Astronomy:1011 Laodamia

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1011 Laodamia
Discovery[1]
Discovered byK. Reinmuth
Discovery siteHeidelberg Obs.
Discovery date5 January 1924
Designations
(1011) Laodamia
Pronunciation/ˌleɪ.oʊdəˈmaɪə/
Named afterΛαοδάμεια Lāodamīa
(Greek mythology)[2]
1924 PK · 1939 FG
1958 OC
Minor planet categoryMars crosser[1][3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc93.50 yr (34,150 days)
|{{{apsis}}}|helion}}3.2315 AU
|{{{apsis}}}|helion}}1.5535 AU
2.3925 AU
Eccentricity0.3507
Orbital period3.70 yr (1,352 days)
Mean anomaly88.023°
Mean motion0° 15m 58.68s / day
Inclination5.4939°
Longitude of ascending node132.53°
353.34°
Physical characteristics
Dimensions7.39 km (derived)[4]
7.56±0.76 km[5]
Rotation period5.17 h[6]
5.17247±0.00007 h[7]
5.175±0.005 h[lower-alpha 1]
Geometric albedo0.248±0.050[5]
0.259[8]
Tholen = S[1] · S[4][9]
SMASS = Sr[1]
B–V = 0.900[1]
U–B = 0.515[1]
V–R = 0.324±0.171[10]
Absolute magnitude (H)12.00[9] · 12.416±0.171[10] · 12.74[1][4][5] · 13.09±0.23[11]


Laodamia (minor planet designation: 1011 Laodamia), provisional designation 1924 PK, is a stony asteroid and sizable Mars-crosser near the innermost regions of the asteroid belt, approximately 7.5 kilometers in diameter. It was discovered on 5 January 1924, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany.[3] The asteroid was named after Laodamia from Greek mythology.[2]

Orbit and classification

Laodamia is a Mars-crossing asteroid, a dynamically unstable group between the main belt and the near-Earth populations, crossing the orbit of Mars at 1.666 AU. It orbits the Sun at a distance of 1.6–3.2 AU once every 3 years and 8 months (1,352 days). Its orbit has an eccentricity of 0.35 and an inclination of 5° with respect to the ecliptic.[1]

The body's observation arc begins 15 years after its official discovery observation with its identification 1939 FG at Turku Observatory in March 1939.[3] On 5 September 2083, it will pass 0.06186 AU (9,254,000 km; 5,750,000 mi) from Mars.[1]

Physical characteristics

In the Tholen classification, Laodamia is a stony S-type asteroid, while in the SMASS taxonomy, it is a transitional type between the stony S-type and rare R-type asteroids.[1]

Rotation period and spin axis

In March 2002, a rotational lightcurve of Laodamia was obtained from photometric observations by French amateur astronomers Laurent Bernasconi and Silvano Casulli. Lightcurve analysis gave a well-defined rotation period of 5.17247 hours with a brightness amplitude of 0.44 magnitude ({{{1}}}).[7] Two other lightcurve gave a concurring period of 5.17 and 5.175 hours, respectively ({{{1}}}).[6][lower-alpha 1]

Photometry taken at the Rozhen Observatory over a period of more than a decade allowed to model the asteroid's shape and gave two spin axis of (95.0°, −85.5°) and (272.0°, −88.0°) in ecliptic coordinates (λ, β) ({{{1}}}).[10]

Diameter and albedo

According to the survey carried out by NASA's Wide-field Infrared Survey Explorer and its subsequent NEOWISE mission, Laodamia measures 7.56 kilometers in diameter and its surface has an albedo of 0.248,[5] while the Collaborative Asteroid Lightcurve Link adopts an albedo of 0.259 and derives a diameter of 7.39 kilometers based on an absolute magnitude of 12.74.[4]

This makes Laodamia one of the largest mid-sized Mars-crossing asteroids comparable with 1065 Amundsenia (9.75 km), 1139 Atami (9.35 km), 1474 Beira (14.9 km), 1727 Mette (5.44 km), 1131 Porzia (7.13 km), 1235 Schorria (5.55 km), 985 Rosina (8.18 km), 1310 Villigera (15.24 km) and 1468 Zomba (7 km), but far smaller than the largest members of this dynamical group, namely, 132 Aethra, 323 Brucia, 1508 Kemi, 2204 Lyyli and 512 Taurinensis, which are all larger than 20 kilometers in diameter.

Naming

This minor planet was named after Laodamia from Greek mythology.[2] The asteroid's name was proposed by Russian astronomer Nikolaj Vasil'evich Komendantov (RI 740), see (3958).[2]

The name either refers to the daughter of Akastos, who was the wife of Protesilaos, see (3540), and killed in the Trojan War, as narrated by Euripides, see (2930). It may also refer to the daughter of Bellerophon, see (1808) and the wife of Sarpedon, see (2223). She was killed by the arrows of Artemis, see (105). (Source of name researched by the author of the Dictionary of Minor Planet Names, Lutz D. Schmadel).[2]

Notes

  1. ↑ 1.0 1.1 Apostolovska (2011): rotation period 5.175 hours with a brightness amplitude of 0.41 mag and a Quality Code of 2+. Summary figures for (1011) Laodamia at Collaborative Asteroid Lightcurve Link (CALL)

References

  1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 "JPL Small-Body Database Browser: 1011 Laodamia (1924 PK)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2001011. Retrieved 4 September 2017. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Schmadel, Lutz D. (2007). "(1011) Laodamia". Dictionary of Minor Planet Names – (1011) Laodamia. Springer Berlin Heidelberg. p. 87. doi:10.1007/978-3-540-29925-7_1012. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 3.2 "1011 Laodamia (1924 PK)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=1011. Retrieved 4 September 2017. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 "LCDB Data for (1011) Laodamia". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=1011%7CLaodamia. Retrieved 4 September 2017. 
  5. ↑ 5.0 5.1 5.2 5.3 Alí-Lagoa, V.; Delbo', M. (July 2017). "Sizes and albedos of Mars-crossing asteroids from WISE/NEOWISE data". Astronomy and Astrophysics 603: 8. doi:10.1051/0004-6361/201629917. Bibcode: 2017A&A...603A..55A. https://www.aanda.org/articles/aa/pdf/2017/07/aa29917-16.pdf. Retrieved 20 October 2017. 
  6. ↑ 6.0 6.1 Ivanova, V. G.; Apostolovska, G.; Borisov, G. B.; Bilkina, B. I. (November 2002). "Results from photometric studies of asteroids at Rozhen National Observatory, Bulgaria". In: Proceedings of Asteroids 500: 505–508. Bibcode: 2002ESASP.500..505I. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2002ESASP.500..505I. Retrieved 4 September 2017. 
  7. ↑ 7.0 7.1 Behrend, Raoul. "Asteroids and comets rotation curves – (1011) Laodamia". Geneva Observatory. http://obswww.unige.ch/~behrend/page3cou.html#001011. Retrieved 4 September 2017. 
  8. ↑ Morrison, D.; Zellner, B. (December 1978). "Polarimetry and radiometry of the asteroids". In: Asteroids. (A80-24551 08-91) Tucson: 1090–1097. Bibcode: 1979aste.book.1090M. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1979aste.book.1090M. Retrieved 4 September 2017. 
  9. ↑ 9.0 9.1 Carry, B.; Solano, E.; Eggl, S.; DeMeo, F. E. (April 2016). "Spectral properties of near-Earth and Mars-crossing asteroids using Sloan photometry". Icarus 268: 340–354. doi:10.1016/j.icarus.2015.12.047. Bibcode: 2016Icar..268..340C. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2016Icar..268..340C. Retrieved 4 September 2017. 
  10. ↑ 10.0 10.1 10.2 Apostolovska, G.; Donchev, Z.; Kostov, A.; Ivanova, V.; Borisov, G.; Bilkina, B. (December 2014). "Photometry and Shape Modeling of Mars Crosser Asteroid (1011) Laodamia". Serbian Astronomical Journal 189 (189): 79–85(SerAJHomepage). doi:10.2298/SAJ1489079A. Bibcode: 2014SerAJ.189...79A. 
  11. ↑ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus 261: 34–47. doi:10.1016/j.icarus.2015.08.007. Bibcode: 2015Icar..261...34V. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015Icar..261...34V. Retrieved 4 September 2017. 

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