5026 Martes

5026 Martes (prov. designation: 1987 QL1) is a carbonaceous asteroid from the inner region of the asteroid belt, approximately 9 kilometers (6 miles) in diameter. It was discovered on 22 August 1987, by Czech astronomer Antonín Mrkos at Kleť Observatory in the Czech Republic.[10] It is named after the two weasel-like animal species: pine marten and beech marten.[2]

5026 Martes
005026-asteroid shape model (5026) Martes.png
Shape model of Martes from its lightcurve
Discovery [1]
Discovered byA. Mrkos
Discovery siteKleť Obs.
Discovery date22 August 1987
(5026) Martes
Named after
pine marten
beech marten
(Mustelidae mammals)[2]
1987 QL1 · 1965 QE
1976 QL · 1980 VA2
main-belt · (inner)[3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc63.37 yr (23,145 days)
Aphelion2.9540 AU
Perihelion1.8020 AU
2.3780 AU
3.67 yr (1,339 days)
0° 16m 7.68s / day
Physical characteristics
Mean diameter
4.93 km (calculated)[3]
8.967±2.335 km[4]
4.423±0.0011 h[5]
4.424087±0.000002 h[6]
4.4243±0.005 h[7]
0.20 (assumed)[3]
B–V = 0.863±0.042[8]
V–R = 0.440±0.047[8]
C[9] · S[3]
13.80[4] · 13.9[1][3] · 14.065±0.010 (R)[5] · 14.17±0.36[9]

Orbit and classificationEdit

Martes is the namesake member of a small asteroid family, named the Martes family.[citation needed] It orbits the Sun in the inner main-belt at a distance of 1.8–3.0 AU once every 3 years and 8 months (1,339 days). Its orbit has an eccentricity of 0.24 and an inclination of 4° with respect to the ecliptic.[1]

A first precovery was taken at Palomar Observatory in 1953, extending the body's observation arc by 34 years prior to its official discovery observation at Klet.[10]


This minor planet was named for the two species of the family Mustelidae, the pine marten and beech marten. They also live in the forests near the discovering Kleť Observatory.[2] The official naming citation was published by the Minor Planet Center on 22 June 1999 (M.P.C. 34920).[11]

Physical characteristicsEdit

Martes has been characterized as a carbonaceous C-type asteroid by PanSTARRS' photometric survey.[9]

Asteroid pairEdit

Martes forms an asteroid pair with 2005 WW113, and was part of the 35 sample asteroid pairs in Petr Pravec's study Formation of asteroid pairs by rotational fission, published in the journal Nature.[7]


Between 2008 and 2010, several rotational lightcurves of Martes were obtained from photometric observations. Lightcurve analysis gave a well-defined rotation period of 4.4243 hours with a brightness amplitude of 0.69 magnitude (U=3-/3/2+/3/2).[3][7][6][5]

Diameter and albedoEdit

According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Martes measures 8.967 kilometers in diameter and its surface has an albedo of 0.066, which is typical for carbonaceous asteroids.[4] The Collaborative Asteroid Lightcurve Link, however, assumes a standard albedo for stony asteroids of 0.20 and consequently calculates a much smaller diameter of 4.93 kilometers, due to the higher albedo.[3]


  1. ^ a b c d "JPL Small-Body Database Browser: 5026 Martes (1987 QL1)" (2016-08-27 last obs.). Jet Propulsion Laboratory. Retrieved 20 June 2017.
  2. ^ a b c Schmadel, Lutz D. (2007). "(5026) Martes". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 432. doi:10.1007/978-3-540-29925-7_4893. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f g "LCDB Data for (5026) Martes". Asteroid Lightcurve Database (LCDB). Retrieved 28 March 2017.
  4. ^ a b c d Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv:1509.02522. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. Retrieved 28 March 2017.
  5. ^ a b c Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 28 March 2017.
  6. ^ a b Polishook, D. (October 2014). "Spin axes and shape models of asteroid pairs: Fingerprints of YORP and a path to the density of rubble piles". Icarus. 241: 79–96. arXiv:1406.3359. Bibcode:2014Icar..241...79P. doi:10.1016/j.icarus.2014.06.018. Retrieved 28 March 2017.
  7. ^ a b c Pravec, P.; Vokrouhlický, D.; Polishook, D.; Scheeres, D. J.; Harris, A. W.; Galád, A.; et al. (August 2010). "Formation of asteroid pairs by rotational fission". Nature. 466 (7310): 1085–1088. arXiv:1009.2770. Bibcode:2010Natur.466.1085P. doi:10.1038/nature09315. PMID 20740010. Retrieved 28 March 2017.
  8. ^ a b Ye, Q.-z. (February 2011). "BVRI Photometry of 53 Unusual Asteroids". The Astronomical Journal. 141 (2): 8. arXiv:1011.0133. Bibcode:2011AJ....141...32Y. doi:10.1088/0004-6256/141/2/32. Retrieved 29 March 2017.
  9. ^ a b c 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. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 28 March 2017.
  10. ^ a b "5026 Martes (1987 QL1)". Minor Planet Center. Retrieved 28 March 2017.
  11. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 28 March 2017.

External linksEdit