It is expected that the upcoming survey by theVera C. Rubin Observatory will discover another 5 million minor planets during the next ten years—almost a tenfold increase from current numbers.[5] While all main-belt asteroids with a diameter above 10 km (6.2 mi) have already been discovered, there might be as many as 10 trillion 1 m (3.3 ft)-sized asteroids or larger out to the orbit of Jupiter; and more than a trillion minor planets in theKuiper belt.[5][6] For minor planets grouped by a particular aspect or property,see§ Specific lists.
The list of minor planets consists of more than 700 partial lists, each containing 1000 minor planets grouped into 10 tables. The data is sourced from theMinor Planet Center (MPC) and expanded with data from theJPL SBDB (mean-diameter), Johnston's archive (sub-classification) and others(see detailed field descriptions below). For an overview of all existing partial lists,see§ Main index.
The information given for a minor planet includes apermanent andprovisional designation(§ Designation), a citation that links to themeanings of minor planet names (only if named), the discovery date, location, and crediteddiscoverers(§ Discovery and§ Discoverers), a category with a more refined classification than the principal grouping represented by the background color(§ Category), a mean-diameter, sourced from JPL'sSBDB or otherwise calculated estimates in italics(§ Diameter), and a reference (Ref) to the corresponding pages at MPC and JPL SBDB.
The MPC may credit one or several astronomers, asurvey or similar program, or even theobservatory site with the discovery. In the first column of the table, an existing stand-alone article is linked in boldface, while (self-)redirects are never linked. Discoverers, discovery site and category are only linked if they differ from the preceding catalog entry.
The example above shows five catalog entries fromone of the partial lists. All five asteroids were discovered atPalomar Observatory by thePalomar–Leiden survey (PLS). The MPC directly credits the survey's principal investigators, that is, the astronomersCornelis van Houten,Ingrid van Houten-Groeneveld andTom Gehrels. (This is the only instance where the list of minor planets diverges from theDiscovery Circumstances in the official MPC list.[7])189004 Capys, discovered on 16 October 1977, is the only named minor planet among these five. Its background color indicates that it is aJupiter trojan (from theTrojan camp at Jupiter'sL5), estimated to be approximately 12 kilometers in diameter. All other objects are smaller asteroids from the inner (white), central (light-grey) and outer regions (dark grey) of theasteroid belt. The provisional designation for all objects is an uncommonsurvey designation.
After discovery, minor planets generally receive aprovisional designation, e.g.1989 AC, then a leading sequential number in parentheses, e.g.(4179) 1989 AC, turning it into a permanent designation (numbered minor planet). Optionally, a name can be given, replacing the provisional part of the designation, e.g.4179 Toutatis. (On Wikipedia, named minor planets also drop their parentheses.)
In modern times, a minor planet receives a sequential number only after it has been observed several times over at least 4 oppositions.[8] Minor planets whose orbits are not (yet) precisely known are known by their provisional designation. This rule was not necessarily followed in earlier times, and some bodies received a number but subsequently becamelost minor planets. The 2000 recovery of719 Albert, which had been lost for nearly 89 years, eliminated the last numbered lost asteroid.[9] Only after a number is assigned is the minor planet eligible to receive a name. Usually the discoverer has up to 10 years to pick a name; many minor planets now remain unnamed. Especially towards the end of the twentieth century, large-scale automated asteroid discovery programs such asLINEAR have increased the pace of discoveries so much that the vast majority of minor planets will most likely never receive names.
For these reasons, the sequence of numbers only approximately matches the timeline of discovery. In extreme cases, such as lost minor planets, there may be a considerable mismatch: for instance the high-numbered69230 Hermes was originally discovered in 1937, but it was lost until 2003. Only after it was rediscovered could its orbit be established and a number assigned.
Top 10discoverers of minor planets account for more than 90% of all discoveries (total of 773,916 numbered bodies, as of 24 February 2025, adjusted MPC-figures).[10][11]
The MPC credits more than 1,000 professional and amateur astronomers asdiscoverers of minor planets. Many of them have discovered only a few minor planets or even just co-discovered a single one. Moreover, a discoverer does not need to be a human being. There are about 300 programs, surveys and observatoriescredited as discoverers. Among these, a small group of U.S. programs and surveys actually account for most of all discoveries made so far(see pie chart). As the total of numbered minor planets is growing by the tens of thousands every year, all statistical figures are constantly changing. In contrast to the Top 10 discoverers displayed in this articles, the MPC summarizes the total of discoveries somewhat differently, that is by a distinct group of discoverers. For example, bodies discovered in thePalomar–Leiden Survey are directly credited to the program's principal investigators.
The vast majority of minor planets are evenly distributed between the inner-, central and outer parts of theasteroid belt, which are separated by the twoKirkwood gaps at 2.5 and 2.82 AU. Nearly 97.5% of all minor planets are main-belt asteroids (MBA), whileJupiter trojans,Mars-crossing andnear-Earth asteroids each account for less than 1% of the overall population. Only a small number ofdistant minor planets, that is thecentaurs andtrans-Neptunian objects, have been numbered so far. In the partial lists, table column "category" further refines this principal grouping:
objects with an exceptionally long or shortrotation period are tagged with "slow" (period of 100+ hours) or "fast" (period of less than 2.2 hours) and link to their corresponding entry inList of slow rotators andList of fast rotators, respectively.[19]
If available, a minor planet'smean diameter in meters (m) or kilometers (km) is taken from theNEOWISE mission of NASA'sWide-field Infrared Survey Explorer, which theSmall-Body Database has also adopted.[21] Mean diameters are rounded to two significant figures if smaller than 100 kilometers. Estimates are in italics and calculated from a magnitude-to-diameter conversion, using an assumedalbedo derived from the body's orbital parameters or, if available, from afamily-specific mean albedo(also seeasteroid family table).[e]
This is an overview of all existing partial lists of numbered minor planets (LoMP). Each table stands for 100,000 minor planets, each cell for a specific partial list of 1,000 sequentially numbered bodies. The data is sourced from theMinor Planet Center.[1] For an introduction,see§ top.
^There are two sources used to determineasteroid families by the synthetichierarchical clustering method. The first one,Identification and Dynamical Properties of Asteroid Families (D. Nesvorný, 2014), is used for asteroids up to number 393,347. The second one is from theAsteroid Dynamic Site (AstDyS) and covers theindividual asteroid family membership for bodies above that number (A. Milani, Z. Knežević, 2014), including all listed bodies that have been numbered since last publication in 2018. Following 8 families from latter were mapped to family names of former: Hertha→Nysa, Minerva→Gefion, Klytaemnestra→Telramund, Lydia→Padua, Innes→Rafita, Zdenekhorsky→Nemesis, Klumpkea→Tirela, Gantrisch→Lixiaohua, Harig→Witt. All other families not listed by Nesvorný at AstDyS do not show an abbreviated family name with a linked "Family Identification Number" (FIN). Instead, listed entries for such members give the designation of their parent body, e.g. (5) for 5 Astraea.
^abSplit-up of NEOs into Amor, Aten, Apollo and Atira asteroid is based on the orbital criteria given in adjunct table. The data is sourced from JPL Small-Body Orbital Elements"Numbered Asteroids (50 MB)" file
^There are a few minor planets that remain unclassified based on the defined orbital criteria. At least five of these bodies have a semi-major axis too large to be an outer main-belt asteroid, and an orbit too eccentric to be classified as a Jupiter trojan (JPL classifies these bodies simply as "asteroids", while the MPC, which never distinguishes between inner, outer and middle MBAs, classifies them as "main-belt asteroids"). Other unclassified minor planets include Mars-crossers (as per MPC) with a semi-major axis of that of an outer-MBA (as per JPL).
^This table adopts the orbital criteria used by theJPL Small-Body Database, with the exception of (1.) using a different limit to categorize asteroids of the intermediate main belt (i.e.a = 2.5–2.82 AU), and (2.) adding another orbital criteria to outer MBAs (q > 1.666 AU). The values for an object's perihelion andaphelion need to be derived from the semi-major axis and theeccentricity as they are not provided in the data source (q = a(1-e); Q = a(1+e)).
^Diameters are calculated as a function ofabsolute magnitude (H) andgeometric albedo (p) as documented atCNEOS. While "H" is taken from theAscii files at the Small Body Data Base, the assumed albedo is taken from an asteroid-family specific figure (Nesvorny, syntheticHCM v.3, as shown intable) or, alternatively – forbackground asteroids,Jupiter trojans,near-Earth anddistant objects – from the body's orbital parameters (as per2. Taxonomic Class, orbital class, and albedo at theLCDB and/orJohnston's Archive). This is: 0.20 (inner MBAs), 0.14 (NEOs), 0.057 (outer MBAs and Jupiter trojans), 0.10 (middle MBAs with a semi-major axis between 2.6 and 2.7 AU), 0.09 (centaurs and TNOs). The conversion formula for a given albedo and abs. magnitude is: pow(10, (3.1236 − (0.5 × log10(p)) − (0.2 × H))).
^An opposition is the time when a body is at its furthest apparent point from the Sun, and in this case is defined as the time when an asteroid is far enough from the Sun to be observed from the Earth. In most cases, this is about 4 to 6 months a year. Some notable minor planets are exceptions to this rule, such as367943 Duende.
Dictionary of Minor Planet Names, 5th ed.:Prepared on Behalf of Commission 20 Under the Auspices of the International Astronomical Union,Lutz D. Schmadel,ISBN3-540-00238-3
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