Effects of a kappa distribution function of electrons on incoherent scatter spectra   总被引：2，自引：0，他引：2  

S. Saito  F. R. E. Forme  S. C. Buchert  S. Nozawa  R. Fujii 《Annales Geophysicae》2000,18(9):1216-1223

In usual incoherent scatter data analysis, the plasma distribution function is assumed to be Maxwellian. In space plasmas, however, distribution functions with a high energy tail which can be well modeled by a generalized Lorentzian distribution function with spectral index kappa (kappa distribution) have been observed. We have theoretically calculated incoherent scatter spectra for a plasma that consists of electrons with kappa distribution function and ions with Maxwellian neglecting the effects of the magnetic field and collisions. The ion line spectra have a double-humped shape similar to those from a Maxwellian plasma. The electron temperatures are underestimated, however, by up to 40% when interpreted assuming Maxwellian distribution. Ion temperatures and electron densities are affected little. Accordingly, actual electron temperatures might be underestimated when an energy input maintaining a high energy tail exists. We have also calculated plasma lines with the kappa distribution function. They are enhanced in total strength, and the peak frequencies appear to be slightly shifted to the transmitter frequency compared to the peak frequencies for a Maxwellian distribution. The damping rate depends on the electron temperature. For lower electron temperatures, plasma lines for electrons with a distribution function are more strongly damped than for a Maxwellian distribution. For higher electron temperatures, however, they have a relatively sharp peak.  相似文献   

GRAPES模式不同云物理方案对短期气候模拟的影响   总被引：10，自引：3，他引：10  

章建成  刘奇俊 《气象》2006,32(7):3-12

在胡志晋、刘奇俊云物理方案的基础上，研制了GRAPES模式的云降水显式方案。用不同云物理方案开展了短期气候（月尺度）过程的模拟试验，并与地面观测资料和NECP再分析资料进行了对比分析。模拟的结果表明，耦合了云降水显式方案的GRAPES模式较好地模拟出了中国地区降水、温度、云量、长短波辐射的特点和分布规律。气候模拟中冰相过程和暖云过程模拟的降水、温度、云量和辐射差异较大，不同相态的水凝物及其分布对辐射特征有较大的影响，混合相云物理方案的模拟结果与实况更为吻合，应使用混合相云物理方案进行短期气候的模拟。  相似文献   

福建省热带气旋暴雨落区完全预报方法   总被引：1，自引：1，他引：1  

蔡义勇刘爱鸣  陈雪钦李白良 《气象科技》2006,34(2):132-137

通过分析近几年影响和登陆福建省的热带气旋区域暴雨过程的T106部分物理量场的分布特征,发现其中的k指数、比湿q、涡度ζ和垂直速度ω场对预报福建省热带气旋区域暴雨有较好的指示意义,它们分别反映了产生暴雨所必须的水汽、不稳定能量和辐合上升运动等基本条件。为了提高暴雨落区预报的效果,提出以动态方式确定物理量临界值的方法作热带气旋暴雨落区预报。通过对1995~2001年7~10月的144个个例T106物理量场的普查和统计分析,得到福建省热带气旋区域暴雨预报的着眼点和物理量诊断模型,建立了应用T213数值预报模式输出的物理量预报场,以动态方式确定物理量临界值,作为福建省热带气旋区域暴雨落区预报的完全预报(PP)方法。  相似文献   

库尔勒地区两次强对流天气过程的形势和雷达回波对比分析     

李海燕  巴哈古丽  储鸿  赵威 《沙漠与绿洲气象(新疆气象)》2007,1(3)

通过对2006年5月3日和7月17日库尔勒地区两次强对流天气的形势和物理量对比分析,以及库尔勒新一代天气雷达(CINRAD-CC)产品中的组合反射率(CR)、风暴相对平均径向速度(V)等产品的分析,得出库尔勒地区夏季强对流天气过程发生时的有利天气形势、物理量场分布及多谱勒天气雷达产品特征。  相似文献   

High-redshift galaxies, their active nuclei and central black holes     

Martin G. Haehnelt  Priyamvada Natarajan  & Martin J. Rees 《Monthly notices of the Royal Astronomical Society》1998,300(3):817-827

We demonstrate that the luminosity function of the recently detected population of actively star-forming galaxies at redshift z  = 3 and the B -band luminosity function of quasi-stellar objects (QSOs) at the same redshift can both be matched with the mass function of dark matter haloes predicted by standard variants of hierarchical cosmogonies for lifetimes of optically bright QSOs anywhere in the range 10⁶ to 10⁸ yr. There is a strong correlation between the lifetime and the required degree of non-linearity in the relation between black hole and halo mass. We suggest that the mass of supermassive black holes may be limited by the back-reaction of the emitted energy on the accretion flow in a self-gravitating disc. This would imply a relation of black hole to halo mass of the form M _bh ∝  v ⁵_halo ∝  M ^5/3_halo and a typical duration of the optically bright QSO phase of a few times 10⁷ yr. The high integrated mass density of black holes inferred from recent black hole mass estimates in nearby galaxies may indicate that the overall efficiency of supermassive black holes for producing blue light is smaller than previously assumed. We discuss three possible accretion modes with low optical emission efficiency: (i) accretion at far above the Eddington rate, (ii) accretion obscured by dust, and (iii) accretion below the critical rate leading to an advection-dominated accretion flow lasting for a Hubble time. We further argue that accretion with low optical efficiency might be closely related to the origin of the hard X-ray background and that the ionizing background might be progressively dominated by stars rather than QSOs at higher redshift.  相似文献   

Line emission from accretion discs around black holes: the analytic approach     

Andrej ?ade?  Claudio Fanton  Massimo Calvani 《New Astronomy》1998,3(8):528-654

The broad X-ray iron line observed in many active galactic nuclei spectra is thought to originate from the accretion disc surrounding the putative supermassive black hole. We show here how to perform the analytical integration of the geodesic equations that describe the photon trajectories in the general case of a rotating black hole (Kerr metric), in order to write a fast and efficient numerical code for modelling emission line profiles from accretion discs.  相似文献   

Observations of the upper frequency cutoffs of the auroral kilometric radiation     

J. Hanasz  R. Schreiber  H. de Feraudy  M. M. Mogilevsky  T. V. Romantsova 《Annales Geophysicae》1998,16(9):1097-1104

Intense auroral kilometric radiation (AKR) is being frequently observed with POLRAD from the Auroral Probe (Interball-2). Observations of the abrupt upper frequency cutoffs (UFCs) in the spectra of AKR are reported. The UFCs can be observed at a frequency range from 300 to 700 kHz, corresponding to AKR generation altitudes from approximately 4800 to 2100 km, and are distributed in magnetic local time (MLT) hours similarly to the AKR events, with a maximum at 1 h MLT. The observed frequency extent of the UFCs is 12 kHz, and is often determined by the instrumental resolution (4 kHz). It is suggested that the UFC may be associated with an abrupt switching on of the generation mechanism, when the electron density becomes sufficiently low inside a plasma depletion at an altitude where the ratio of f_pe/f_ce crosses some threshold value. The steepness of the UFCs can imply a non-linear process of generation. The estimated distance of the e-folding field aligned wave amplification is between 3 and 8 km. The UFCs are sometimes, though very seldom (10%), accompanied by narrow band (less than 4 kHz) ridges of radiation observed at the cutoff frequency. They are smoothly drifting in frequncy for several minutes. The power density of radiation in the ridge can be up to 2 orders of magnitude stronger than in the accompanying wide band emission of AKR. The ridge at UFC can imply either energy concentration at the source bottom, or focusing, if specific conditions for the escape of the radiation are assumed.  相似文献   

Are our ideas about Dst correct?     

A. Grafe 《Annales Geophysicae》1998,17(1):1-10

The idea of two separate storm time ring currents, a symmetric and an asymmetric one has accepted since the 1960s. The existence of a symmetric equatorial ring current was concluded from Dst. However, the asymmetric development of the low-latitude geomagnetic disturbance field during storms lead to the assumption of the real existence of an asymmetric ring current. I think it is time to inquire whether this conception is correct. Thus, I have investigated the development of the low-latitude geomagnetic field during all the magnetic local times under disturbed and quiet conditions. The storm on February 6–9, 1986 and a statistical analysis of many storms has shown that the asymmetry does not vanish during the storm recovery phase. The ratio between the recovery phase asymmetry and the main phase asymmetry is low only for powerful storms. Storms of moderate intensity show the opposite. The global picture of the field evolution of the February storm shows clear differences at different local times. For instance the main phase and recovery phase start time does not coincide with Dst. Also the ring current decay is not the same at different local times. Therefore, Dst gives an incorrect picture of the field development. Moreover, asymmetry does not disappear during international quiet days as the investigation of the low-latitude geomagnetic field shows. Considering all these observations, I think we must revise our ideas about the ring current. In my opinion only one ring current exists and this is an asymmetric one. This asymmetry increases during storms and develops rather fast to more or less symmetric conditions. However, in no case is itjustified to conclude from Dst that a symmetric ring current exists.  相似文献   

Measurements of the direction of the solar wind using interplanetary scintillation     

P. J. Moran  A. R. Breen  C. A. Varley  P. J. S. Williams  W. P. Wilkinson  J. Markkanen 《Annales Geophysicae》1998,16(10):1259-1264

EISCAT observations of the interplanetary scintillation of a single source were made over an extended period of time, during which the orientation of the baselines between the two observing sites changed significantly. Assuming that maximum correlation between the scintillations observed at the two sites occurs when the projected baseline is parallel to the direction of plasma flow, this technique can be used to make a unique determination of the direction of the solar wind. In the past it has usually been assumed that the plasma flow is radial, but measurements of eleven sources using this technique have indicated conclusively that in at least six cases observed at mid or high heliocentric latitude there is a significant non-radial component directed in four cases towards the heliocentric equator and in two cases towards the pole.  相似文献   

Velocity of auroral arcs drifting equatorward from the polar cap     

P. J. S. Williams  C. F. del Pozo  I. Hiscock  R. Fallows 《Annales Geophysicae》1998,16(10):1322-1331

The drift velocity of an auroral arc is compared with the component of F-region plasma velocity in the same direction for ten cases where the arc is seen to move steadily equatorward for several minutes without any major change in appearance or orientation. In most cases the two velocities are close, but on two occasions the drift velocity of the arc is much higher than the plasma velocity. From the cases studied it appears that during the growth and recovery phase of the substorm cycle the arc moves with a velocity close to the convection velocity, but during the expansion phase this is not the case.  相似文献