| Issue |
A&A
Volume 381, Number 3, JanuaryIII 2002
|
|
|---|---|---|
| Page(s) | 1059 - 1065 | |
| Section | Celestial mechanics and astrometry | |
| DOI | https://doi.org/10.1051/0004-6361:20011587 | |
| Published online | 15 January 2002 | |
Hyperion-Iapetus: Collisional relationships
1
Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio 2, 35122 Padova, Italy
2
Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio 2, 35122 Padova, Italy e-mail: barbieri@pd.astro.it
3
Dipartimento di Fisica, Università di Pisa, piazza Torricelli 2, 56127 Pisa, Italy e-mail: aldo@astr15pi.difi.unipi.it
4
Dipartimento di Fisica, Università di Pisa, piazza Torricelli 2, 56127 Pisa, Italy e-mail: paolicchi@df.unipi.it
Corresponding author: S. Marchi, marchi@pd.astro.it
Received:
29
June
2001
Accepted:
25
October
2001
In this paper, we will deal with one of the most fascinating problems of the Solar System: the origin of the double face of Iapetus, where one half of the satellite is significantly brighter than the other. The “transfer of mass” process (see Marchi et al. [CITE]) may be a viable explanation for the visible dichotomy. In this process a satellite undergoes mass transfer from other satellites belonging to the same system. We analyze the pair Hyperion–Iapetus and suggest a possible explanation for the formation of the dark region, which is also known as Cassini Regio.
Key words: minor planets, asteroids / solar system: general
© ESO, 2002
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