HD 6840 is a double-lined visual binary with an orbital period of ～7.5 years. By fitting the speckle interferometric measurements made by the 6 m BTA telescope and 3.5 m WIYN telescope, Balega et al. gave a preliminary astrometric orbital solution of the system in 2006. Recently, Griffin derived a precise spectroscopic orbital solution from radial velocities observed with OPH and Cambridge Coravel.However, due to the low precision of the determined orbital inclination, the derived component masses are not satisfying. By adding the newly collected astrometric data in the Fourth Catalog of Interferometric Measurements of Binary Stars, we give a three-dimensional orbit solution with high precision and derive the preliminary physical parameters of HD 6840 via a simultaneous fit including both astrometric and radial velocity measurements.
For tracking spacecraft and performing radio science,the transformation between the proper time(τ) given by a clock carried onboard a spacecraft and the barycentric coordinate time(TCB) is investigated under IAU resolutions.In order to more clearly demonstrate manifestations of a physical model and improve computational efficiency,an analytic approach is adopted.After numerical verification,it is confirmed that this method is adequate to describe a Mars orbiter during one year,and is particularly good at describing the influence from perturbing bodies.Further analyses demonstrate that there are two main effects in the transformation:the gravitational field of the Sun and the velocity of the spacecraft in the barycentric coordinate reference system.The combined contribution of these effects is at the level of a few sub-seconds.
A pure two-body problem has seven integrals including the Kepler energy,the Laplace vector and the angular momentum vector.However,only five of them are independent.When the five independent integrals are preserved,the two other dependent integrals are naturally preserved from a theoretical viewpoint;but they may not necessarily be from a numerical computational viewpoint.Because of this,we use seven scale factors to adjust the integrated positions and velocities so that the adjusted solutions strictly satisfy the seven constraints.Noticing the existence of the two dependent integrals,we adopt the Newton iterative method combined with singular value decomposition to calculate these factors.This correction scheme can be applied to perturbed two-body and N-body problems in the solar system.In this case,the seven quantities associated with each planet slowly vary with time.More accurate values can be given to the seven slowly-varying quantities by integrating the integral invariant relations of these quantities and the equations of motion.They should be satisfied with the adjusted solutions.Numerical tests show that the new method can significantly reduce the rapid growth of numerical errors for all orbital elements.
中天观测数据在建立太阳系高精度行星历表时具有重要作用.在处理由JPL(Jet Propulsion Laboratory)以及IMCCE(Institut De Mecanique Celeste Et De Calcul Des Ephemerides)提供的中天数据时发现,有若干组数据的参考星表没有被明确指出。对于这些信息不完整的数据,无从改正数据由参考星表而引起的系统差。课题研究的主要目的是利用DE421历表确定存在缺陷的这类观测数据的参考星表。通过DE421给出行星在GCRS(Geocentric Celestial Reference System)中的相应位置,并把此位置转换到参考假定的参考星表时行星的理论视位置。通过引入的两个统计量分析原始数据与理论位置的差异显著性,检验假定的数据参考星表是否恰当.结果显示,此方法能够有效区分数据的参考星表,能够确定信息不完整的数据组缺少的参考星表。最后,所有中天数据被转换到GCRS坐标系,以便在历表研制中使用。
