958 Asplinda

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958 Asplinda
000958-asteroid shape model (958) Asplinda.png
Modelled shape of Asplinda from its lightcurve
Discovery  [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date28 September 1921
Designations
(958) Asplinda
Named after
 Bror A. Asplind
(Swedish astronomer) [2]
A921 SD ·1921 KC
main-belt   [1]  ·(outer) [3]
Hilda   [1] [4] [5]
Orbital characteristics   [3]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc 97.88 yr (35,751 d)
Aphelion 4.7204 AU
Perihelion 3.2494 AU
3.9849 AU
Eccentricity 0.1846
7.95 yr (2,905 d)
152.91°
0° 7m 26.04s / day
Inclination 5.6288°
343.12°
92.950°
Jupiter  MOID 0.7147 AU
TJupiter 3.0180
Physical characteristics
  • 45.112±0.405  km [6]
  • 47.08±6.2 km [7]
  • 48.57±1.51 km [8]
16.543±0.007  h [9] [lower-alpha 1]
  • (228.0°, 33.0°) (λ1/β1) [9]
  • (46.0°, 45.0°) (λ2/β2) [9]
  • 0.041±0.003 [8]
  • 0.0415±0.013 [7]
  • 0.045±0.008 [6]
10.4 [1] [3]

    958 Asplinda (prov. designation: A921 SDor1921 KC) is a resonant Hilda asteroid, approximately 47 kilometers (29 miles) in diameter, located in the outermost region of the asteroid belt. It was discovered on 28 September 1921, by astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. [1] The assumed C-type asteroid has a rotation period of 16.5 hours and is likely elongated in shape. It was named after Swedish astronomer Bror Asplind (1890–1954). [2]

    Contents

    Orbit and classification

    Asplinda is a member of the distant orbital Hilda group of asteroids, which stay in a 3:2  orbital resonance with Jupiter. [1] [4] [5] It is however not a member of the collisional Hilda family ( 001 ) but a non-family asteroid of the background population when applying the hierarchical clustering method to its proper orbital elements. [4] It orbits the Sun in the outermost asteroid belt at a distance of 3.2–4.7  AU once every 7 years and 11 months (2,905 days; semi-major axis of 3.98 AU). Its orbit has an eccentricity of 0.18 and an inclination of 6° with respect to the ecliptic. [3] The body's observation arc begins at Heidelberg on 24 October 1921, four weeks after its official discovery observation. [1]

    Naming

    This minor planet was named after Bror Ansgar Asplind (1890–1954), a Swedish astronomer and orbit computer. The following, sequentially numbered asteroids 959 Arne, 960 Birgit and 961 Gunnie are named after his three children, respectively. The naming was mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 92 ). [2]

    Physical characteristics

    No spectral type has been published for Asplinda. As an Hildian asteroid with a low albedo (see below) it is a carbonaceous C-type asteroid (assumed), [10] or possibly a D-type or P-type asteroid, which are very common among the Hildian and more distant Jupiter trojan population.

    Rotation period and poles

    3D-model of Asplinda based on its lightcurve 958Asplinda (Lightcurve Inversion).png
    3D-model of Asplinda based on its lightcurve

    In December 2017, a rotational lightcurve of Asplinda was obtained from photometric observations by Brian Warner, Robert Stephens and Daniel Coley at the Center for Solar System Studies ( U81 ) in California. Lightcurve analysis gave a rotation period of 16.543±0.007 hours with a high brightness amplitude of 0.64±0.02 magnitude, indicative of an elongated, non-spherical shape ( U=3− ). [9] [lower-alpha 1] The results supersedes previous observations with a period determination of 17.55±0.03 h by the same astronomers in 2016, and a period of 25.3 h published by Mats Dahlgren in 1998 ( U=2+/2 ). [10]

    The 2017 observations by Warner, Stephens and Coley also gave two spin axes of (228.0°, 33.0°) and (46.0°, 45.0°) in ecliptic coordinates (λ, β) and a sidereal period of 16.556100±0.000002 hours.

    These results supersede the asteroid's 2016 modeled spin axes and lightcurve with a sidereal period of 16.556100±0.000002 hours based on data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers led by Czech astronomers Josef Hanuš and Josef Ďurech, as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys ( 950 ). [10] [11]

    Diameter and albedo

    According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Asplinda measures 45.112±0.405, 47.08±6.2 and 48.57±1.51 kilometers in diameter, and its surface has an albedo of 0.045±0.008, 0.0415±0.013 and 0.041±0.003, respectively. [6] [8] [7]

    Another published measurement by the WISE team also gives a mean-diameters of 45.117±0.091 km with corresponding albedo of 0.045±0.005. [5] [10] The Collaborative Asteroid Lightcurve Link adopts the results from IRAS, that is, an albedo of 0.0415 and a diameter of 47.08 km based on an absolute magnitude of 10.71. [10] An asteroid occultation on 15 August 2006, gave a best-fit ellipse dimension of 47.0 × 47.0 kilometers. [5] These timed observations are taken when the asteroid passes in front of a distant star. However the quality of the measurement is poorly rated. [5]

    Notes

    1. 1 2 Lightcurve plot of (958) Asplinda by Brian D. Warner, Robert D. Stephens and Daniel R. Coley (2017). Rotation period 16.543±0.007 hours with a brightness amplitude of 0.64±0.02 mag. Quality code of 3–. Summary figures for at the LCDB and the CS3.

    Related Research Articles

    957 Camelia is a large, carbonaceous background asteroid and slow rotator, approximately 70 kilometers in diameter. It is located in the outer regions of the asteroid belt and was discovered on 7 September 1921, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in Germany and given the provisional designations A921 RF and 1921 JX. The C-type asteroid (Cb) has a long rotation period of at least 150 hours. It was named after the genus of flowering plants, Camellia.

    959 Arne is a background asteroid and slow rotator, approximately 52 kilometers in diameter, located in the outer region of the asteroid belt. It was discovered by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory on 30 September 1921. The X-type asteroid has an exceptionally long rotation period of 123.7 hours. It was named after Arne Asplind, son of Swedish astronomer Bror Asplind (1890–1954).

    1144 Oda, provisional designation 1930 BJ, is a dark Hildian asteroid from the outermost regions of the asteroid belt, approximately 57 kilometers in diameter. It was discovered on 28 January 1930, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory. The asteroid's name is a German female name, not related to the discoverer's contemporaries.

    1162 Larissa, provisional designation 1930 AC, is a metallic Hildian asteroid from the outermost regions of the asteroid belt, approximately 43 kilometers in diameter. It was discovered on 5 January 1930, by astronomer German astronomer Karl Reinmuth at Heidelberg Observatory in southwest Germany. The asteroid was named after the Greek city of Larissa.

    2797 Teucer is a large Jupiter trojan from the Greek camp, approximately 110 kilometers in diameter. It was discovered on 4 June 1981, by American astronomer Edward Bowell at the Anderson Mesa Station near Flagstaff, Arizona, in the United States. The dark D-type asteroid belongs to the 20 largest Jupiter trojans and has a rotation period of 10.15 hours. It was named after the Greek hero and great archer, Teucer.

    1268 Libya, provisional designation 1930 HJ, is a dark Hildian asteroid from the outer regions of the asteroid belt, approximately 95 kilometers in diameter. It was discovered on 29 April 1930, by South African astronomer Cyril Jackson at the Union Observatory in Johannesburg, South Africa. The asteroid was named for the country Libya.

    3254 Bus, provisional designation 1982 UM, is a rare-type Hildian asteroid from the outermost region of the asteroid belt, approximately 32 kilometers in diameter. It was discovered on 17 October 1982, by American astronomer Edward Bowell at Lowell's Anderson Mesa Station in Flagstaff, Arizona. It is named after astronomer Schelte J. Bus.

    4446 Carolyn, provisional designation 1985 TT, is a dark Hildian asteroid from the outermost regions of the asteroid belt, approximately 30 kilometers in diameter. It was discovered on 15 October 1985, by American astronomer Edward Bowell at the Anderson Mesa Station of the Lowell Observatory near Flagstaff, Arizona, in the United States. The asteroid was named after American astronomer Carolyn Shoemaker. It has a longer than average rotation period of 40.9 hours.

    2312 Duboshin, provisional designation 1976 GU2, is a dark Hildian asteroid from the outermost regions of the asteroid belt, approximately 54 kilometers (34 miles) in diameter. It was discovered on 1 April 1976, by Soviet–Russian astronomer Nikolai Chernykh at the Crimean Astrophysical Observatory in Nauchnij, on the Crimean peninsula. It was named after Russian astronomer Georgij Duboshin. The D-type asteroid has a longer than average rotation period of 50.78 hours.

    1212 Francette is a dark Hildian asteroid from the outermost regions of the asteroid belt, approximately 82 kilometers in diameter. It was discovered on 3 December 1931, by French astronomer Louis Boyer at the Algiers Observatory in Algeria, North Africa, who named it after his wife Francette Boyer.

    <span class="mw-page-title-main">2483 Guinevere</span> Hilda asteroid

    2483 Guinevere is a dark and elongated Hilda asteroid from the outermost regions of the asteroid belt, approximately 43 kilometers in diameter. The asteroid was discovered on 17 August 1928, by German astronomer Max Wolf at Heidelberg Observatory in southwest Germany and given the provisional designation 1928 QB. In the 1980s, it was named after King Arthur's wife Guinevere.

    <span class="mw-page-title-main">1256 Normannia</span> Hilda asteroid and slow rotator

    1256 Normannia is a dark Hilda asteroid and slow rotator from the outermost regions of the asteroid belt, approximately 69 kilometers in diameter. It was discovered on 8 August 1932, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in Germany. The asteroid was likely named after the Normans who gave their name to the region of Normandy in France.

    1529 Oterma, provisional designation 1938 BC, is a reddish, rare-type Hildian asteroid from the outermost region of the asteroid belt, approximately 56 kilometers in diameter. It was discovered on 26 January 1938, by Finnish astronomer Yrjö Väisälä at Turku Observatory in Southwest Finland. It is named for Liisi Oterma.

    <span class="mw-page-title-main">1512 Oulu</span> Hildian asteroid and slow rotator

    1512 Oulu, provisional designation 1939 FE, is a dark Hildian asteroid, slow rotator and possibly the largest known tumbler orbiting in the outermost region of the asteroid belt. With a diameter of approximately 80 kilometers, it belongs to the fifty largest asteroids in the outer main-belt. The body was discovered on 18 March 1939, by Finnish astronomer Heikki Alikoski at Turku Observatory in Southwest Finland and named for the Finnish town Oulu.

    1269 Rollandia, provisional designation 1930 SH, is a dark Hildian asteroid from the outermost region of the asteroid belt, approximately 105 kilometers (65 mi) in diameter. It was discovered on 20 September 1930, by Soviet astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The asteroid was named after French writer Romain Rolland. The D-type asteroid has a rotation period of 17.4 hours. It was one of the last 100-kilometer sized asteroids discovered in the main belt.

    2959 Scholl, provisional designation 1983 RE2, is a carbonaceous Hildian asteroid from the outer regions of the asteroid belt, approximately 34 kilometers in diameter. It was discovered on 4 September 1983 by English–American astronomer Edward Bowell of the Lowell Observatory at Anderson Mesa Station near Flagstaff, Arizona. The asteroid was named after German astronomer Hans Scholl.

    <span class="mw-page-title-main">1902 Shaposhnikov</span> Hilda asteroid

    1902 Shaposhnikov is a dark Hilda asteroid from the outermost region of the asteroid belt, approximately 92 kilometers in diameter. It was discovered on 18 April 1972, by Russian astronomer Tamara Smirnova at the Crimean Astrophysical Observatory in Nauchnyj, on the Crimean peninsula. The asteroid was named after Soviet astronomer and WWII casualty Vladimir Shaposhnikov. It was one of the last larger asteroids discovered in the main belt.

    <span class="mw-page-title-main">4230 van den Bergh</span> Hildian asteroid

    4230 van den Bergh (prov. designation: 1973 ST1) is a highly elongated Hildian asteroid and member of the Schubart family from the outer regions of the asteroid belt. It was discovered on 19 September 1973, by Dutch astronomer couple Ingrid and Cornelis van Houten at Leiden Observatory, on photographic plates taken by Dutch–American astronomer Tom Gehrels at the Palomar Observatory, California. The assumed carbonaceous C-type asteroid has a very long rotation period of 88 hours and measures approximately 37 kilometers (23 miles) in diameter. It was named for Dutch–Canadian astronomer Sidney Van den Bergh.

    1439 Vogtia, provisional designation 1937 TE, is a dark Hildian asteroid from the outermost region of the asteroid belt, approximately 48 kilometers in diameter. It was discovered on 11 October 1937, by German astronomer Karl Reinmuth at Heidelberg Observatory in southern Germany. It is named for astronomer Heinrich Vogt.

    (15502) 1999 NV27 (provisional designation 1999 NV27) is a Jupiter trojan from the Trojan camp, approximately 53 kilometers (33 miles) in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The dark Jovian asteroid has a rotation period of 15.1 hours and belongs to the 90 largest Jupiter trojans. It has not been named since its numbering in June 2000.

    References

    1. 1 2 3 4 5 6 7 "958 Asplinda (A921 SD)". Minor Planet Center. Retrieved 13 February 2020.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(958) Asplinda". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 84. doi:10.1007/978-3-540-29925-7_959. ISBN   978-3-540-00238-3.
    3. 1 2 3 4 5 "JPL Small-Body Database Browser: 958 Asplinda (A921 SD)" (2019-08-16 last obs.). Jet Propulsion Laboratory . Retrieved 13 February 2020.
    4. 1 2 3 "Asteroid 958 Asplinda – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 13 February 2020.
    5. 1 2 3 4 5 "Asteroid 958 Asplinda". Small Bodies Data Ferret. Retrieved 13 February 2020.
    6. 1 2 3 Grav, T.; Mainzer, A. K.; Bauer, J.; Masiero, J.; Spahr, T.; McMillan, R. S.; et al. (January 2012). "WISE/NEOWISE Observations of the Hilda Population: Preliminary Results". The Astrophysical Journal. 744 (2): 15. arXiv: 1110.0283 . Bibcode:2012ApJ...744..197G. doi:10.1088/0004-637X/744/2/197. S2CID   44000310.
    7. 1 2 3 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T . Retrieved 13 February 2020.
    8. 1 2 3 Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. (online, AcuA catalog p. 153)
    9. 1 2 3 4 Warner, Brian D.; Stephens, Robert D.; Coley, Daniel R. (April 2018). "Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 2017 October-December" (PDF). The Minor Planet Bulletin. 45 (2): 147–161. Bibcode:2018MPBu...45..147W. ISSN   1052-8091. Archived from the original (PDF) on 12 February 2020. Retrieved 13 February 2020.
    10. 1 2 3 4 5 6 "LCDB Data for (958) Asplinda". Asteroid Lightcurve Database (LCDB). Retrieved 13 February 2020.
    11. ↑ Hanuš, J.; Ďurech, J.; Brož, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution". Astronomy and Astrophysics. 551: A67. arXiv: 1301.6943 . Bibcode:2013A&A...551A..67H. doi:10.1051/0004-6361/201220701. ISSN   0004-6361. S2CID   118627434.
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