Standard

The rotation states predominant among the planetary satellites. / Melnikov, A. V.; Shevchenko, I. I.

In: Icarus, Vol. 209, No. 2, 01.10.2010, p. 786-794.

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

Harvard

Melnikov, AV & Shevchenko, II 2010, 'The rotation states predominant among the planetary satellites', Icarus, vol. 209, no. 2, pp. 786-794. https://doi.org/10.1016/j.icarus.2010.04.022

APA

Melnikov, A. V., & Shevchenko, I. I. (2010). The rotation states predominant among the planetary satellites. Icarus, 209(2), 786-794. https://doi.org/10.1016/j.icarus.2010.04.022

Vancouver

Melnikov AV, Shevchenko II. The rotation states predominant among the planetary satellites. Icarus. 2010 Oct 1;209(2):786-794. https://doi.org/10.1016/j.icarus.2010.04.022

Author

Melnikov, A. V. ; Shevchenko, I. I. / The rotation states predominant among the planetary satellites. In: Icarus. 2010 ; Vol. 209, No. 2. pp. 786-794.

BibTeX

@article{cd713e0dc07548d8bce9793dd5f57090,
title = "The rotation states predominant among the planetary satellites",
abstract = "On the basis of tidal despinning timescale arguments, Peale showed in 1977 that the majority of irregular satellites (with unknown rotation states) are expected to reside close to their initial (fast) rotation states. Here we investigate the problem of the current typical rotation states among all known satellites from a viewpoint of dynamical stability. We explore location of the known planetary satellites on the (ω0,e) stability diagram, where ω0 is an inertial parameter of a satellite and e is its orbital eccentricity. We show that most of the satellites with unknown rotation states cannot rotate synchronously, because no stable synchronous 1:1 spin-orbit state exists for them. They rotate either much faster than synchronously (those tidally unevolved) or, what is much less probable, chaotically (tidally-evolved objects or captured slow rotators).",
keywords = "Celestial mechanics, Resonances, Spin-orbit, Rotational dynamics, Satellites, General",
author = "Melnikov, {A. V.} and Shevchenko, {I. I.}",
year = "2010",
month = oct,
day = "1",
doi = "10.1016/j.icarus.2010.04.022",
language = "English",
volume = "209",
pages = "786--794",
journal = "Icarus",
issn = "0019-1035",
publisher = "Elsevier",
number = "2",

}

RIS

TY - JOUR

T1 - The rotation states predominant among the planetary satellites

AU - Melnikov, A. V.

AU - Shevchenko, I. I.

PY - 2010/10/1

Y1 - 2010/10/1

N2 - On the basis of tidal despinning timescale arguments, Peale showed in 1977 that the majority of irregular satellites (with unknown rotation states) are expected to reside close to their initial (fast) rotation states. Here we investigate the problem of the current typical rotation states among all known satellites from a viewpoint of dynamical stability. We explore location of the known planetary satellites on the (ω0,e) stability diagram, where ω0 is an inertial parameter of a satellite and e is its orbital eccentricity. We show that most of the satellites with unknown rotation states cannot rotate synchronously, because no stable synchronous 1:1 spin-orbit state exists for them. They rotate either much faster than synchronously (those tidally unevolved) or, what is much less probable, chaotically (tidally-evolved objects or captured slow rotators).

AB - On the basis of tidal despinning timescale arguments, Peale showed in 1977 that the majority of irregular satellites (with unknown rotation states) are expected to reside close to their initial (fast) rotation states. Here we investigate the problem of the current typical rotation states among all known satellites from a viewpoint of dynamical stability. We explore location of the known planetary satellites on the (ω0,e) stability diagram, where ω0 is an inertial parameter of a satellite and e is its orbital eccentricity. We show that most of the satellites with unknown rotation states cannot rotate synchronously, because no stable synchronous 1:1 spin-orbit state exists for them. They rotate either much faster than synchronously (those tidally unevolved) or, what is much less probable, chaotically (tidally-evolved objects or captured slow rotators).

KW - Celestial mechanics

KW - Resonances, Spin-orbit

KW - Rotational dynamics

KW - Satellites, General

UR - http://www.scopus.com/inward/record.url?scp=77956296265&partnerID=8YFLogxK

U2 - 10.1016/j.icarus.2010.04.022

DO - 10.1016/j.icarus.2010.04.022

M3 - Article

AN - SCOPUS:77956296265

VL - 209

SP - 786

EP - 794

JO - Icarus

JF - Icarus

SN - 0019-1035

IS - 2

ER -

ID: 45988062