Standard

On the stability of the rotational motion of nonspherical natural satellites in a synchronous resonance. / Mel'nikov, A. V.; Shevchenko, I. I.

In: Solar System Research, Vol. 34, No. 5, 01.12.2000, p. 434-442.

Research output: Contribution to journal › Article › peer-review

Harvard

Mel'nikov, AV & Shevchenko, II 2000, 'On the stability of the rotational motion of nonspherical natural satellites in a synchronous resonance', Solar System Research, vol. 34, no. 5, pp. 434-442.

APA

Mel'nikov, A. V., & Shevchenko, I. I. (2000). On the stability of the rotational motion of nonspherical natural satellites in a synchronous resonance. Solar System Research, 34(5), 434-442.

Vancouver

Mel'nikov AV, Shevchenko II. On the stability of the rotational motion of nonspherical natural satellites in a synchronous resonance. Solar System Research. 2000 Dec 1;34(5):434-442.

Author

Mel'nikov, A. V. ; Shevchenko, I. I. / On the stability of the rotational motion of nonspherical natural satellites in a synchronous resonance. In: Solar System Research. 2000 ; Vol. 34, No. 5. pp. 434-442.

BibTeX

@article{d9cc51e382754ae0bc0b66cae952b90e,
title = "On the stability of the rotational motion of nonspherical natural satellites in a synchronous resonance",
abstract = "The stability of the rotational motion of a nonspherical natural satellite in an elliptical orbit in a synchronous spin-orbital resonance is studied. The axis of rotation of a satellite is assumed to coincide with the axis of its maximum moment of inertia and to be orthogonal to the orbital plane. On the plane of the inertial parameters (A/C, B/C), where A, B, and C (A < B < Q are the principal moments of inertia, the boundaries of regions of stability and instability with respect to tilting the axis of rotation are determined by calculating the multiplicators of linearized Hamiltonian equations of motion. High resolution, achieved in the determination of the boundaries of these regions, makes it possible to impose additional constraints on the values of inertial parameters for Hyperion and, in the case of Amalthea, to draw a conclusion on the instability of its relative motion with respect to tilting the axis of rotation in one of two possible synchronous resonances.",
author = "Mel'nikov, {A. V.} and Shevchenko, {I. I.}",
year = "2000",
month = dec,
day = "1",
language = "English",
volume = "34",
pages = "434--442",
journal = "Solar System Research",
issn = "0038-0946",
publisher = "МАИК {"}Наука/Интерпериодика{"}",
number = "5",

}

RIS

TY - JOUR

T1 - On the stability of the rotational motion of nonspherical natural satellites in a synchronous resonance

AU - Mel'nikov, A. V.

AU - Shevchenko, I. I.

PY - 2000/12/1

Y1 - 2000/12/1

N2 - The stability of the rotational motion of a nonspherical natural satellite in an elliptical orbit in a synchronous spin-orbital resonance is studied. The axis of rotation of a satellite is assumed to coincide with the axis of its maximum moment of inertia and to be orthogonal to the orbital plane. On the plane of the inertial parameters (A/C, B/C), where A, B, and C (A < B < Q are the principal moments of inertia, the boundaries of regions of stability and instability with respect to tilting the axis of rotation are determined by calculating the multiplicators of linearized Hamiltonian equations of motion. High resolution, achieved in the determination of the boundaries of these regions, makes it possible to impose additional constraints on the values of inertial parameters for Hyperion and, in the case of Amalthea, to draw a conclusion on the instability of its relative motion with respect to tilting the axis of rotation in one of two possible synchronous resonances.

AB - The stability of the rotational motion of a nonspherical natural satellite in an elliptical orbit in a synchronous spin-orbital resonance is studied. The axis of rotation of a satellite is assumed to coincide with the axis of its maximum moment of inertia and to be orthogonal to the orbital plane. On the plane of the inertial parameters (A/C, B/C), where A, B, and C (A < B < Q are the principal moments of inertia, the boundaries of regions of stability and instability with respect to tilting the axis of rotation are determined by calculating the multiplicators of linearized Hamiltonian equations of motion. High resolution, achieved in the determination of the boundaries of these regions, makes it possible to impose additional constraints on the values of inertial parameters for Hyperion and, in the case of Amalthea, to draw a conclusion on the instability of its relative motion with respect to tilting the axis of rotation in one of two possible synchronous resonances.

UR - http://www.scopus.com/inward/record.url?scp=0141447852&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0141447852

VL - 34

SP - 434

EP - 442

JO - Solar System Research

JF - Solar System Research

SN - 0038-0946

IS - 5

ER -

ID: 45989718