981 Martina

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981 Martina (prov. designation: Template:Mp or [[Provisional designation in astronomy#Temporary minor planet designations|Template:Mp]]) is a carbonaceous Themistian asteroid from the outer regions of the asteroid belt, approximately Script error: No such module "convert". in diameter. It was discovered on 23 September 1917, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula.[1] The C/B-type asteroid has a rotation period of 11.3 hours.[2] It was named after French historian and revolutionary Henri Martin (1810–1883).[3]

Orbit and classification

Martina is a core member of the Themis family (602Script error: No such module "Check for unknown parameters".), a very large family of carbonaceous asteroids, named after 24 Themis.[4][5][6]Template:Rp It orbits the Sun in the outer asteroid belt at a distance of 2.5–3.7 AU once every 5 years and 5 months (1,992 days; semi-major axis of 3.1 AU). Its orbit has an eccentricity of 0.20 and an inclination of 2° with respect to the ecliptic.[7] The body's observation arc begins with its first observation as Template:Mp (Template:Mp) at Lowell Observatory in August 1906, more than 11 years prior to its official discovery observation at Crimea–Simeis.[1]

Naming

This minor planet was named after French historian and revolutionary politician, Henri Martin (1810–1883). The Template:MoMP was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 94Script error: No such module "Check for unknown parameters".).[3]

Physical characteristics

In the SDSS-based taxonomy, Martina is a carbonaceous C-type asteroid,[8] while in the classical Tholen classification, it has been classified as a CFU: asteroid, closest to a C-type and somewhat similar to an F-type, though with an unusual (U) and noisy spectra (:).[7] In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Martina is a B-type asteroid, a "brighter" variant of the more common C-type.[5][9] Members of the Themis family are typically classified as C-types with an albedo of 0.07, a value notably lower than for this asteroid at 0.10–0.13 (see below).[6]Template:Rp

Rotation period

In August 2004, a rotational lightcurve of Martina was obtained from photometric observations by David Higgins at the Hunters Hill Observatory Template:Obscode in Australia. Lightcurve analysis gave a rotation period of Script error: No such module "val". hours with a brightness variation of Script error: No such module "val". magnitude (U=2Script error: No such module "Check for unknown parameters".).[10][2] Astronomers at the Palomar Transient Factory in California also determined the period in the R-band on two occasions, measuring 11.263 and 11.268 hours with an amplitude of 0.24 and 0.15 in 2010 and 2012, respectively (U=2/2Script error: No such module "Check for unknown parameters".).[10][11]

Diameter and albedo

According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Franklina measures between 28.8 and 32.5 kilometers in diameter and its surface has an albedo between 0.10 and 0.13.[12][13][14][15] The Collaborative Asteroid Lightcurve Link adopts the results from IRAS, that is, an albedo of 0.1254 and a diameter of 28.87 kilometers, based on an absolute magnitude of 10.9.[10]

References

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External links

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