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(35107) 1991 VH

Binary near-Earth asteroid


Binary near-Earth asteroid

FieldValue
minorplanetyes
name(35107) 1991 VH
background#FFC2E0
image1991VH Arecibo radar Aug9.png
captionRadar images of and its satellite by Arecibo Observatory in 2008
discovery_ref
discovererR. H. McNaught
discovery_siteSiding Spring Obs.
discovered9 November 1991
mpc_name1991 VH
mp_categoryNEOApolloPHA
orbit_ref
epoch21 January 2022 (JD 2459600.5)
uncertainty0
observation_arc29.34 yr (10,717 days)
aphelion1.3014 AU
perihelion0.9732 AU
semimajor1.1373 AU
eccentricity0.1443
period1.21 yr (443.02 days)
mean_anomaly7.959°
mean_motion/ day
inclination13.912°
asc_node139.349°
arg_peri206.940°
moid0.02467 AU
satellites1
physical_ref
dimensionskm
mean_diameter(primary)
mass(system)
(primary)
density
rotation
albedo0.17–0.18
spectral_typeSk (SMASS)
V–R=
R–I=
abs_magnitude(H-G)
16.76 (assumed)

(primary) V–R= R–I= 16.76 (assumed)

**** (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 1991 VH experienced 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 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU 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 100 m-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 1.30 x, or a volume-equivalent diameter of 1.18 km. 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

M. Wolf L. Šarounová [spurious designation at JPL] () (wrt ecliptic)

**** 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

Main article: Janus (spacecraft)

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.

Notes

References

References

  1. (2024-08-01). "An Earth Encounter as the Cause of Chaotic Dynamics in Binary Asteroid (35107) 1991VH". The Planetary Science Journal.
  2. Foust, Jeff. (9 June 2022). "Psyche launch delay forcing revamp of rideshare mission".
  3. (December 31, 2022). "Evidence of surface heterogeneity on active asteroid (3200) Phaethon". Icarus.
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