849 Ara

849 Ara ("prov. designation": "or" ) is a large, metallic background asteroid, approximately in diameter, that is located in the outer region of the asteroid belt. It was discovered on 9 February 1912, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The M-type asteroid has a short rotation period of 4.1 hours and is likely elongated in shape. It was named after the American Relief Administration (ARA) for the help given during the Russian famine of 1921–22.
Orbit and classification.
"Ara" is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.5–3.8 AU once every 5 years and 7 months (2,038 days; semi-major axis of 3.15 AU). Its orbit has an eccentricity of 0.20 and an inclination of 20° with respect to the ecliptic. In addition, "Ara" has a low Jupiter tisserand of 3.09, just above the defined threshold of 3.0 which is used to distinguish asteroids from the Jupiter-family comets. The body's observation arc begins at the Collegio Romano Observatory in Italy on 3 July 1919, more than 6 years after its official discovery observation at Simeiz.
Naming.
This minor planet was named after American Relief Administration (ARA), in appreciation of the help it gave during the Russian famine of 1921–22. Headed by Herbert Hoover, ARA was a relief mission after World War I to Europe which also included post-revolutionary Russia later on. The was mentioned in "The Names of the Minor Planets" by Paul Herget in 1955 ().
Physical characteristics.
In the Tholen classification as well as in the lesser known taxonomic method by Howell, "Ara" is a metallic M-type asteroid. This spectral type translates into the X-type in more modern asteroid taxonomic systems. In 2018 and 2019, a study using photometry from the Korea Microlensing Telescope Network and the South African Astronomical Observatory, grouped "Ara" into the X-type category based on the Bus–DeMeo classification.
Rotation period and pole.
In June 1981, a rotational lightcurve of "Ara" was obtained from photometric observations by Alan Harris. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude, indicative of an elongated shape (). Numerous observations have since confirmed this period. This includes Laurent Bernasconi (2004) and (2006), Davide Gandolfi (2006), Adam Marciniak (2009), Maurice Audejean (2010), and Richard E. Schmidt (2017). In 2017, a modeled lightcurve gave a concurring sidereal period of hours as well as a spin axis of (223.0°, −41.0°) in ecliptic coordinates (λ, β).
Diameter and albedo.
According to the surveys carried out by the Japanese Akari satellite, the Infrared Astronomical Satellite IRAS, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), "Ara" measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. Alternative mean-diameters published by the WISE team include () and () with corresponding albedos of () and ().
In 2009 and 2015, several asteroid occultations of "Ara" were observed. The two best-rated observations from January 2009 and April 2015 and August 2008, gave a best-fit ellipse dimension of () and (), respectively. These timed observations are taken when the asteroid passes in front of a distant star. The "Collaborative Asteroid Lightcurve Link" adopts Petr Pravec's revised WISE albedo of 0.1149 and takes a diameter of 84.61 kilometers based on an absolute magnitude of 8.33, while Josef Ďurech calculates a diameter of by combining lightcurve inversion models with asteroid occultation silhouettes.