(39546) 1992 DT5

(39546) 1992 DT5
Discovery[1]
Discovered byUESAC
Discovery siteLa Silla Obs.
Discovery date29 February 1992
Designations
(39546) 1992 DT5
1992 DT5 · 1999 TA162
main-belt[1][2] · (middle)[3]
Hoffmeister[4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc25.68 yr (9,378 d)
Aphelion2.8587 AU
Perihelion2.7254 AU
2.7921 AU
Eccentricity0.0239
4.67 yr (1,704 d)
276.01°
0° 12m 40.68s / day
Inclination5.2622°
150.60°
304.53°
Physical characteristics
5.34 km (calculated)[3]
1167±100 h[5]
0.057 (assumed)[3]
C (assumed)[3]
14.641±0.007 (R)[5]
14.7[2]
14.88±0.30[6]
15.09[3]

(39546) 1992 DT5 is a dark Hoffmeister asteroid and exceptionally slow rotator from the central region of the asteroid belt, approximately 5.3 kilometers (3.3 miles) in diameter. The likely elongated C-type asteroid was discovered on 29 February 1992, by the Uppsala–ESO Survey of Asteroids and Comets at ESO's La Silla astronomical observatory site in northern Chile.[1]

Orbit and classification

1992 DT5 is an attributed member of the very compact Hoffmeister family (519), which, based upon its low albedo, was most likely formed from the breakup of a 50–100 kilometer-sized, carbon-rich parent body within the past several hundred million years.[7][8] The family consist of nearly 2000 known members and its namesake is the asteroid 1726 Hoffmeister.[9]

It orbits the Sun in the central main-belt at a distance of 2.7–2.9 AU once every 4 years and 8 months (1,704 days; semi-major axis of 2.79 AU). Its orbit has an eccentricity of 0.02 and an inclination of 5° with respect to the ecliptic.[2] The body's observation arc begins with its discovery observation at La Silla in February 1992.[1]

Physical characteristics

1992 DT5 is an assumed carbonaceous C-type asteroid.[3] The overall spectral type of the Hoffmeister family is that of a C- and F-type.[9]: 23 

Rotation period

In September 2013, a rotational lightcurve for this asteroid was obtained from photometric observations in the R-band at the Palomar Transient Factory in California. It gave an exceptionally long rotation period of 1167 hours with an estimated error margin of ±100 hours. According to the Light Curve Data Base (LCDB),[3] it is the 8th slowest rotating minor planet known to exist. Due to its high brightness amplitude of 0.80 magnitude, the body has a likely elongated shape (U=2).[5]

Diameter and albedo

The Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous asteroids of 0.057 and calculates a diameter of 5.3 kilometers based on an absolute magnitude of 15.09.[3]

Numbering and naming

This minor planet was numbered by the Minor Planet Center on 26 May 2002 (M.P.C. 45660).[10] As of 2018, it has not been named.[1]

References

  1. ^ a b c d e "39546 (1992 DT5)". Minor Planet Center. Retrieved 11 April 2018.
  2. ^ a b c d "JPL Small-Body Database Browser: 39546 (1992 DT5)" (2016-07-25 last obs.). Jet Propulsion Laboratory. Retrieved 11 April 2018.
  3. ^ a b c d e f g h "LCDB Data for (39546)". Asteroid Lightcurve Database (LCDB). Retrieved 11 April 2018.
  4. ^ "Asteroid (39546) 1992 DT5 – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 27 October 2019.
  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. S2CID 8342929.
  6. ^ 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. S2CID 53493339.
  7. ^ Migliorini, F.; Manara, A.; di Martino, M.; Farinella, P. (June 1996). "The Hoffmeister asteroid family: inferences from physical data". Astronomy and Astrophysics. 310: 681. Bibcode:1996A&A...310..681M.
  8. ^ Carruba, V.; Novakovic, B.; Aljbaae, S. (March 2017). "The Hoffmeister asteroid family". Monthly Notices of the Royal Astronomical Society. 465 (4): 4099–4105. arXiv:1611.06176. Bibcode:2017MNRAS.465.4099C. doi:10.1093/mnras/stw3022.
  9. ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. S2CID 119280014.
  10. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.