The **Hilda asteroids** (adj. *Hildian*) are a dynamical group of more than 4000 asteroids located beyond the asteroid belt in a 3:2 orbital resonance with Jupiter.^{[1]}^{[2]} The namesake is the asteroid 153 Hilda. Hildas move in their elliptical orbits so that their aphelia put them opposite Jupiter (at L_{3}), or 60° ahead of or behind Jupiter at the L_{4} and L_{5} Lagrangian points.^{[3]} Over three successive orbits each Hilda asteroid approaches all of these three points in sequence. A Hilda's orbit has a semi-major axis between 3.7 and 4.2 AU (the average over a long time span is 3.97), an eccentricity less than 0.3, and an inclination less than 20°.^{[4]} Two collisional families exist within the Hilda group: the **Hilda family** and the Schubart family. The namesake for the latter family is 1911 Schubart.^{[5]}

Hildas' surface colors often correspond to the low-albedo D-type and P-type; however, a small portion are C-type. D-type and P-type asteroids have surface colors, and thus also surface mineralogies, similar to those of cometary nuclei. This implies that they share a common origin.^{[4]}^{[6]}

The asteroids of the Hilda group (Hildas) are in 3:2 mean-motion resonance with Jupiter.^{[4]} That is, their orbital periods are 2/3 that of Jupiter. They move along the orbits with a semimajor axis near 4.0 AU and moderate values of eccentricity (up to 0.3) and inclination (up to 20°). Unlike the Jupiter trojans they may have any difference in longitude with Jupiter, nevertheless avoiding dangerous approaches to the planet.

The Hildas taken together constitute a dynamic triangular figure with slightly convex sides and trimmed apices in the triangular libration points of Jupiter—the "Hildas Triangle".^{[3]} The "asteroidal stream" within the sides of the triangle is about 1 AU wide, and in the apexes this value is 20-40% greater. Figure 1 shows the positions of the Hildas (black) against a background of all known asteroids (gray) up to Jupiter's orbit at January 1, 2005.^{[7]}

Each of the Hilda objects moves along its own elliptic orbit. However, at any moment the Hildas together constitute this triangular configuration, and all the orbits together form a predictable ring. Figure 2 illustrates this with the Hildas positions (black) against a background of their orbits (gray). For the majority of these asteroids, their position in orbit may be arbitrary, except for the external parts of the apexes (the objects near aphelion) and the middles of the sides (the objects near perihelion). The Hildas Triangle has proven to be dynamically stable over a long time span.^{[citation needed]}

The typical Hilda object has a retrograde perihelion motion. On average, the velocity of perihelion motion is greater when the orbital eccentricity is lesser, while the nodes move more slowly. All typical objects in aphelion would seemingly approach closely to Jupiter, which should be destabilising for them—but the variation of the orbital elements over time prevents this, and conjunctions with Jupiter occur only near the perihelion of Hilda asteroids. Moreover, the apsidal line oscillates near the line of conjunction with different amplitude and a period of 2.5 to 3.0 centuries.

In addition to the fact that the Hildas triangle revolves in sync with Jupiter, the density of asteroids in the stream exhibits quasi-periodical waves. At any time, the density of objects in the triangle's apexes is more than twice the density within the sides. The Hildas "rest" at their aphelia in the apexes for an average of 5.0-5.5 years, whereas they move along the sides more quickly, averaging 2.5 to 3.0 years. The orbital periods of these asteroids are approximately 7.9 years, or two thirds that of Jupiter.

Although the triangle is nearly equilateral, some asymmetry exists. Due to the eccentricity of Jupiter's orbit, the side L_{4}-L_{5} slightly differs from the two other sides. When Jupiter is in aphelion, the mean velocity of the objects moving along this side is somewhat smaller than that of the objects moving along the other two sides. When Jupiter is in perihelion, the reverse is true.

At the apexes of the triangle corresponding to the points L_{4} and L_{5} of Jupiter's orbit, the Hildas approach the Trojans. At the mid-sides of the triangle, they are close to the asteroids of the external part of the asteroid belt. The velocity dispersion of Hildas is more evident than that of Trojans in the regions where they intersect. The dispersion of Trojans in inclination is twice that of the Hildas. Due to this, as much as one quarter of the Trojans cannot intersect with the Hildas, and at all times many Trojans are located outside Jupiter's orbit. Therefore, the regions of intersection are limited. This is illustrated by the adjacent figure that shows the Hildas (black) and the Trojans (gray) along the ecliptic plane. One can see the spherical form of the Trojan swarms.

When moving along each side of the triangle, the Hildas travel more slowly than the Trojans, but encounter a denser neighborhood of outer-asteroid-belt asteroids. Here, the velocity dispersion is much smaller.

The observed peculiarities in the Hildas' motion are based on data for a few hundred objects known to date and generate still more questions. Further observations are needed to expand on the list of Hildas. Such observations are most favorable when Earth is near conjunction with the mid-sides of the Hildas Triangle. These moments occur each 4 and 1/3 months. In these circumstances the brilliance of objects of similar size could run up to 2.5 magnitudes as compared to the apexes.^{[citation needed]}

The Hildas traverse regions of the Solar system from approximately 2 AU up to Jupiter's orbit. This entails a variety of physical conditions and the neighborhood of various groups of asteroids. On further observation some theories on the Hildas may have to be revised.^{[citation needed]}

**^**"Objects with orbit type Hilda – Database query".*Minor Planet Center*. Retrieved 14 September 2018.**^**Broz, M.; Vokrouhlický, D. (October 2008). "Asteroid families in the first-order resonances with Jupiter".*Monthly Notices of the Royal Astronomical Society*.**390**(2): 715–732. arXiv:1104.4004. Bibcode:2008MNRAS.390..715B. doi:10.1111/j.1365-2966.2008.13764.x.- ^
^{a}^{b}Matthias Busch. "The triangle formed by the Hilda asteroids". EasySky. Retrieved 2009-12-15. - ^
^{a}^{b}^{c}Ohtsuka, Katsuhito; Yoshikawa, M.; Asher, D. J.; Arakida, H.; Arakida, H. (October 2008). "Quasi-Hilda comet 147P/Kushida-Muramatsu. Another long temporary satellite capture by Jupiter".*Astronomy and Astrophysics*.**489**(3): 1355–1362. arXiv:0808.2277. Bibcode:2008A&A...489.1355O. doi:10.1051/0004-6361:200810321. **^**Brož, M.; Vokrouhlický, D. (2008). "Asteroid families in the first-order resonances with Jupiter".*Monthly Notices of the Royal Astronomical Society*.**390**(2): 715–732. arXiv:1104.4004. Bibcode:2008MNRAS.390..715B. doi:10.1111/j.1365-2966.2008.13764.x.**^**Gil-Hutton, R.; Brunini, Adrián (2008). "Surface composition of Hilda asteroids from the analysis of the Sloan Digital Sky Survey colors".*Icarus*.**193**(2): 567–571. Bibcode:2008Icar..193..567G. doi:10.1016/j.icarus.2007.08.026. Retrieved 14 April 2014.**^**L'vov V.N., Smekhacheva R.I., Smirnov S.S., Tsekmejster S.D. Some peculiarities in the Hildas motion. Izv. Pulkovo Astr. Obs., 2004, 217, 318-324 (in Russian)