Orbital Evolution of Planetesimals due to the Galactic Tide: Formation of the Comet Cloud

2007 ◽  
Vol 134 (4) ◽  
pp. 1693-1706 ◽  
Author(s):  
A. Higuchi ◽  
E. Kokubo ◽  
H. Kinoshita ◽  
T. Mukai
Keyword(s):  
Orbital Evolution ◽  
Galactic Tide

scholarly journals Anisotropy of long-period comets explained by their formation process

2020 ◽  
Author(s):  
Arika Higuchi
Keyword(s):  
Analytical Solutions ◽  
Formation Process ◽  
Ecliptic Plane ◽  
Radial Component ◽  
Orbital Evolution ◽  
Oort Cloud ◽  
Long Period ◽  
Numerical Integrations ◽  
Galactic Tide ◽  
Galactic Longitude

<p>Long-period comets coming from the Oort cloud are thought to be<span class="Apple-converted-space"> </span>planetesimals formed in the planetary region on the ecliptic plane.<span class="Apple-converted-space"> </span>We have investigated the orbital evolution of these bodies<span class="Apple-converted-space"> </span>due to the Galactic tide.<span class="Apple-converted-space"> </span>We extended Higuchi et al. (2007) and derived the<span class="Apple-converted-space"> </span>analytical solutions to the Galactic longitude and latitude of<span class="Apple-converted-space"> </span>the direction of aphelion, <em>L</em> and <em>B</em>.<span class="Apple-converted-space"> </span>Using the analytical solutions,<span class="Apple-converted-space"> </span>we show that the ratio of the periods of the evolution of <em>L</em> and <em>B</em> is very close to either 2 or ∞ for initial eccentricities <em>e</em><sub>i</sub>∼1,<span class="Apple-converted-space"> </span>as is true for the Oort cloud comets.<span class="Apple-converted-space"> </span>From the relation between <em>L</em> and <em>B</em>, we predict that Oort cloud comets returning to the planetary region concentrate on the ecliptic plane<span class="Apple-converted-space"> </span>and a second plane, which we call the "empty ecliptic".<span class="Apple-converted-space"> </span>This consists in a rotation of 180<sup>°</sup> of the ecliptic around the Galactic pole. Our numerical integrations confirm that the radial component of the Galactic tide, which is neglected in the derivation of the analytical solutions,<span class="Apple-converted-space"> </span>is not strong enough to break the relation between <em>L</em> and <em>B</em> derived analytically. Brief examination of observational data shows<span class="Apple-converted-space"> </span>that there are concentrations near both the ecliptic and the empty ecliptic. We also show that the anomalies of the distribution of <em>B</em> of long-period comets mentioned by several authors are explained by the concentrations on the two planes more consistently than the previous explanation.</p>

Results in orbital evolution of objects in the geosynchronous region

1990 ◽  
Author(s):  
LARRY FRIESEN ◽  
ALBERT JACKSON, IV ◽  
HERBERT ZOOK ◽  
DONALD KESSLER
Keyword(s):  
Orbital Evolution

scholarly journals Tidal interactions in rotating multiple stars and their impact on their evolution

2014 ◽  
Vol 9 (S307) ◽  
pp. 208-210
Author(s):  
P. Auclair-Desrotour ◽  
S. Mathis ◽  
C. Le Poncin-Lafitte
Keyword(s):  
Fluid Model ◽  
Orbital Evolution ◽  
Tidal Dissipation ◽  
Tidal Waves ◽  
Physical Mechanisms ◽  
Tidal Interactions ◽  
The Earth ◽  
Half Height ◽  
Multiple Stars ◽  
Stellar Interiors

AbstractTidal dissipation in stars is one of the key physical mechanisms that drive the evolution of binary and multiple stars. As in the Earth oceans, it corresponds to the resonant excitation of their eigenmodes of oscillation and their damping. Therefore, it strongly depends on the internal structure, rotation, and dissipative mechanisms in each component. In this work, we present a local analytical modeling of tidal gravito-inertial waves excited in stellar convective and radiative regions respectively. This model allows us to understand in details the properties of the resonant tidal dissipation as a function of the excitation frequencies, the rotation, the stratification, and the viscous and thermal properties of the studied fluid regions. Then, the frequencies, height, width at half-height, and number of resonances as well as the non-resonant equilibrium tide are derived analytically in asymptotic regimes that are relevant in stellar interiors. Finally, we demonstrate how viscous dissipation of tidal waves leads to a strongly erratic orbital evolution in the case of a coplanar binary system. We characterize such a non-regular dynamics as a function of the height and width of resonances, which have been previously characterized thanks to our local fluid model.

Long-term effects of the Galactic tide on cometary dynamics

2006 ◽  
Vol 95 (1-4) ◽  
pp. 299-326 ◽  
Author(s):  
Marc Fouchard ◽  
Christiane Froeschlé ◽  
Giovanni Valsecchi ◽  
Hans Rickman
Keyword(s):  
Long Term Effects ◽  
Galactic Tide

Influence of a hyperbolic flyby of a small mass on the orbital evolution of a massive binary

1987 ◽  
Vol 41 (1-4) ◽  
pp. 313-321 ◽  
Author(s):  
L. K. Babadzanjanz ◽  
V. A. Brumberg
Keyword(s):  
Small Mass ◽  
Orbital Evolution

scholarly journals Tidal dissipation in rotating low-mass stars and implications for the orbital evolution of close-in planets

2017 ◽  
Vol 604 ◽  
pp. A112 ◽  
Author(s):  
F. Gallet ◽  
E. Bolmont ◽  
S. Mathis ◽  
C. Charbonnel ◽  
L. Amard
Keyword(s):  
Orbital Evolution ◽  
Low Mass Stars ◽  
Tidal Dissipation ◽  
Low Mass
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