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低纬子午环配备科学CCD的必要性和可行性 总被引:1,自引:1,他引:0
从基本天体测量学科的发展趋势和低纬子午环的课题目标出发,叙述了该仪器配备科学CCD的必要性和对仪器性能的相应要求,并根据仪器的各种误差的测定方法和测定精度的分析,论述了该仪器配备科学CCD后对天体位置作高精度绝对测定的可行性,文中还提出了对配备科学CCD的总体要求。 相似文献
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1991年3月,我们利用上海25m射电望远镜和欧洲VLBI网联合对几个河外射电源进行了第二历元的327MHzVLBI观测.数据的相关处理先后在上海天文台三台站MK2相关处理机和美国的Caltech/JPL相关处理机进行,以便于比较相关结果。本文给出3C84、3C345和3C380的混合图。与第一历元的观测比较,3C345和3C380的流量密度没有明显的变化,但3C345的结构变化明显。3C84和3C345有喷流的迹象.3C454.3的总流量在不到两年的时间内增加了25%,如果这个变化是内禀的话,那么可能意味着一次新的流量爆发。 相似文献
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Comptonγ射线望远镜COMPTEL/CGRO工作于0.75-30MeV能区,本文应用直接解调方法分析CGRO#1观测的COMPTEL数据,准确定出Crabγ射线源的位置,在10-30MeV能区,分辨开最大似然法所不能完全分辨的Crabγ射线源和类星体PKS0528+134,得出优于传统成像方法所得的成像结果.应用直接成像方法处理γ射线脉冲星Geminga分位相数据,发现Geminga在10-30MeV能区仍存在辐射,辐射集中在Geminga第一个峰的位相区域.结果表明,应用直接解调方法对Compton望远镜数据作成像分析是完全可行的 相似文献
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介绍了低纬子午环上原设计的光子计数测微器的结构和观测方式,并针对目前仪器的具体状态,说明了为什么这一测微器不能采用,而用视频CCD替代它,文中还叙述了采用视频CCD的观测方式和有关参数的测定方法。 相似文献
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本文推导了低纬子午环采用CCD测微器观测时所得测定值的各种星径曲率改正公式。针对云南天文台具体的地理位置(纬度为25°),在不同观测天顶距情况下,给出了CCD视场中不同位置的天体通过参考平面(子午平面或卯酉平面)时,星过记录时刻和天顶距测定值的星径曲率改正模拟运算结果。结果表明:对于偏离CCD芯片相对中心的天体,其星径曲率改正值比较大,且随天体偏离距离的增加而增大。 相似文献
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Comptonγ射线望远镜的直接解调成像 总被引:2,自引:0,他引:2
Comptonγ射线望远镜COMPTEL/CGRO工作于0.75-30MeV能区,本应用直接解调方法分析了CGRO#1观测的COMPTEL数据,准确定出Carabγ射线源的位置,在10-30MeV能区,分辨开最大似然法所不能完全分辨的Crabγ射线源和类星体PKS0528+134,得出优于传统成像方法所得的成像结果。 相似文献
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Range of values of the Sun's mass quadrupole moment of coefficient J2 arising both from experimental and theoretical determinations enlarge across literature on two orders of magnitude, from
around 10-7 until to 10-5. The accurate knowledge of the Moon's physical librations, for which the Lunar Laser Ranging data reach an outstanding precision
level, prove to be appropriate to reduce the interval of J2 values by giving an upper bound of J2. A solar quadrupole moment as high as 1.1 10-5 given either from the upper bounds of the error bars of the observations, or from the Roche's theory, is not compatible with
the knowledge of the lunar librations accurately modeled and observed with the LLR experiment. The suitable values of J2 have to be smaller than 3.0 10-6.
As a consequence, this upper bound of 3.0 10-6 is accepted to study the impact of the Sun's quadrupole moment of mass on the dynamics of the Earth-Moon system. Such as
effect (with J2 = 5.5±1.3 × 10-6) has been already tested in 1983 by Campbell & Moffat using analytical approximate equations, and thus for the orbits of
Mercury, Venus, the Earth and Icarus. The approximate equations are no longer sufficient compared with present observational
data and exact equations are required. As if to compute the effect on the lunar librations, we have used our BJV relativistic
model of solar system integration including the spin-orbit coupled motion of the Moon. The model is solved by numerical integration.
The BJV model stems from general relativity by using the DSX formalism for purposes of celestial mechanics when it is about
to deal with a system of n extended, weakly self-gravitating, rotating and deformable bodies in mutual interactions.
The resulting effects on the orbital elements of the Earth have been computed and plotted over 160 and 1600 years. The impact
of the quadrupole moment of the Sun on the Earth's orbital motion is mainly characterized by variations of
,
, and
. As a consequence, the Sun's quadrupole moment of mass could play a sensible role over long time periods of integration of
solar system models.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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Wu Lin-xiang 《Chinese Astronomy and Astrophysics》1992,16(4):427-433
By means of a simple relation between the velocity v of the fluid particle and the velocity vf of the photospheric footpoint of the magnetic field line vz and Bz being respectively the components of v and the magnetic field B normal to the photospheric surface, it is shown formally that through the phtospheric surface the transport of all the quantities attributed to the magnetic field, such as the magnetic flux, the magnetic energy and the helicity, is independent of vz, and vf is the only kinematical quantity on which the transport depends. In addition, in the neighborhood of the neutral line the velocity vl of the moving curve of constant Bz is found to be equal approximately to the component of v or vf in the direction of vl. Since vl can be measured or extimated, so can the components of v and vf near the neutral line. 相似文献
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介绍和论述了在后牛顿引力理论(PPN形式)中在优越参考系和非优越参考系中经过参数化后引力常数变化对地球自转产生的效应,其中特别重点介绍了年周期变化的效应。此外也将理论结果同观测结果相对比。 相似文献
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In this paper we first emphasize why it is important to know the successive zonal harmonics of the Sun's figure with high
accuracy: mainly fundamental astrometry, helioseismology, planetary motions and relativistic effects. Then we briefly comment
why the Sun appears oblate, going back to primitive definitions in order to underline some discrepancies in theories and to
emphasize again the relevant hypotheses. We propose a new theoretical approach entirely based on an expansion in terms of
Legendre's functions, including the differential rotation of the Sun at the surface. This permits linking the two first spherical
harmonic coefficients (J
2 and J
4) with the geometric parameters that can be measured on the Sun (equatorial and polar radii). We emphasize the difficulties
in inferring gravitational oblateness from visual measurements of the geometric oblateness, and more generally a dynamical
flattening. Results are given for different observed rotational laws. It is shown that the surface oblateness is surely upper
bounded by 11 milliarcsecond. As a consequence of the observed surface and sub-surface differential rotation laws, we deduce
a measure of the two first gravitational harmonics, the quadrupole and the octopole moment of the Sun: J
2=−(6.13±2.52)×10−7 if all observed data are taken into account, and respectively, J
2=−(6.84±3.75)×10−7 if only sunspot data are considered, and J
2=−(3.49±1.86)×10−7 in the case of helioseismic data alone. The value deduced from all available data for the octopole is: J
4=(2.8±2.1)×10−12. These values are compared to some others found in the literature.
Supplementary material to this paper is available in electronic form at http://dx.doi.org/10.1023/A:1005238718479 相似文献
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A. M. Boichenko 《Astrophysics》2004,47(1):134-142
Observational data on the dynamics of stars in the neighborhood of the sun indicate the existence of a third integral besides the integrals of the angular momentum and energy. The Poincaré integral is proposed as a third integral. The consequences of this assumption are derived and compared with available astrophysical data. 相似文献
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B. P. Kondratyev 《Solar System Research》2013,47(1):1-10
A two-component theoretical model of the physical libration of the Moon in longitude is constructed with account taken of the viscosity of the core. In the new version, a hydrodynamic problem of motion of a fluid filling a solid rotating shell is solved. It is found that surfaces of equal angular velocity are spherical, and a velocity field of the fluid core of the Moon is described by elementary functions. A distribution of the internal pressure in the core is found. An angular momentum exchange between the fluid core and solid mantle is described by a third-order differential equation with a right-hand side. The roots of a characteristic equation are studied and the stability of rotation is proved. A libration angle as a function of time is found using the derived solution of the differential equation. Limiting cases of infinitely large and infinitely small viscosity are considered and an effect of lag of a libration phase from a phase of action of an external moment of forces is ascertained. This makes it possible to estimate the viscosity and sizes of the lunar fluid core from data of observations. 相似文献
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M. V. Samokhin 《Earth, Moon, and Planets》1993,61(1):29-37
Using the well-known equation for the normal component of the current which exist near the tangential discontinuity in the plasma in the case of the frozen-in magnetic field, and supposing that the current closes in the ionosphere in the auroral oval in the region 1, one calculates and compares with the data of observations the dependence of the density of the field-aligned current at the level of the ionosphere on the local time. 相似文献
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In the framework of the programme of studying the meridional section of the Galaxy (MEGA) the absolute proper motions of more than 11000 stars with respect to 3000 galaxies and their stellar magnitudes in the B, V Johnson system are determined in two sky regions near the North Galactic Pole (NGP) by means of Tautenburg Schmidt plates. The limiting and completing apparent stellar magnitudes are B = 20.4 and 18.3 mag, the overall and the investigated sky areas are 16.4 and 14.6 square degrees, respectively. Distances have been determined using the stellar magnitudes, colours, proper motions and reduced proper motions. Stellar kinematics, eccentricities of Galactic orbits, spatial distribution and changes of these characteristics with Z-distance from the Galactic plane are obtained up to 15 kpc. Four subsystems distinguished in the NGP direction, respectively with semithicknesses of 0.25, 0.38, 0.67, 1.48 kpc and density ellipsoid axial ratios of 0.09, 0.20, 0.28, 0.49 show mean velocities in the Galactic rotation direction relative to the LSR of 5.6 ± 0.6, − 11.0 ± 0.6, − 62.5 ± 1.2, − 181.6 ± 4.4 km/s, and ages of 0.1, 0.4, 0.9, 1 of the Galaxy age. 相似文献