14627 Emilkowalski

14627 Emilkowalski
Discovery [1]
Discovered by R. A. Kowalski
Discovery site Quail Hollow Obs.
Discovery date 7 November 1998
Designations
MPC designation 14627 Emilkowalski
Named after
 Emil Kowalski
(discoverer's family)[2]
1998 VA
main-belt · (inner) [3]
Orbital characteristics [1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 0
Observation arc 61.80 yr (22,574 days)
Aphelion 2.9853 AU
Perihelion 2.2142 AU
2.5997 AU
Eccentricity 0.1483
4.19 yr (1,531 days)
10.639°
0° 14m 6.36s / day
Inclination 17.740°
41.468°
44.406°
Jupiter Tisserand parameter 3.333
Physical characteristics
Dimensions 6.98±2.55 km[4]
7.105±0.106 km[5]
10.61 km (calculated)[3]
11.131±0.005h[lower-alpha 1]
0.120±0.108[4]
0.2013±0.0170[5]
0.057 (assumed)[3]
C [3] · DL [6]
13.6[1][3]
13.7[4]
13.1[5]
14.19±0.75[6]
13.38 (R)[7]

    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.[8]

    The asteroid orbits the Sun at a distance of 2.2–3.0 AU once every 4 years and 2 months (1,531 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][9] Due to precoveries at Palomar Observatory (DSS) and Siding Spring Observatory from 1953 and 1975, the asteroid has an observation arc of 62 and 40 years, respectively.[1][8]

    In 2012, several photometric observations by a team lead by Petr Pravec at Ondřejov Observatory, Czech Republic, rendered a rotational light-curve with a period of 11.131±0.005 hours and a brightness amplitude of 0.55 in magnitude (U=3).[lower-alpha 1] Observations in 2008 also rendered a period of 11.131 hours with an amplitude of 0.85 mag, which implies an elongated shape.[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][6]

    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]

    References

    1. 1 2 Pravec (2012) web: 3 rotational light-curves constructed in Januaray, 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. 1 2 3 4 5 "JPL Small-Body Database Browser: 14627 Emilkowalski (1998 VA)" (2016-03-20 last obs.). Jet Propulsion Laboratory. Retrieved 9 April 2016.
    2. 1 2 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (14627) Emilkowalski. Springer Berlin Heidelberg. p. 815. ISBN 978-3-540-00238-3. Retrieved April 2016.
    3. 1 2 3 4 5 6 7 "LCDB Data for (14627) Emilkowalski". Asteroid Lightcurve Database (LCDB). Retrieved April 2016.
    4. 1 2 3 4 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. Retrieved April 2016.
    5. 1 2 3 4 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:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved April 2016.
    6. 1 2 3 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 April 2016.
    7. 1 2 3 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 December 7, 2008.
    8. 1 2 "14627 Emilkowalski (1998 VA)". Minor Planet Center. Retrieved April 2016.
    9. ↑ 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 April 2016.

    External links


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