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Among the numbered minor planets with an unambiguous period solution are (459872) 2014 EK 24, a 60-meter sized stony NEO with a period of 352 seconds, as well as (335433) 2005 UW 163 and (60716) 2000 GD 65, two main-belt asteroids, with a diameter of 0.86 and 2.25 kilometers and a period of 1.29 and 1.95 hours, respectively (see full list).
Since then numerous binary asteroids and several triple asteroids have been detected. [1] The mass ratio of the two components – called the "primary" and "secondary" of a binary system – is an important characteristic. Most binary asteroids have a large mass ratio, i.e. a relatively small satellite in orbit around the main component.
Therefore, this article will restrict itself for the most part to the classical asteroids: objects of the asteroid belt, Jupiter trojans, and near-Earth objects. For almost two centuries after the discovery of Ceres in 1801, all known asteroids spent most of their time at or within the orbit of Jupiter, though a few, such as 944 Hidalgo ...
2021 PH 27 has the smallest semi-major axis and shortest orbital period among all known asteroids as of 2021, [7] with a velocity at perihelion of 106 km/s (240,000 mph). [5] It also has the largest relativistic perihelion shift of any object orbiting the Sun, 1.6 times that of Mercury. [ 8 ]
The Eunomia or Eunomian family (FIN: 502) is a large asteroid family of S-type asteroids named after the asteroid 15 Eunomia.It is the most prominent family in the intermediate asteroid belt and the 6th-largest family with nearly six thousand known members, or approximately 1.4% of all asteroids in the asteroid belt.
These are lists of asteroids, e.g. by discoverer or by number. See list of minor planets for an overview and numbering and naming conventions . Pages in category "Lists of asteroids"
Common orbital subgroups of Near-Earth Objects (NEOs). Atira asteroids / ə ˈ t ɪr ə / or Apohele asteroids, also known as interior-Earth objects (IEOs), are Near-Earth objects whose orbits are entirely confined within Earth's orbit; [1] that is, their orbit has an aphelion (farthest point from the Sun) smaller than Earth's perihelion (nearest point to the Sun), which is 0.983 astronomical ...
When the mean orbital period of an asteroid is an integer fraction of the orbital period of Jupiter, a mean-motion resonance with the gas giant is created that is sufficient to perturb an asteroid to new orbital elements. Primordial asteroids entered these gaps because of the migration of Jupiter's orbit. [87]