(5201) Ferraz-Mello (=1983
© S.Ferraz-Mello (IAG-USP)
Unusual asteroid discovered by Ted Bowell at Anderson Mesa Station (Lowell Observatory) on December 1st, 1983. May be an inactive Jupiter- family comet (T=2.972) in a very eccentric orbit (e=0.54). The orbit perihelion (q= 1.53 AU) and aphelion (Q= 4.82 AU) lie near the orbits of Mars and Jupiter, respectively. Recent observations with the SOAR (Southern Astrophyisics Research Telescope) Optical Imager using four SDSS filters has given strong indication that (5201) is a dormant or extinct comet.
Where is it now? (Allow 1-2 minutes to download the orbits. After that, you may play and see the next approaches to Jupiter and Mars.)
What's its current position in the sky?
Magnitude and Size: The absolute magnitude is H=14.8. The effective diameter may be estimated through the formula: log D = 3.12 - 0.5 log A - 0.2 H. The albedo of asteroids in that region of the belt are A~0.03-0.06 and thus D~6-8 km.
Recent close approaches to Jupiter and Mars:
MJD 53993.0 (Sep. 14, 2006) 0.451 AU (67.5 Gm) from Mars
MJD 54872.1 (Feb. 09, 2009) 0.358 AU (53.5 Gm) from Jupiter
Dynamics: The asteroid is currently (and will remain till ca. 2300) in the 2/1 resonance with Jupiter as shown by the evolution of the critical angle:
A succession of approaches to Jupiter and Mars: CHAOS!
While s is far from 180 deg, the asteroid cannot approach Jupiter; however at every half libration period, s approaches 180 deg, and at those dates a close approach to Jupiter becomes possible. The libration period is close to 175 yrs, and we may count 8 approaches in the next 600 years, most of them below 0.3 AU and the last of them close to 0.2 AU. The motion lies at the border of the 2/1 resonance and the above libration diagram shows that at each half libration period, the motion approaches a saddle point and is chaotic. As a consequence the actual evolution after some approaches is unpredictable. In several runs before the one shown above, the behavior was only "almost" the same. Always the closest approximation to Jupiter occurs in 500 to 700 years, with values that may be even much closer that the one shown above. The transition shown after year 2700 was seen in every simulation, always showing a large increase in the semi-major axis.
The simulation included all planets from Venus to Neptune. The distance to Mars after yr 2700 is not shown since close approaches no longer occur because the large semi-major axis and smaller eccentricity. The labels of the curves are the same shown in the plot of the next approaches.
After! The unpredictability of the motion makes any run for a longer time senseless. However, even if only of qualitative interest, in the present simulation, the motion in the millennium starting in yr 3000, after the big transition shown in the above figure, is co-orbital:
The projection of the motion on the ecliptic is shown in a heliocentric reference frame co-rotating with Jupiter. Jupiter's position is shown by a cross.
The past: A monotonous succession of very-high-amplitude s-librations. The last circulation happened around yr -800. No approaches to Jupiter less than 0.3 AU in this period (the last one, 0.365 AU, in 1926.36). Many close approaches (down to 0.07 AU) to Mars.
(The labels of the curves are the same shown in the plot showing the next approaches.)
References in the literature:
- 1983 XF, (Bowell, E.; Mrkos, A.; Everhart, E.) IAU Circular 3905, 2 (1984).
- Asteroids in cometary orbits (Hahn, G.; Rickman, H.) Icarus, vol. 61, pp 417-442. (1985) (abstract)
- A study of the pre-discovery motion of the two asteroids 1983 SA and 1983 XF (Benest, D.; Bien, R.; Rickman, H.) In "Dynamics of comets: Their origin and evolution". Proceedings of IAU Coloquium 83, Rome, Italy, June 11-15, 1984 (A86-37726 17-90). Dordrecht, D. Reidel Publishing Co., 1985, pp. 365-370. (link to ADS)
- Relation between small bodies - Discussion (Rickman, Hans), Celestial Mechanics,vol. 43, pp.413-416 (1988) Alexander von Humboldt Colloquium on Celestial Mechanics: Long Term Evolution of Planetary Systems, Ramsau, Austria, Mar. 14-18, 1988].(link to ADS).
- Dynamics of planet-crossing asteroids: Classes of orbital behavior. Project SPACEGUARD (Milani,A., Carpino, M., Hahn, G., Nobili, A.M.) Icarus, vol. 78, pp. 212-269, 1989 (abstract)
- Evolution of comets into asteroids (Weissman, Paul R.; A'Hearn, Michael F.; Rickman, H.; McFadden, L. A.) In "Asteroids II", R.P.Binzel, T.Gehrels, M.S. Matthews (eds.), University of Arizona Press, Tucson, p. 880-920, 1989. (abstract)
- Asteroids in the 2 : 1 resonance with Jupiter: dynamics and size distribution (Roig, F.; Nesvorný, D.; Ferraz-Mello, S.) Monthly Notices of the Royal Astronomical Society, Volume 335, pp. 417-431, 2002 (link to ADS)
- Evolution of Comets into Asteroids (Weissman, P. R.; Bottke, W. F., Jr.; Levison, H. F.) In "Asteroids III", W. F. Bottke Jr., A. Cellino, P. Paolicchi, and R. P. Binzel (eds), University of Arizona Press, Tucson, p.669-686, 2002.(link to LPI)
- Asteroid encounters suitable for mass determinations.(A. Galád; B. Gray) Astronomy and Astrophysics. 391, 1115-1122(2002) (link to ADS)
- Yarkovsky origin of the unstable asteroids in the 2/1 mean motion resonance with Jupiter (Brož, M.; Vokrouhlický, D.; Roig, F.; Nesvorný, D.; Bottke, W. F.; Morbidelli, A) Monthly Notices of the Royal Astronomical Society, Volume 359, pp. 1437-1455, 2005 (link to ADS)
- Jupiter approaching asteroids and their possibilities for activity (A. Galád) Astronomisches Nachrichten, Volume 326, pp. 709-715, 2005 (link to ADS)
- Physical and dynamical characterization of (5201) Ferraz-Mello, a possible extinct Jupiter family comet (J.Carvano, S.Ferraz-Mello and D.Lazzaro). Astronomy and Astrophysics, 489, 811-817 (2008) (link to ADS)
- Modelling the effects of a faint dust coma on asteroid spectra (J.M.Carvano and S.Lorenz-Martins) Icy Bodies of the Solar System, IAU Symposium, 263, 223-226 (2010) (link to ADS)