(35107) 1991 VH

(provisional designation ) is a binary near-Earth asteroid and potentially hazardous asteroid of the Apollo group. It was discovered on 9 November 1991, by Australian astronomer Robert McNaught at Siding Spring Observatory. This binary system is composed of a roughly-spheroidal primary body about one kilometre in diameter, and an elongated natural satellite less than half a kilometre in diameter.

The system is unusual for its dynamically excited state; the satellite has a tumbling, non-synchronous rotation that chaotically exchanges energy and angular momentum with its precessing, eccentric orbit. The cause of this is not known however a likely scenario is that (35107) 1991 VH had a close planetary encounter with Earth within ~50,000 to 80,000 kilometers. Another idea, though very unlikely, is that (35107) 1991 VH experience a significant collision event within the past million years.

This asteroid system was one of the two targets of NASA's ''Janus Mayhem'' mission, until the delay of the rocket launch made both targets inaccessible.

Numbering and naming

This minor planet was numbered by the Minor Planet Center on 27 February 2002. It has not yet been named.

Orbit

orbits the Sun at a distance of 0.98–1.30  AU once every 1.21 years (443 days). Its orbit has an eccentricity of 0.14 and an inclination of 14 ° with respect to the ecliptic.

Close approaches

The asteroid has an Earth minimum orbital intersection distance of , which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being or 17.8 LD on 15 August 2008.

Physical characteristics

Diameter, shape, and albedo

High-resolution radar imaging from Goldstone and Arecibo Observatory in 2008 show that the primary is a roughly-spheroidal object with an equatorial ridge, bearing resemblance to a spinning top. This shape is not unique to as it been observed in other near-Earth asteroids; most notably 3200 Phaethon, 66391 Moshup, 101955 Bennu, and 162173 Ryugu. A number of topographical features, including a -wide concavity, are present along the object's equatorial ridge. A bright linear feature casting a shadow at the object's mid- to high-latitudes was also seen in the 2008 radar images.

Preliminary modeling of the primary's shape in radar images indicates dimensions of , or a volume-equivalent diameter of . The geometric albedo for the primary is 0.17–0.18, considerably lower than infrared-based estimates of 0.30–0.40.

Mass and density

The total mass of the system is , based on the orbital motion of the satellite. The mass ratio of the satellite to the primary is , corresponding to a primary mass of —approximately 12 times as massive as the satellite. Given the primary mass and diameter, its density is estimated to be about , indicative of a rubble pile internal structure.

Spectral type

In the SMASS taxonomy, is classified as a transitional Sk-type, which is an intermediary between the common stony S-type and the less frequent K-type asteroids.

Rotation

Photometric observations in 1997 determined a primary rotation period of 2.624 hours, with a light curve amplitude of magnitudes (). Later photometric observations from 2003–2020 corroborated this result down to a precision of ±0.0001 seconds.

Satellite

is the secondary component and natural satellite of the system.

Discovery

is among the first near-Earth asteroid satellites discovered, alongside those of and 3671 Dionysus. It was discovered on 27 February 1997, by astronomers Petr Pravec, Marek Wolf, and Lenka Šarounová at Ondřejov Observatory. The satellite was detected through photometric observations of periodic dips in the system's brightness, caused by mutual eclipses and occultations of the components. The discovery of the satellite was reported in a notice published by the International Astronomical Union on 29 March 1997, but was not officially confirmed until it was individually resolved in adaptive optics imaging by the Keck II telescope at Mauna Kea Observatory on 9 August 2008. The satellite was given the provisional designation on 19 September 2008.

Origin

As with many binary near-Earth asteroids, the system is thought to have formed through rotational fissioning of a progenitor body due to spin-up by the YORP effect. The resulting mass shed from the progenitor body coalesced in orbit to form the satellite.

Exploration

This asteroid system was the target of NASA's ''Janus Mayhem'' mission, which was planned to launch in 2022 alongside NASA's ''Psyche'' spacecraft, and to arrive in 2026. became impossible to reach for ''Janus'' when the launch of Psyche got delayed in May 2022.

See also

* , binary near-Earth asteroid and former target of the ''Janus Serenity'' mission, until it became inaccessible due to the launch delay

Notes

References

External links

Asteroid (35107) 1991 VH
''Small Bodies Data Ferret'', NASA

LCDB Data for (35107) 1991 VH
''Asteroid Lightcurve Database''

Photometric observations of the unrelaxed binary near-Earth asteroid (35107) 1991 VH in support of the NASA Janus space mission – Detection of a spin-orbit interaction
Petr Pravec et al., ''7th IAA Planetary Defense Conference'', International Academy of Astronautics, 27 April 2021

Radar observations of (35107) 1991 VH
Jean-Luc Margot et al. ''Department of Earth and Space Sciences'', University of California, Los Angeles

1991 VH double period lightcurve
Petr Pravec, Astronomical Institute of Czech Academy of Sciences (Archived 6 December 1998)
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{{DEFAULTSORT:035107
Apollo asteroids
Discoveries by Robert H. McNaught
Potentially hazardous asteroids
Sk-type asteroids (SMASS)
Binary asteroids
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