4318 Baťa

From Wikipedia, the free encyclopedia
4318 Baťa
Discovery [1]
Discovered byZ. Vávrová
Discovery siteKleť Obs.
Discovery date21 February 1980
Designations
MPC designation
(4318) Baťa
Named after
Tomáš Baťa [1]
(Czech businessman)
1980 DE1 · 1977 TB3
1986 GJ
Minor planet category
main-belt [1] · (outer) [2][3]
background [4][5]
Orbital characteristics [2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc61.48 yr (22,457 d)
Aphelion3.5580 AU
Perihelion2.8881 AU
3.2231 AU
Eccentricity0.1039
5.79 yr (2,113 d)
313.92°
0° 10m 13.08s / day
Inclination9.5410°
33.144°
96.856°
Physical characteristics
Mean diameter
25.79±4.95 km[6][7]
27.47±8.03 km[8]
28.26±1.20 km[9]
Synodic rotation period
10.571±0.2523 h[10]
0.05[8]
0.051[9]
0.055[6][7]
D (SDSS-MOC)[11][12]
Absolute magnitude (H)
11.60[9]
11.70[2][6][7]
11.8[1]
11.98[8]

4318 Baťa, provisional designation 1980 DE1, is a dark background asteroid from the outermost regions of the asteroid belt, approximately 27 kilometers (17 miles) in diameter. It was discovered on 21 February 1980, by astronomer Zdeňka Vávrová at the Kleť Observatory in the Czech Republic.[1] The D-type asteroid has a rotation period of 10.6 hours and is likely elongated in shape.[3] It was named in memory of Czech businessman Tomáš Baťa.[1]

Orbit and classification[]

Baťa is a non-family asteroid from the main belt's background population.[4][5] It orbits the Sun in the outermost asteroid belt at a distance of 2.9–3.6 AU once every 5 years and 9 months (2,113 days; semi-major axis of 3.22 AU). Its orbit has an eccentricity of 0.10 and an inclination of 10° with respect to the ecliptic.[2] The body's observation arc begins with a precovery taken at Palomar Observatory in April 1957, almost 23 years prior to its official discovery observation at the Kleť Observatory.[1]

Naming[]

This minor planet was named in memory of Tomáš Baťa (1876–1932), a world-renowned Czech businessman and founder of the Bata Shoe Organization. The official naming citation was published by the Minor Planet Center on 8 June 1990 (M.P.C. 16444).[13]

Physical characteristics[]

In the SDSS-based taxonomy, Baťa is a very dark D-type asteroid.[11] This spectral type is typical in the outermost asteroid belt and often found in the Jupiter trojan population.

Rotation period[]

In April 2004, a rotational lightcurve of Baťa was obtained from photometric observations by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 10.571±0.2523 hours with a high brightness amplitude of 0.62 magnitude, indicative of an elongated, non-spherical shape (U=2).[10]

Diameter and albedo[]

According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Baťa measures between 25.79 and 28.26 kilometers in diameter and its surface has an albedo between 0.05 and 0.055.[6][7][8][9] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 21.09 kilometers based on an absolute magnitude of 12.11.[3]

References[]

  1. ^ a b c d e f g "4318 Bata (1980 DE1)". Minor Planet Center. Retrieved 27 November 2018.
  2. ^ a b c d "JPL Small-Body Database Browser: 4318 Bata (1980 DE1)" (2018-10-22 last obs.). Jet Propulsion Laboratory. Retrieved 27 November 2018.
  3. ^ a b c "LCDB Data for (4318) Baťa". Asteroid Lightcurve Database (LCDB). Retrieved 27 November 2018.
  4. ^ a b "Asteroid 4318 Bata". Small Bodies Data Ferret. Retrieved 27 November 2018.
  5. ^ a b "Asteroid (4318) Bata – Proper elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 27 November 2018.
  6. ^ a b c d Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R.; et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System: EAR-A-COMPIL-5-NEOWISEDIAM-V1.0. Bibcode:2016PDSS..247.....M. Retrieved 27 November 2018.
  7. ^ a b c d Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8.
  8. ^ a b c d Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv:1606.08923. Bibcode:2016AJ....152...63N. doi:10.3847/0004-6256/152/3/63.
  9. ^ a b c d 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)
  10. ^ a b 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.
  11. ^ a b Carvano, J. M.; Hasselmann, P. H.; Lazzaro, D.; Mothé-Diniz, T. (February 2010). "SDSS-based taxonomic classification and orbital distribution of main belt asteroids". Astronomy and Astrophysics. 510: 12. Bibcode:2010A&A...510A..43C. doi:10.1051/0004-6361/200913322. Retrieved 30 October 2019. (PDS data set)
  12. ^ 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.
  13. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 27 November 2018.

External links[]

Retrieved from ""