A new method of discovering new meteor showers from the IMO single-station video meteor database

It has been found that unknown meteor showers could be efficiently discovered from the single station video meteor database of the International Meteor Organization (IMO) by assuming the geocentric velocity and adjusting it within the dynamically permitted range. The mean geocentric velocities of new meteor showers can be obtained, as well as the coordinates of the radiants. The activity period and maximum time can also be obtained if there are sufficient shower meteors. All single station video meteor observations between February 13 and 17 (from 2000 to 2005) in IMO’s database are processed with this method. As a result, two new meteor showers, one near RA=245.10°, Dec=41.82° in Hercules and the other near RA=233.03°, Dec=17.04° in Serpenids, are discovered. Some dynamical characteristics of the new meteor showers are also determined. Considering the random nature on the selection of period in this work, it is expected that there are some more potential new meteor showers in IMO’s video database. Supported by the National Natural Science Foundation of China (Grant No. 10373004)     

Mass distribution of meteoroids obtained by a meteor forward-scatter (MFS) radar method

Summary The cumulative distributions of the numbervs. duration of echoes belonging to main meteor showers (Lyrids, ν-Aquarids, δ-Aquarids, Perseids, Orionids, Leonids, Geminids) and sporadic background were investigated using a forward-scatter (FS) continuous-wave (CW) meteor radar link operational during 1992–95 over the long baseline Bologna-Lecce in Italy. The trend of the mass distribution of particles in the quoted meteoroid streams was derived, and the values of the mass indexs were compared for each meteor population with the steady-state condition (s<11/6). It was found that the mass indexs generally increases towards long-duration echoes, but many of the observed meteor streams appear to have unstable populations. The values of the mass index of the sporadic complex are generally higher (2.07≤s≤ 2.57) than the corresponding ones of meteor showers in the range of echo durations 0.1≤T≤10 s. This is a possible consequence of longer-lasting FS signals, indicating a shift of the mass distribution functionvs. higher echo durations. Moreover, non-gravitational forces in connection with solar radiation pressure, Poynting-Robertson effect, solar-wind particle streaming, mutual collisions, etc., appear to be responsible for the observed widespread radiants and for unstable populations in the meteoroid streams.     

Range distribution of sporadic meteors and sunrise

Summary The echo ranges of 6921 sporadic meteors, determined by the Budrio meteor radar in April-September 1978 during a 15 hour interval around sunrise, are analysed. The variation of the mean ranges exhibits no correlation with the geomagneticK _p index. The observed seasonal variation of the mean ranges at three times of the day is accounted for by the position of the Earth's apex. The mean ranges with respect to local sunrise in the meteor region show a variation with a minimum just after sunrise.

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Riassunto Si analizzano le distanze degli echi da 6921 meteore sporadiche determinate utilizzando la stazione radar di Budrio nel corso di 15 ore di osservazioni centrate intorno all'alba nel periodo aprile-settembre 1978. Le variazioni delle distanze medie non evidenziano alcuna correlazione con l'indice geomagneticoK _p. Le variazioni stagionali delle distanze medie osservate a tre ore diverse del giorno sono da attribuire alla posizione dell'apice della Terra. Le distanze medie rispetto alla locale alba nella regione delle meteore mostrano una variazione che presenta un minimo appena dopo l'alba.

     

On the fragmentation processes in the meteoroid streams

Summary Radar observations of the main meteor showers in 1993–1995 carried out by a forward-scatter radiosystem Bologna-Lecce in Italy are analysed and discussed in terms of fragmentation effects even in the orbit of the streams of interplanetary matter. The existence of very small particles in all meteoroid streams is revealed by counts of echoes of durationT≤0.05 s. A progressive fragmentation is observed to procede in any meteoric complex, likely as a possible consequence of the disintegration of larger bodies in the stream. This disintegration appears to be more significant in some meteoric complexes (Geminids, Leonids and δ-Aquarids), in connection with their differentiated structure and composition.     

A study of non-extensivity in the Earth’s magnetosphere

Magnetic storms are undoubtedly among the most important phenomena in space physics and also a central subject of space weather. The non-extensive Tsallis entropy has been recently introduced, as an effective complexity measure for the analysis of the geomagnetic activity D _st index. Tsallis entropy has been shown to sensitively detect the complexity dissimilarity between pre-storm activity and intense magnetic storms in the Earth’s magnetosphere. Here, we show that the D _st time series obey a modified form of the Gutenberg-Richter law for the case of non-extensive statistics, thus providing evidence for universality in magnetic storm and earthquake occurrence.     

上层大气中石质流星尾迹的紫外光谱模拟

利用Sparrow的粒子碰撞理论,计算了海拔100～90 km范围内的大气中的不同初始地心坐标速度的石质流星的有效温度;分别采取不同的成分配比,给出了速度72 km·s-1的石质流星尾迹主要成分的粒子数密度;应用大型光谱合成程序Cloudy模拟了上述流星尾迹的240～400 nm波段紫外辐射,给出了若干预期的强谱线的相对强度;经比较发现,有效温度5 680 K、蒸汽分压0.1 Pa的尾迹光谱比较接近观测结果。     

Reflection properties of meteor trails in a forward-scatter radar experiment

Summary The distribution of the energy reflected by a meteor trail is strongly connected to the ionization density distribution across and along a meteor trail. Recent forward-scatter observations over the Bologna-Lecce baseline in Italy carried out in 1991–92, show that the number of underdense meteor trails (with electron line densityq≤2.10¹⁴ electrons/mvs. peak signal amplitudes decreases more rapidly with the increasing signal level than what predicted. An exponential (simple and/or log-normal) model is proposed, by taking into account different signal-to-noise ratio thresholds and the Kolmogorov-Smirnov (K-S) procedure is used to test the overall goodness of fit between the set of observations and specified theoretical distributions. It is shown that this model provides a better fit to data mainly for middle-high levels of received power and for values ofq≥10¹³ electrons/m.     

Electron-related optical responses in triple δ-doped quantum wells

A detailed theoretical study on the electron-related optical responses in triple δ-doped GaAs quantum wells in the presence of non-resonant, monochromatic intense laser field is presented. For this purpose, we first obtained the bound subband energy levels and their corresponding envelope wave functions of the structure for different central doping concentrations within the effective-mass approximation. Then, we calculate the effect of the non-resonant intense laser field on the optical properties of this structure using the compact-density-matrix approach via the iterative method. We found that the optical absorption coefficients and refractive index changes in the triple δ-doped GaAs quantum well can be modulated by changing the central doping concentration and the intensity of the non-resonant, monochromatic laser field. In addition, it is shown that a sufficiently intense laser field suppresses the multiple quantum well configuration towards a single potential well one and the optical response becomes practically independent of the δ-doping concentration.     

An observational method for upper-atmospheric wind fluctuations on very small scales

Summary Irregular wind motions in the meteor region ((70÷120) km) on very small space-time scales have been tentatively deduced by radar observations of relatively rare, but long enduring ionized trails of bright meteors (fireballs). The method here presented seems to be proper for the study of the turbulent winds in the upper mesosphere and lower thermosphere.     

Study on the structure functions of electrons and the energy flow in the soft component of cosmic-ray extensive air showers

Summary Cosmic-ray air shower structure functions for the distance dependence of electron density in cosmic-ray air showers in the size range 10⁴⋎10⁸ have been computed for their intercomparison and comparison with Monte Carlo simulation results and measurements from recent experiments. The analysis has yielded the present status of theoretical structure functionsvis à vis experimental results and Monte Carlo simulation distributions. The effect of core location error on the lateral distribution of electrons is also discussed from the point of view of different theoretical and experimental results. The energy flow in the soft component of air showers of size ∼4·10⁵ has been evaluated within a ring of radius 10m about the axis of the showers.     

Spatial and Angular Characteristics of the Atmospheric Showers Initiated by Photons of Energy E γ = 1018–1022 eV in the Magnetosphere of the Earth

Spatial-angular characteristics are calculated for the atmospheric electromagnetic showers generated by primary photons of ultrahigh energies (E = 10¹⁸–10²² eV) coming from outer space. Calculations carried out for vertical and oblique showers in view of the interaction of photons and electrons with the dipole magnetic field of the Earth (formation of electron-positron pairs, synchrotron radiation) and taking into account the Landau–Pomeranchuk–Migdal effect in the processes of interaction of electrons and photons with matter in the meteorological atmosphere.     

Are there tachyons in extensive air showers?

The results obtained by studying double-front extensive air showers in which more than 107 particles are contained and in which the fronts are separated by a time interval of Δt ∼ 100 ns are presented. Serious difficulties in explaining “delayed” showers are revealed. In this connection, a hypothesis that the “leading” showers are initiated by tachyons produced in the first interaction of primary particles is proposed.     

Phase space quantization as a moment problem

We consider questions related to the following quantization scheme: a classical variable f: Ω → ℝ on a phase space Ω is associated with a unique semispectral measure E ^f , such that the kth moment operator of E ^f is required to coincide with the operator integral L(f ^k , E) of f ^k with respect to a certain fixed phase space semispectral measure E. Mainly, we take the phase space Ω to be a locally compact unimodular group. In the concrete case where Ω = ℝ² and E is a translation covariant semispectral measure, we determine explicitly the relevant operators L(f ^k , E) for certain variables f. In addition, we consider the question under what conditions a positive operator measure is projection valued. The text was submitted by the author in English.     

Is (Ins)2 rise in nucleon-nucleon total cross section excluded by cosmic ray data?

Problem of extraction of nucleon-nucleon total cross section from data on zenith angle dependence of frequencies of extensive air showers is discussed. It is shown that one cannot in this way distinguish even between asymptotically constant cross section and that increasing like (Ins)².Presented at the Symposium on Hadron-Hadron Scattering at High Energies, Liblice, Czechoslovakia, June 16–21, 1975.     

Application of new methods of interpretation of meteor observations at the Institute of Astrophysics of Tajikistan

New methods of interpretation of meteor observations were developed and published in [1?C9]. The interpretation of ground-based observations of meteors and bolides available today in the scientific literature all over the world suffers from serious contradictions. Observers use the so-called photometric approach for determination of extra-atmospheric masses of meteoric bodies. This approach is based on the formula proposed in 1933 [10] and very simple ideas of how to describe the interaction between the atmospheric air and the surface of a meteoric body. These ideas are provisionally suitable to describe the flow around a body in a free molecular regime. Subsequently, the photometric approach was applied to all the meteor events including bolides. The main effort aimed to elaborate the approach included a choice of new formulas for the radiative efficiency.     

Kaon absorption from kaonic atoms and formation spectra of kaonic nuclei

We considered the kaon absorption from atomic states into the nucleus. We found that the nuclear density probed by the atomic kaon significantly depends on the kaon orbit. Then, we re-examined the meanings of the observed strengths of one-body and two-body kaon absorption, and investigated the effects to the formation spectra of kaon bound states by in-flight (K ^-, p) reactions. As a natural consequence, if the atomic kaon probes a smaller nuclear density, the ratio of the two-body absorption at nuclear center is larger than the observed value in kaonic atoms, and the depth of the imaginary potential is deeper even at smaller kaon energies as in kaonic nuclear states because of the large phase space for the two-body processes. This deeper imaginary potential makes the signals of kaonic nucleus formation more unclear in the (K ^-, p) spectra.     

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.     

<Emphasis Type="Italic">q</Emphasis>-Breathers and thermalization in acoustic chains with arbitrary nonlinearity Index

Nonlinearity shapes lattice dynamics affecting vibrational spectrum, transport and thermalization phenomena. Beside breathers and solitons one finds the third fundamental class of nonlinear modes, q-breathers, i.e., periodic orbits in nonlinear lattices, exponentially localized in the reciprocal mode space. To date, the studies of q-breathers have been confined to the cubic and quartic nonlinearity in the interaction potential. In this paper we study the case of arbitrary nonlinearity index γ in an acoustic chain. We uncover qualitative difference in the scaling of delocalization and stability thresholds of q-breathers with the system size: there exists a critical index γ* = 6, below which both thresholds (in nonlinearity strength) tend to zero, and diverge when above. We also demonstrate that this critical index value is decisive for the presence or absence of thermalization. For a generic interaction potential the mode space localized dynamics is determined only by the three lowest order nonlinear terms in the power series expansion.     

Some metallic properties in the framework of Tsallis generalized statistics

Some metallic quantities are calculated on the grounds of Tsallis generalized statistics: the specific heat at constant volume, c _V (T); the chemical potential, ; the Pauli paramagnetic susceptibility, and the Korringa constant, . First it is found that for a general value of q, the Sommerfeld expansion series will exhibit both, odd and even terms, contrary to what is obtained if we use the Fermi-Dirac (FD) statistics, where only even terms appear. It follows that: (i) the specific heat coefficient, , is q-dependent, but the temperature dependence of c_V remains linear, as in the FD case; (ii) the Fermi energy, , differs from the chemical potential by a linear term in T, and not quadratic, as in FD, the same happening for ; (iii) the Korringa constant is q-dependent, but not T-dependent. In the limit the results of FD statistics are recovered. Metallic thin films and multilayers exhibiting fractal surface structures are possible systems where the present results could be tested. Received 30 June 1999 and Received in final form 7 September 1999     

Existence,Non-existence,and Uniqueness for a Heat Equation with Exponential Nonlinearity in ℝ2

We consider a semilinear heat equation with exponential nonlinearity in ?². We prove that local solutions do not exist for certain data in the Orlicz space exp L ²(?²), even though a small data global existence result holds in the same space exp L ²(?²). Moreover, some suitable subclass of exp L ²(?²) for local existence and uniqueness is proposed.