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Observational results for five short-period and five long-period comets
Planetary and Space Science, 2020 Abstract In this work we studied the activity of a group of long and short period comets at different heliocentric distances in order to explore and compare their dust production and characteristics. The targets observed were the comets 22P/Kopff, 29P/Schwassmann-Wachmann 1, 218P/LINEAR, 221P/LINEAR, 318P/McNaught-Hartley, C/2010 FB87 (WISE-Garradd),
Garcia, Romina Soledad +2 more
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Celestial Mechanics and Dynamical Astronomy, 1992
Reasons for interest in the origin of short-period comets and the difficulties of computing their long-term dynamical evolution are reviewed. The relative advantages of a source region in an extended ‘inner core’ of the Oort cloud or a compact ‘comet belt‘ just beyond the planetary system are finely balanced, and it is premature to consider the problem
M E Bailey, Bailey M E
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Reasons for interest in the origin of short-period comets and the difficulties of computing their long-term dynamical evolution are reviewed. The relative advantages of a source region in an extended ‘inner core’ of the Oort cloud or a compact ‘comet belt‘ just beyond the planetary system are finely balanced, and it is premature to consider the problem
M E Bailey, Bailey M E
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Invisible comets on evolutionary track of short-period comets
Celestial Mechanics and Dynamical Astronomy, 1992We systematically surveyed the orbits of short-period (SP) comets that show a large change of perihelion distance (q) between 1-2 AU (visible comets) and 4-5 AU (invisible comets) during 4400 years. The data are taken from Cosmo-DICE (Nakamura and Yoshikawa 1991a), which is a long-term orbital evolution project for SP comets.
Makoto Yoshikawa, Nakamura Tsuko
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The origin of short-period comets
Icarus, 1990Abstract Recent work has shown that if short-period comets predominantly occur as a result of planetary “captures” of long-period comets, the relevant source flux of nearly parabolic orbits must involve comets with perihelia in the range 5–30 AU, significantly beyond the region in which the flux is observationally constrained. The numbers and orbital
Mark E. Bailey, Chris R. Stagg
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Meteor contribution by short-period comets
1988The contribution of P/Halley and other comets to the meteor streams are discussed. Particular attention is given to the meteoric production by P/Encke as the potential major contributor to the meteoric complex in the inner part of the solar system. The density and total mass of the meteoric stream associated with P/Encke is derived, taking into account
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New edition of the catalogue of short-period comets
Earth, Moon, and Planets, 1995The Institute of Theoretical Astronomy in St. Petersburg and the Astronomical Institute in Bratislava are preparing a new edition of the Catalogue of short-period comets. This edition will be supplemented by short-period comets discovered after the year 1983 and comprises some new features, e. g. the evolution of orbital elements between the years 1750
Y. D. Medvedev +2 more
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Thermal evolution and differentiation of a short-period comet
Planetary and Space Science, 1993Abstract The evolution of the subsurface layers of a short-period comet has been studied. The structure and composition of the surface layers due to sublimation recondensation phenomena, to gas diffusion processes through the pore system and to the ejection of dust particles have been investigated in detail. The nucleus has been modelled as a mixture
S. Espinasse +6 more
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Hypothetical evolutions of short-period comets
Symposium - International Astronomical Union, 1996The hypothetical model of capture I consider is as follows: a comet with an initial conic orbit, meets close to one of its vertices an outer planet and generates one or several little comets (crossing of the Roche limit) with an elliptic orbit. This initial vertex always remains one of the vertices of the captured orbit by the Solar System.
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The distribution of short-period comet magnitudes
Earth, Moon, and Planets, 1987Short-period comets with P ≤ 15 yr represent one of the most complete comet samples. The magnitude distribution of these comets was analysed using a maximum likelihood method. The brightness (magnitude) index for the comets with H 10 ≤ 11 mag was estimated together with the large sample errors and found to be 0.62 ± 0.09.
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