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Capture and escape in the elliptic restricted three-body problem
Several families of irregular moons orbit the giant planets. These moonsare thought to have been captured into planetocentric orbits afterstraying into a region in which the gravitation of the planet dominatessolar perturbations (the Hill sphere). This mechanism requires a sourceof dissipation, such as gas drag, in order to make capture permanent.However, capture by gas drag requires that particles remain inside theHill sphere long enough for dissipation to be effective. Recently wehave proposed that in the circular restricted three-body problem (CRTBP)particles may become caught up in sticky chaotic layers, which tends toprolong their sojourn within the Hill sphere of the planet therebyassisting capture. Here, we show that this mechanism survivesperturbations due to the ellipticity of the orbit of the planet.However, Monte Carlo simulations indicate that the ability of the planetto capture moons decreases with increasing orbital eccentricity. At theactual orbital eccentricity of Jupiter, this results in approximately anorder of magnitude lower capture probability than estimated in thecircular model. Eccentricities of planetary orbits in the Solar systemare moderate but this is not necessarily the case for extrasolarplanets, which typically have rather eccentric orbits. Therefore, ourfindings suggest that these extrasolar planets are unlikely to havesubstantial populations of irregular moons.
| H-beta photometry of northern intermediate galactic latitude early-type stars and galactic structure away from the plane
Photoelectric H-beta photometry is presented for 255 early-type stars atintermediate galactic latitudes. Absolute magnitudes and distances arederived for the more luminous stars. Those with visual magnitudes lessthan or equal to 2.5 and at distances of up to 1 kpc from the galacticplane may follow the spiral structure in the plane.
| UBV photometry and MK spectral classification of northern early-type stars at intermediate galactic latitudes
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977MNRAS.180..691H&db_key=AST
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Membre dels grups següents:
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Dades d'Observació i Astrometria
| Constel·lació: | Cepheus |
| Ascensió Recta: | 22h01m02.23s |
| Declinació: | +66°04'56.9" |
| Magnitud Aparent: | 8.269 |
| Distancia: | 3571.429 parsecs |
| Moviment propi RA: | -4.5 |
| Moviment propi Dec: | -1.8 |
| B-T magnitude: | 8.394 |
| V-T magnitude: | 8.28 |
Catàlegs i designacions:
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