14627 Emilkowalski

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14627 Emilkowalski
Discovery [1]
Discovered by R. A. Kowalski
Discovery site Quail Hollow Obs.
Discovery date 7 November 1998
MPC designation 14627 Emilkowalski
Named after
Emil Kowalski
(discoverer's family)[2]
1998 VA
main-belt · (inner)[3]
Orbital characteristics[1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc 62.01 yr (22,648 days)
Aphelion 2.9885 AU
Perihelion 2.2138 AU
2.6011 AU
Eccentricity 0.1489
4.20 yr (1,532 days)
0° 14m 5.64s / day
Inclination 17.747°
Jupiter Tisserand parameter 3.3320
Physical characteristics
Dimensions 6.98±2.55 km[4]
7.105±0.106 km[5][6]
10.61 km (calculated)[3]
11.131 h[7]
0.057 (assumed)[3]
C[3] · DL [8]
13.1[5] · 13.38 (R)[7] · 13.6[1][3] · 13.7[4] · 14.19±0.75[8]

14627 Emilkowalski, provisional designation 1998 VA, is an asteroid from the inner regions of the asteroid belt, approximately 7 to 10 kilometers in diameter. It was discovered on 7 November 1998, by American astronomer Richard Kowalski at the U.S. Quail Hollow Observatory (761) in Zephyrhills, Florida.[9]

The asteroid orbits the Sun at a distance of 2.2–3.0 AU once every 4 years and 2 months (1,532 days). Its orbit has an eccentricity of 0.15 and an inclination of 18° with respect to the ecliptic.[1] Emilkowalski is the biggest member of a collisional group of asteroids, that resulted from the destruction of a larger parent body. The disruption happened approximately 220,000 years ago and it is one of the most recent asteroid breakups discovered in the main belt.[7][10] The first unused observation at Palomar Observatory (DSS) dates back to 1953. The first used precovery was taken at Siding Spring Observatory in 1975, extending the asteroid's observation arc by 23 years prior to its discovery.[9]

Between January and March 2012, photometric observations for this asteroid were made by a team led by Petr Pravec at Ondřejov Observatory, Czech Republic. The three obtained rotational light-curves gave an identical period of 11.131 hours with a brightness variation of 0.55, 0.64 and 0.65 in magnitude, respectively (U=3/2+/3-).[a] Previously, during the first quarter of 2008, a light-curve was obtained from observations at Simeiz Observatory and the Chuguev Observing Station (121) in Ukraine, as well as at Maidanak Observatory, Uzbekistan. It also gave a period of 11.131 hours with an amplitude of 0.85 in magnitude, which implies an elongated shape (U=n.a.).[7]

According to the surveys carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures 7.0 and 7.1 kilometers in diameter and its surface has an albedo of 0.12 and 0.20, respectively.[4][5] The Collaborative Asteroid Lightcurve Link (CALL), however, assumes an albedo for carbonaceous asteroids of 0.057 and hence calculates a larger diameter of 10.6 kilometers.[3] While CALL assigns a C-type for the asteroid's spectra, a study based on data from the Panoramic Survey Telescope and Rapid Response System, Pan-STARRS (PS1), assigns a DL-type.[3][8]

The minor planet is named after American Emil Kowalski (1918–1994) from Syosset, New York. She inspired the discoverer of space science when he was still a child.[2] Naming citation was published on 4 August 2001 (M.P.C. 43192).[11]


  1. ^ a b Pravec (2012) web: 3 rotational light-curves constructed in January, February and March 2012, rendered a rotation period 11.131±0.005 hours (sigma only for first lightcurve) with a brightness amplitude of 0.55, 0.64 and 0.66 in magnitude, respectively. Summary figures at Collaborative Asteroid Lightcurve Link (CALL) for (14627) Emilkowalski and at Ondrejov Asteroid Photometry Project
  1. ^ a b c d "JPL Small-Body Database Browser: 14627 Emilkowalski (1998 VA)" (2016-06-02 last obs.). Jet Propulsion Laboratory. Retrieved 3 December 2016. 
  2. ^ a b Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (14627) Emilkowalski. Springer Berlin Heidelberg. p. 815. ISBN 978-3-540-00238-3. Retrieved 6 April 2016. 
  3. ^ a b c d e f g "LCDB Data for (14627) Emilkowalski". Asteroid Lightcurve Database (LCDB). Retrieved 6 April 2016. 
  4. ^ 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:1209.5794Freely accessible. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 20 May 2016. 
  5. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 20 May 2016. 
  6. ^ a b Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096Freely accessible. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. Retrieved 3 December 2016. 
  7. ^ a b c d Krugly; et al. (May 2008). Photometry of asteroids: detection of the YORP effect (PDF). The Solar System Bodies: from Optics to Geology. Kharkiv, Ukraine: Astronomical Institute of Kharkiv. Retrieved 7 December 2008. 
  8. ^ 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:1506.00762Freely accessible. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 20 May 2016. 
  9. ^ a b "14627 Emilkowalski (1998 VA)". Minor Planet Center. Retrieved 6 April 2016. 
  10. ^ Nesvorný, D.; Vokrouhlický, D. (November 2006). "New Candidates for Recent Asteroid Breakups". The Astronomical Journal. 132 (5): 1950–1958. Bibcode:2006AJ....132.1950N. doi:10.1086/507989. Retrieved 6 April 2016. 
  11. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 20 May 2016. 

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