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
Mean diameter
  • 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.

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    References

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    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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