,可能对应于单一的磁场重联和磁能释放.根据太阳射电天文学研究,识别尖峰爆发是对新一代太阳射电望远镜的基本要求.尖峰爆发的时间尺度和空间尺度又是随频率而变化的.从分析不同频段太阳射电尖峰爆发的时间和带宽的标度律来说明如何为新一代望远镜的设计选择合理的参数指标,并提出谱-像结合观测模式,最大程度地保证望远镜科学目标的实现.这种观测模式或将成为未来太阳射电观测的主要方式,对揭示太阳爆发现象中的非热过程的物理本质具有非常重要的意义. 相似文献
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本文在电子回旋脉塞不稳定性理论的基础上,着重讨论了等离子体背景参数ω_(pe)/Ω_e对尖峰辐射性质的影响,内容包括:该参数的物理意义、取值范围,以及在尖峰辐射性质中,对ω_(pe)/Ω_e的变化比较敏感的偏振和谐波结构,等等。 相似文献
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本文介绍用“三波段太阳射电高时间分辨率同步观测系统”所观测到的1988年12月16日三波段(1420MHz、2840MHz、4000MHz)太阳射电大爆发中毫秒级精细结构的观测特征,指出太阳射电快速活动在射电爆发的不同阶段具有不同的特征,首先在爆发的上升沿出现2840MHz的毫秒尖峰辐射群,继而在1420MHz上出现毫秒级尖峰辐射群,并且还在以后的几个爆发次峰上陆续出现,在长达两小时的大爆发过程中,在4000MHz上始终未产生毫秒级尖峰辐射,这也反应了射电尖峰辐射现象存在着一定的带宽。特别引起注意的是毫秒级尖峰辐射群均出现在射电爆发的峰值附近,在其它时间的记录中尚未发现毫秒尖峰辐射。 三波段的秒级射电爆发曲线如图1所示。毫秒级精细结构如图2所示。由图2可见,单个尖峰辐射的持续随频率的减小而增加,2840MHz多为10—20ms,1420MHz多为30—170ms;所产生的尖峰辐射群强度不大,而且很少有孤立的尖峰;2840MHz尖峰辐射的强度一般为450—900sfu,1420MHz一般为500—1770sfu(1sfu=10~(-22)WM~(-2)Hz~(-1));还特别引起注意的是在2840MHz上当所出现的尖峰辐射群结束时,往往出现持续时间为100ms的流量下降现象,(此种现象在以往的观测中未曾见过),详见图2b和2c;关于事件尖峰辐射的丰度,仅对几个尖峰辐射群作了统计如下: 在1420M 相似文献
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本文利用10米天线上21cmms级连续无间隙快速记录系统,在第22周太阳峰年期间观测到大量的分米波段的太阳射电尖峰辐射的快速活动资料,对这些资料进行分析、比对发现尖峰辐射的快速活动至少包括：毛刺型、缓变型、缓变脉冲型、脉冲型、开关型．同时也对太阳射电尖峰辐射与其它共生现象进行分析,并对尖峰辐射的形态进行了简单的讨论． 相似文献
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本文分析了云南天文台四波段快速采样射电望远镜在1990年1月至1991年3月间记录到的毫秒级尖峰辐射事件。结合此期间S.G.D.公布的米波射电大爆发资料,给出了毫秒级尖峰辐射的各种特征,总结出毫秒级尖峰辐射同Ⅲ型、Ⅱ型和Ⅳ型太阳射电爆发的关系,最后做出了相应的解释和讨论。 相似文献
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Chian Abraham C.-L. Abalde JOSÉ R. Alves M. Virginia Lopes Sergio R. 《Solar physics》1997,173(1):199-202
It is shown that narrow-band radio bursts of right- and left-hand circular polarizations from the Sun and flare stars can be produced via nonlinear conversion of Langmuir waves into high-frequency electromagnetic electron cyclotron waves near the plasma frequency by coupling to low-frequency electromagnetic cyclotron waves such as Alfvén-ion cyclotron or magnetosonic-whistler waves. 相似文献
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V. V. Zheleznyakov 《Astrophysics and Space Science》1983,97(2):229-259
The influence of radiation on the electron velocity distribution in a hot nonrelativistic plasma localized near the surface of magnetic white dwarfs is investigated. The part played by the plasma in the formation of cyclotron features in the optical spectrum of these stars is studied. The region of parameters where the transverse temperature of plasma is defined by the brightness temperature of extraordinary radiation at the gyrofrequency is found. When escaping from the plasma in a homogeneous magnetic field, this component forms a cyclotron line in absorption. The ordinary radiation at the gyrofrequency and both modes at higher cyclotron harmonics are in emission or absorption depending on the magnetic field strength and hot plasma density. Possible interpretation of the observed spectral features of magnetic white dwarfs in terms of the developed theory is discussed. 相似文献
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Location and parameters of a microwave millisecond spike event 总被引：1，自引：0，他引：1
A typical microwave millisecond spike event on November 2, 1997 was observed by the radio spectrograph of National Astronomical
Observatories (NAOs) at 2.6–3.8 GHz with high time and frequency resolution. This event was also recorded by Nobeyama Radio
Polarimeters (NoRP) at 1–35 GHz and Radio Heliograph (NoRH) at 17 GHz. The source at 17 GHz is located in one foot-point of
a small bright coronal loop of YOHKOH SXT and SOHO EIT images with strong photospheric magnetic field in SOHO MDI magnetograph.
It is assumed that the electron cyclotron maser instability and gyro-resonance absorption dominate, respectively, the rising
and decay phase of the spike event. For different harmonic number of gyro-frequency or magnetic field strength, a fitting
program with free plasma parameters is used to minimize the difference between the observational and theoretical values of
the exponential growth and decay rates for a given spike. The plasma parameters at third harmonic number are more comparable
to their typical values in solar corona. Hence, it is able to provide a diagnosis for the source parameters (magnetic field,
density, and temperature), the properties of radiations (wave vector and propagation angle), and the properties of non-thermal
electrons (density, pitch angle, and energy). The results are also comparable with the diagnosis of the gyro-synchrotron radiation
model, the frequency drift rates and a dipole magnetic field model, as well as the YOHKOH SXT and SOHO MDI data.
This study is supported by the NFSC project nos. 10333030 and 10273025, and “973” program with no. G2000078403. 相似文献
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Spectropolarimetric features of thermal cyclotron radiation of solar coronal loops and the possibility of interpretation of the observed reversal of the sense of polarization of centimeter and decimeter waves are discussed. To this end, thermal cyclotron radiation is computed in terms of the simplest model of a three-dimensional hot loop (a half-torus). Such a loop is shown to be capable of changing appreciably the properties of the radiation of a solar active region at centimeter and decimeter wavelengths. A detailed analysis is performed to determine the conditions under which the radiation spectrum of an active region containing a coronal loop may have a complex pattern with several maxima or relatively narrow-band cyclotron lines, and the sense of polarization may change several times in the wavelength interval considered. These conditions are modelled by such parameters as the structure of the magnetic field, electron density, and size of the loop. The results of the computations of two-dimensional brightness temperature distributions at different wavelengths for ordinary and extraordinary waves at fixed points of the loop and the integrated parameters of the flux and polarization of radiation in terms of the model discussed are reported. Cases are considered where the line of sight is crossed by one or two loops. The expected distribution of polarization across the source in the model considered is compared to the results of RATAN-600 observations of the solar active region AR 7962 made on May 12–14, 1996. 相似文献
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A theoretical study is made of the whistler mode cyclotron instability both in linear and nonlinear regimes in conjunction with the generation of VLF emissions in the magnetosphere. For the nonlinear treatment, a well-established quasilinear method is used and some physical processes of the cyclotron instability viz. energy conservation, mechanism of instability and frequency change of the excited emissions are clarified. The results are applied to some types of the triggered VLF emissions; whistler triggered emissions and artificially stimulated emissions (ASE). It is found that whistler triggered emissions excited around the upper cutoff frequencies of whistlers may be explained by the whistler mode cyclotron instability by a model distribution function inferred from satellite data. In order to see a nonlinear evolution of the whistler mode cyclotron instability, computer simulations were carried out and it is shown that the change of frequency with time of whistler triggered emissions as well as characteristics of ASE are well explained by resonant nonlinear behaviour of whistler mode cyclotron instability considered in the present paper. 相似文献
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An analytical derivation is given of possible electron instabilities in the solar wind, related to the observed forms of the electron distribution functions. The instabilities refer to the frequency regime intermediate between ion and electron cyclotron frequencies. Instability criteria are discussed in terms of the various parameters which have been measured by different solar wind experiments. 相似文献
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We present our calculations of the expected characteristics of the integrated spectrum of thermal cyclotron radiation from a solar active region with a coronal magnetic loop. A hot torus is considered as a three-dimensional loop model. We show that the hot-loop emission can change appreciably the emission characteristics of the active region at centimeter and decimeter wavelengths. At certain loop parameters, the emission frequency spectrum can have a nonmonotonic and complex pattern with several peaks or contain narrow-band cyclotron lines. The polarization structure of the source with a hot loop is also complex and the polarization is repeatedly reversed over the observed frequency range under certain conditions. The revealed spectral-polarization peculiarities are considered from the standpoint of whether some atypical observed properties of the emission sources associated with solar active regions can be explained. 相似文献
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We consider the transfer of radiation and calculate the force of its pressure in the electron gyroresonance line in the atmospheres of magnetic degenerate stars. We specify the atmospheric parameters for which an outflow of plasma is possible under radiation pressure in the cyclotron line. We show that the permittivity tensor of a mildly relativistic plasma in a strong magnetic field found by applying relativistic corrections to the cyclotron resonance condition and by taking into account the vacuum polarization and recoil effects during photon scattering should be used to obtain proper results. We have determined the real and imaginary parts of the refractive indices and the polarization coefficients for normal electromagnetic waves when scattering dominates over absorption. Relativistic effects, which change greatly the dispersion and resonant absorption of waves propagating almost perpendicular to the magnetic field, and vacuum polarization have been found to change qualitatively the gyroresonance radiation spectrum and pressure for a wide range of parameters of stellar magnetospheres. 相似文献
19.
The absorption coefficients for extraordinary and ordinary electromagnetic modes are found for a tenuous hot magnetized plasma, taking into account the collisions between plasma particles and the scattering of photons. An approach is suggested which generalizes collisionless and cold-plasma approximations. The simple formulae obtained are valid both near, and at a distance from, the cyclotron harmonics. In particular, the ordinary mode is shown to have resonance at the cyclotron frequency. The number of noticeable reasonances of absorption coefficient at cyclotron harmonics is estimated for both modes.Using the coefficients obtained, the intensity, Stokes parameters and polarization of radiation of a homogeneous plasma slab are calculated for conditions which may be realized in the heated regions of accreted plasma in an AM Herculis-type system. The large difference between the absorption coefficient of extra-ordinary and ordinary modes near the cyclotron harmonics may result in the emission of the broad polarized continuum together with the narrow cyclotron lines. The polarization of these lines has a complicated spectral dependence.The results obtained are shown to be useful for explaining the main properties of AM Herculistype objects. 相似文献
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V. V. Zheleznyakov 《Astrophysics and Space Science》1981,77(2):279-297
The origin of hard X-ray spectrum (continuum and cyclotron lines) of pulsars in binary systems is discussed. A model of the polar region of a neutron star consisting of a hot spot in a dense plasma atmosphere with a quasi-homogeneous magnetic field and an extended accreting column in an inhomogeneous dipolar field is investigated. In the hot spot bremsstrahlung and Thomson scattering form continuum radiation, while bremsstrahlung and cyclotron scattering produce the absorption cyclotron lines. By the observed continuum intensity one can estimate the maximum distances to pulsars. Cyclotron scattering in gyro-resonant layers localized in the accreting column leads to a general attenuation of the radiation of a hot spot, but is unable to ensure the formation of cyclotron lines. For strong accretion the hot spot radiation becomes insignificant, the lines disappear and the pulsating component of an X-ray pulsar is produced by the accreting column bremsstrahlung transformed by Thomson scattering. 相似文献