1975.0-2011.0 期间钱德勒极点涛动参数变化的动力学研究

IF 0.5 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS
N. M. Zalivadny, L. Ya. Khalyavina
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引用次数: 0

摘要

根据非线性最小二乘法,对 1975.0-2011.0 期间的磁极坐标变化时间序列(C01 国际地球资源卫星版本)进行了结构分析。得到了这一时期极点运动主要组成部分参数的平均估计值,即钱德勒摆动、年摆动和半年摆动。得到的主要成分的周期 T 和振幅 A 值如下钱德勒摆动的周期 T = 433.49 ± 0.22 天,振幅 A = 160 ± 3 玛;年度摆动的周期 T = 365.19 ± 0.37 天,振幅 A = 93 ± 5 玛;半年度摆动的周期 T = 183.03 ± 0.34 天,振幅 A = 4 ± 2 玛。在关注钱德勒振荡的表现时,对时间序列中的极坐标变化进行了研究。研究了振荡参数(包括振幅、周期、相位和 Q 因子)的动态变化。钱德勒振荡参数的变化显示了它们之间的相互依存关系。相位和周期变化之间的相关系数为 +0.94,相位和振幅变化之间也有类似的关系,相关系数为 +0.88。相位变化先于振幅和周期变化。钱德勒摆动参数的这种行为表明,周期和振幅的变化应被视为相位变化的结果。研究表明,钱德勒摆动振幅的增加与衰减递减的减少相关,相关系数为-0.98。这些发现与梅尔基奥尔阐述的统计模式一致,表明(a)钱德勒振荡的周期随时间变化不稳定;(b)振荡周期和振幅之间的比例变化。因此,在所研究的一段时间内,应优先考虑周期可变的钱德勒极运动单分量复杂模型。
本文章由计算机程序翻译,如有差异,请以英文原文为准。

A Study of Dynamics of Changes in Parameters of the Chandler Pole Oscillation in the Period 1975.0–2011.0

A Study of Dynamics of Changes in Parameters of the Chandler Pole Oscillation in the Period 1975.0–2011.0

A structural analysis of the time series of pole coordinate changes (version C01 IERS) for the period of 1975.0–2011.0 has been performed based on the nonlinear least squares method. Average estimates of the parameters of the main components of the pole movement—namely, Chandler, annual, and semiannual wobbles—are obtained for this period. The obtained values of periods T and amplitudes A of the main components are as follows: T = 433.49 ± 0.22 days and A = 160 ± 3 mas for the Chandler oscillations; T = 365.19 ± 0.37 days and A = 93 ± 5 mas for the annual oscillations; and T = 183.03 ± 0.34 days and A = 4 ± 2 mas for the semiannual oscillations. Changes in the pole coordinates are examined in the time series when focusing on the manifestation of Chandler oscillations. The dynamics of oscillation parameters (including amplitude, period, phase, and Q factor) is studied. Changes in the Chandler oscillation parameters show their interdependence. The correlation coefficient between phase and period variations is +0.94, and a similar relationship is observed between phase and amplitude variations with a correlation coefficient of +0.88. It is shown that the phase change precedes the changes in the amplitude and in the period. This behavior of the parameters of the Chandler wobble suggests that changes in the period and in the amplitude should be considered a consequence of the phase changes. It is revealed that an increase in the amplitude of Chandler oscillations correlates with a decrease in the attenuation decrement with a correlation coefficient of –0.98. These findings align with the statistical patterns articulated by Melchior, which are indicative of (a) inconstancy of the period of Chandler oscillations over time and (b) proportional changes between the period and the amplitude of oscillations. Thus, preference should be given to the one-component complicated model of the Chandler pole movement with a variable period for the studied period of time.

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来源期刊
Kinematics and Physics of Celestial Bodies
Kinematics and Physics of Celestial Bodies ASTRONOMY & ASTROPHYSICS-
CiteScore
0.90
自引率
40.00%
发文量
24
审稿时长
>12 weeks
期刊介绍: Kinematics and Physics of Celestial Bodies is an international peer reviewed journal that publishes original regular and review papers on positional and theoretical astronomy, Earth’s rotation and geodynamics, dynamics and physics of bodies of the Solar System, solar physics, physics of stars and interstellar medium, structure and dynamics of the Galaxy, extragalactic astronomy, atmospheric optics and astronomical climate, instruments and devices, and mathematical processing of astronomical information. The journal welcomes manuscripts from all countries in the English or Russian language.
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