共查询到20条相似文献，搜索用时 31 毫秒
1.
V. G. Kaydash S. Yu. Gerasimenko Yu. G. Shkuratov N. V. Opanasenko Yu. I. Velikodsky V. V. Korokhin M. V. Kaydash 《Solar System Research》2010,44(4):267-280
From the ground-based colorimetry performed for two surface regions of the near side of the Moon, images of the phase ratio
of the color index C(600 nm/470 nm) have been built for the phase angles between 2° and 95°. It has been found that for phase angles smaller than
α ∼ 40°–50°, the color index of the highlands grows with the phase quicker than that of the mare regions. For larger phase
angles, α > 50°, a reverse situation is observed. The laboratory data on the spectrophotometry of the lunar samples confirm
the peculiarities found in the phase dependence of color. The influence of multiple scattering on the phase dependence of
the color of the mare and highland regions of the Moon are discussed. 相似文献
2.
A method for interpretation of asteroid phase curves, based on empirical modeling and laboratory measurements, is outlined and preliminary results are presented. A linear-exponential function is used to describe the opposition peaks and negative polarization surges of various asteroids and laboratory samples and a statistical algorithm is used in parameter estimation. The linear-exponential function describes well the phase curves, but dense phase angle coverage, particularly at small phase angles must be obtained to improve the results. Major emphasis should also be put on laboratory study: with an extensive library of laboratory measurements, a stronger connection between the phase curve properties and surface characteristics is possible. 相似文献
3.
GPS接收机天线相位中心偏差的检测 总被引：5，自引：0，他引：5
GPS接收机天线相位中心偏差是指GPS天线接收卫星信号的电气中心与基机械几何中心之差。在高精度测量中，这是不容忽视的。讨论了采用基线测量相对测定法确定天线相位中心在水平和垂直方向上的偏差的原理和方法，并给出了测量结果及建议。 相似文献
4.
We performed photometry of Cassini Visual Infrared Mapping Spectrometer observations of Iapetus to produce the first phase integrals calculated directly from solar phase curves of Iapetus for the leading hemisphere and to estimate the phase integrals for the trailing hemisphere. We also explored the phase integral dependence on wavelength and geometric albedo. The extreme dichotomy of the brightness of the leading and trailing sides of Iapetus is reflected in their phase integrals. Our phase integrals, which are lower than the results of Morrison et al. (Morrison, D., Jones, T.J., Cruikshank, D.P., Murphy, R.E. [1975]. Icarus 24, 157-171) and Squyres et al. (Squyres, S.W., Buratti, B.J., Veverka, J., Sagan, C. [1984]. Icarus 59, 426-435), have profound implications on the energy balance and volatile transport on this icy satellite. 相似文献
5.
Spectral reflectivities ?(λ) of the features on the disk of Jupiter (NTrZ, NEB, EZ, SEB, STrZ) and the center of the disk of Saturn were measured for different phase angles. The phase dependence of ?(λ) is shown to correspond to the shape of the phase function. 相似文献
6.
闭合相位法是实现长基线恒星光干涉高分辨成像的重要技术手段之一,获得精确的闭合相位信息是进行光干涉图像重构的先决条件.提出一种基于精密光程差调制的时域干涉信号闭合相位检测方法,在3路干涉臂上进行非冗余精密光程调制,并通过多次干涉测量结合数据拟合的方法消除光程差调制中存在的正弦误差,使得光程调制的精度达到20 nm以内.引入高速探测器件提升时域干涉信号的采样频率,对探测器上获得的时域干涉信号进行傅立叶变换处理,获得3路干涉臂精确的闭合相位信息.室内实验结果表明,基于精密光程调制的时域信号闭合相位计算精度可以达到1/50波长以内. 相似文献
7.
8.
We present the results of a statistical study of the solar cycle based on the analysis of the superficial toroidal magnetic
field component phase space. The magnetic field component used to create the embedded phase space was constructed from monthly
sunspot number observations since 1750. The phase space was split into 32 sections (or time instants) and the average values
of the orbits on this phase space were calculated (giving the most probable cycle). In this phase space it is shown that the
magnetic field on the Sun’s surface evolves through a set of orbits that go around a mean orbit (i.e., the most probable magnetic cycle that we interpret as the equilibrium solution). It follows that the most probable cycle
is well represented by a van der Pol oscillator limit curve (equilibrium solution), as can be derived from mean-field dynamo
theory. This analysis also retrieves the empirical Gnevyshev – Ohl’s rule between the first and second parts of the solar
magnetic cycle. The sunspot number evolution corresponding to the most probable cycle (in phase space) is presented. 相似文献
9.
We have used the integrated brightnesses from Mariner 9 high-resolution images to determine the large phase angle (20° to 80°) phase curves of Phobos and Deimos. The derived phase coefficients are β = 0.032 ± 0.001 mag/deg for Phobos and β = 0.030 ± 0.001 mag/deg for Deimos, while the corresponding phase integrals are qPhobos = 0.52 and qDeimos = 0.57. The predicted intrinsic phase coefficients of the surface material are βi = 0.019 mag/deg and βi = 0.017 mag/deg for Phobos and Deimos, respectively. The phase curves, phase coefficients and phase integrals are typical of objects whose surface layers are dark and intricate in texture, and are consistent with the presence of a regolith on both satellites. The relative reflectance of Deimos to Phobos is 1.15±0.10. The presence of several bright patches on Deimos could account for this slight difference in average reflectance. 相似文献
10.
The time-sequence of polar magnetic substorms is discussed to clarify some controversies on the magnetospheric substorm model including the growth phase. The main purpose of the analyses is to examine magnetic variations in the polar cap and in low latitudes. The onset of the expansion phase is confirmed to be reasonably defined by a vector change of polar-cap magnetic disturbance, a sharp intensification of the auroral electrojet disturbance and the beginning of positive ΔH disturbance in midlatitudes near midnight. It is shown that the growth phase signatures so far proposed are consistent when the onset of the expansion phase is identified from the above mentioned features. 相似文献
11.
The change of source characteristics during the transition from the impulsive phase to the post-burst phase is investigated for cm bursts on a statistical basis. The results are the following: (1) The sudden decrease of the circular polarization degree is found almost invariably at the transition; typically from 20–30% down to a few percent. (2) Some bursts show remarkable source expansions in the post-burst phase. There are no cases in which impulsive bursts have larger source size than the associated post-burst increases. (3) Type III bursts which are indicative of non-thermal phenomena are associated with the impulsive phase but not with the post-burst phase. Implications of these observed results are discussed. 相似文献
12.
V.G. Shevchenko I.N. Belskaya I.G. Slyusarev Yu.N. Krugly V.G. Chiorny N.M. Gaftonyuk Z. Donchev V. Ivanova M.A. Ibrahimov Sh.A. Ehgamberdiev I.E. Molotov 《Icarus》2012,217(1):202-208
CCD-photometry of three Jupiter Trojan asteroids were carried out to study their opposition effect. We obtained well-sampled magnitude–phase curves for (588) Achilles, (884) Priamus, and (1143) Odysseus in the maximal attainable phase angle range down to 0.1–0.2°. The magnitude–phase relations have a linear behavior in all observed range of phase angles and do not show any non-linear opposition brightening. We have not found any confident differences between phase slopes measured in B, V and R bands. The values of the measured phase slopes of Trojans are different from available data for Centaurs. They are within the range of phase slopes measured for some low-albedo main belt asteroids, also exhibit a linear behavior down to small phase angles. An absence of non-linear opposition brightening puts constraints on the surface properties of the studied objects, assuming very dark surfaces where single scattering plays dominating role.We also determined the rotation periods, amplitudes, the values of color indexes B–V and V–R, and the absolute magnitudes of these asteroids. 相似文献
13.
We study the longitudinal distribution of sunspot activity in 1917–1995 using vector sums of sunspot areas. The vector sum
of sunspots of one solar rotation gives a total vector whose amplitude characterizes the size of longitudinal asymmetry and
whose phase describes the location of the momentarily dominating longitude. We find that when the phase distributions are
calculated separately for the ascending phase and maximum (AM) on the one hand and for the declining phase and minimum (DM)
on the other hand, they behave differently and depict broad maxima around roughly opposite longitudes. While the maximum of
the phase distribution for the AM period is found around the Carrington longitude of 180°, the maximum for the DM period is
at the longitude of about 0°. This difference can be seen in both solar hemispheres, but it is more pronounced in the southern
hemisphere where the phase distribution has a particularly clear pattern. No other division of data into two intervals leads
to similar systematic differences. 相似文献
14.
Somenath Chakrabarty 《Journal of Astrophysics and Astronomy》1995,16(3-4):399-405
The effect of intense magnetic field on the cosmic quark-hadron phase transition and also on the baryon number inhomogeneity
has been investigated using phenomenological MIT bag model for the quark sector. For the sake of simplicity an ideal gas equation
of state has been considered for the hadronic phase. 相似文献
15.
A hierarchy of cyclic changes in solar activity is studied based on energetic and phase wavelet analyses. The phase wavelet spectrum of yearly number of sunspot groups shows fork-like bifurcations. Separate 11-yr cycles are combined in pairs and wave trains to make up complete magnetic cycles with complex synergies. The phase spectrum also indicates the existence of different regimes in solar activity cyclic changes. This variability seems to be controlled by changes in the solar dynamo regime. 相似文献
16.
The evolution of two dimensional wave packets on the surface of a self-gravitating fluid layer is investigated and shown to be governed by a nonlinear Schrödinger equation. The wave train of finite amplitude is modulationally unstable. Obtained also are the dynamical equations for the second harmonic resonance. The analysis reveals that the general motion consists of both amplitude and phase modulated waves of which the pure phase and amplitude modulated waves, solitary waves, and phase jump are just the special cases. 相似文献
17.
18.
The dependence of brightness and polarization of cometary on the phase angle is studied. The similarity between the phase curves of comets, minor planets, and the zodiacal cloud is pointed out. The dependence found correspond to dielectric particles with dimensions greater than 1 μm. 相似文献
19.
Kyoung W. Min 《Astrophysics and Space Science》1988,150(2):345-355
The recovery phase of the magnetospheric substorm is studied numerically by means of a two-dimensional time-dependent nonlinear resistive MHD code. The initial configuration was chosen from the earlier numerical model in which the magnetospheric substorm was driven by the solar wind plasmas. In order to study the recovery phase, the entering solar wind energy flux was reduced when the magnetospheric substorm was in its expansive phase. The system was found to respond instantly to this change and the result showed many characteristic features related to the recovery phase including the tailward motion of thex-point of the reconnected magnetic field lines and the restoration of a tail-like configuration of the magnetic field. Thex-point moved at almost the same speed of the plasma flow in the upstream region, which was considerably smaller than the speed of the plasma jetting or the speed of the plasmoid. As the recovery phase progressed, the plasma jetting across thex-point was reduced very much in the Earthside region. Although the plasma flow was generally in the Earthward direction in the Earthside region of thex-point, the tailward flow was also found near thex-point. The current density was reduced near thex-point and the neutral sheet was broadened in the recovered region. The plasma sheet also became thick in this region. During the recovery of the substorm, the energy conversion rate, both in the form of plasma acceleration and the Joule heating, was reduced. These results on the recovery phase together with the earlier simulation result on the expansive phase indicate that driven reconnection can be a viable mechanism for the magnetospheric substorm including the recovery phase. 相似文献
20.
E.F. Tedesco 《Icarus》1976,28(1):21-28
UBV photometry and lightcurves of Eros were obtained on nine dates between October 1974 and March 1975. The absolute V magnitude at photometric maximum extrapolated to a solar phase angle of zero is 10.75 while the linear phase coefficient is 0.026mag deg?1. The mean colors at solar phase angles greater than 30° are B?V = 0.92 and U?B = 0.52mag. No significant color variations over the surface were detected. 相似文献