731 Sorga

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731 Sorga (prov. designation: Template:Mp or Template:Mp) is a highly elongated background asteroid from the outer regions of the asteroid belt, approximately Template:Convert in diameter. It was discovered on 15 April 1912, by German astronomer Adam Massinger at the Heidelberg-Königstuhl State Observatory in southwest Germany.[1] The C-type (CD) and X-type asteroid (Xe) has a rotation period of 8.2 hours. It was named Sorga, meaning "the heavens" in the Indonesian language.[2]

Orbit and classification

Sorga is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements.[3][4][5] It orbits the Sun in the outer asteroid belt at a distance of 2.6–3.4 AU once every 5 years and 2 months (1,886 days; semi-major axis of 2.99 AU). Its orbit has an eccentricity of 0.14 and an inclination of 11° with respect to the ecliptic.[6] The body's observation arc begins at Heidelberg Observatory on 21 October 1919, more than seven years after its official discovery observation.[1]

Naming

This minor planet was named Sorga, the word for "the heavens" in the Indonesian language, also transliterated as "surga". The Template:MoMP was not mentioned in The Names of the Minor Planets by Paul Herget.[2]

Physical characteristics

In the Tholen classification, Sorga is closest to a common, carbonaceous C-type asteroid and somewhat similar to a dark D-type asteroid (CD), while in the Bus–Binzel SMASS classification, it is an Xe-subtype which transitions from the X-type to the bright E-type.[6][4] Sorga has also been classified as a metallic M-type asteroid.[7]

Rotation period and poles

File:731Sorga (Lightcurve Inversion).png
Lightcurve-based 3D shape model of Sorga

In April 2005, a rotational lightcurve of Sorga was obtained from photometric observations by Brian Warner at his Palmer Divide Observatory Template:Obscode in Colorado. Analysis gave a classically shaped bimodal lightcurve with a well-defined rotation period of (Template:Val) hours and a high brightness variation of (Template:Val) magnitude, indicative of its elongated shape (U=3Script error: No such module "Check for unknown parameters".).[8] In February 2009, Warner revisited Sorga and determined a very similar period of (Template:Val) hours though with a much lower amplitude of (Template:Val) magnitude (U=3Script error: No such module "Check for unknown parameters".).[9]Template:Efn

In January 2010, astronomers at the Palomar Transient Factory measured a period of Template:Val hours with an amplitude of Template:Val magnitude (U=2Script error: No such module "Check for unknown parameters".).[7][10] Additional observations by Christophe Demeautis in September 2017, and by Bruno Christmann in April 2020, gave a period of (Template:Val) and (Template:Val) hours with an amplitude of Template:Val and Template:Val magnitude, respectively (U=3–/3Script error: No such module "Check for unknown parameters".).[11]

In 2016, a modeled lightcurve rendered a concurring sidereal period of Template:Val hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers, as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys Template:Obscode. The study also determined two spin axes of (83.0°, 40.0°) and (275.0°, 21.0°) in ecliptic coordinates (λ, β).[12]

Diameter and albedo

According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Japanese Akari satellite, and the Infrared Astronomical Satellite IRAS, Sorga measures (Template:Val), (Template:Val) and (Template:Val) kilometers in diameter and its surface has an albedo of (Template:Val), (Template:Val) and (Template:Val), respectively.[13][14][15][16] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1339 and a diameter of 41.70 kilometers based on an absolute magnitude of 9.7.[7] The WISE team also published an alternative mean-diameter of (Template:Val) with an albedo of (Template:Val).[7]

Two asteroid occultations on 24 October 2007, and on 31 October 2012, gave a best-fit ellipse dimension of (Template:Val) and (Template:Val), with an intermediate and low quality rating of 2 and 1, respectively.[4] These timed observations are taken when the asteroid passes in front of a distant star.[4]

Notes

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References

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External links

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  1. ↑ a b Cite error: Invalid <ref> tag; no text was provided for refs named MPC-object
  2. ↑ a b Cite error: Invalid <ref> tag; no text was provided for refs named springer
  3. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named AstDys-object
  4. ↑ a b c d Cite error: Invalid <ref> tag; no text was provided for refs named Ferret
  5. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Zappala-family
  6. ↑ a b Cite error: Invalid <ref> tag; no text was provided for refs named jpldata
  7. ↑ a b c d Cite error: Invalid <ref> tag; no text was provided for refs named lcdb
  8. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Warner-2005g
  9. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Warner-2009k
  10. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Waszczak-2015
  11. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named geneva-obs
  12. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Hanus-2013a
  13. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Mainzer-2016
  14. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Masiero-2014
  15. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named AKARI
  16. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named SIMPS
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