О чандлеровском периоде Венеры

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Abstract

Проведено исследование чандлеровского колебания Венеры на основе землеподобных моделей планеты. Метод расчета периода чандлеровского колебания для Венеры протестирован на Земле. Для учета неупругости недр планеты применяется реология Андраде, и определены значения параметров реологической модели, которые могут объяснить наблюдаемый период чандлеровского колебания Земли. Получены прогностические оценки периода чандлеровского колебания Венеры. Для наиболее правдоподобных моделей внутреннего строения Венеры с радиусом ядра в интервале 3288±167 км период чандлеровского колебания составляет 30–48 тыс. лет. Большая погрешность в результатах связана, в основном, с большим разбросом возможных значений постоянной прецессии Венеры.

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About the authors

D. O. Amorim

Московский физико-технический университет

Author for correspondence.
Email: amorim.dargilan@gmail.com
Russian Federation, Москва

Т. В. Гудкова

Институт физики Земли им. О.Ю. Шмидта РАН

Email: gudkova@ifz.ru
Russian Federation, Москва

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Supplementary files

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2. Fig. 1. Comparison of model values ​​of the period of the Earth's Chandler TCW with the observed value from (Chen et al., 2023). For each value of the rheological parameter α, the TCW period is calculated for two values ​​of the precession constant (Hmin and Hmax) and two viscosity profiles (LVP and HVP). Models with α = 0.09–0.11 fall within the range of observed values.

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3. Fig. 2. Comparison of model values ​​of the Earth's Love number k2 with the estimate from (Chen et al., 2023). The Love number k2 is calculated over the period of the Chandler oscillation TCW for two values ​​of the precession constant (Hmin and Hmax) and two viscosity profiles (LVP and HVP) for each value of the rheological parameter α. Models with α = 0.10–0.12 satisfy the k2 value from (Chen et al., 2023).

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4. Fig. 3. Model values ​​of the period of the Chandler wobble of Venus TCW for different combinations of the core radius Rc, precession constant H and parameter B. The TCW values ​​lie in the range from 30 to 48 thousand years. The main part of the error is caused by the uncertainty of the precession constant of Venus. Dashed lines highlight the range of the most probable models of the internal structure of Venus according to (Amorim, Gudkova, 2024b).

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5. Fig. 4. Model values ​​of the tidal Love number k2 of Venus during the period of the Chandler oscillation TCW. Dashed lines highlight the interval of the most probable models of Venus according to (Amorim, Gudkova, 2024b).

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