About the Hill stability of extrasolar planets in stellar binary systems

We use a three dimensional generalization of Szebehely’s invariant relation obtained by us (Makó and Szenkovits, Celest. Mech. Dyn. Astron. 90 , 51, 2004) in the elliptic restricted three-body problem, to establish more accurate criterion of the Hill stability. By using this criterion, the Hill stab...

Ausführliche Beschreibung

Gespeichert in:

Bibliographische Detailangaben
Veröffentlicht in:	Celestial mechanics and dynamical astronomy 2008-07, Vol.101 (3), p.273-287
Hauptverfasser:	Szenkovits, Ferenc, Makó, Zoltán
Format:	Artikel
Sprache:	eng
Schlagworte:	Aerospace Technology and Astronautics Astrophysics Astrophysics and Astroparticles Binary stars Classical Mechanics Dynamical Systems and Ergodic Theory Extrasolar planets Geophysics/Geodesy Original Article Physics Physics and Astronomy Solar system Stability criteria Stars & galaxies Three body problem
Online-Zugang:	Volltext
Tags:	Tag hinzufügen Keine Tags, Fügen Sie den ersten Tag hinzu!

Beschreibung
Zusammenfassung:	We use a three dimensional generalization of Szebehely’s invariant relation obtained by us (Makó and Szenkovits, Celest. Mech. Dyn. Astron. 90 , 51, 2004) in the elliptic restricted three-body problem, to establish more accurate criterion of the Hill stability. By using this criterion, the Hill stability of four extrasolar planets ( γ Cephei Ab, Gliese 86 Ab, HD 41004 Ab and HD 41004 Bb) is investigated.
ISSN:	0923-2958 1572-9478
DOI:	10.1007/s10569-008-9144-7