(9992) 1997 TG19

(9992) 1997 TG19
Discovery [1]
Discovered by T. Kagawa
T. Urata
Discovery site Gekko Obs.
Discovery date 8 October 1997
Designations
MPC designation (9992) 1997 TG19
1997 TG19 · 1974 HC1
1980 BD
Mars-crosser [1][2]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 42.77 yr (15,622 days)
Aphelion 2.8054 AU
Perihelion 1.5370 AU
2.1712 AU
Eccentricity 0.2921
3.20 yr (1,169 days)
154.42°
0° 18m 29.16s / day
Inclination 2.5944°
42.994°
234.83°
Physical characteristics
Dimensions 3.07 km (derived)[2]
4.75±0.36 km[3]
5.7300±0.0016 h[4]
5.7402±0.0005 h[5]
5.7408±0.0009 h[lower-alpha 1]
0.137±0.022[3]
0.20 (assumed)[2]
S [2]
14.40[3] · 14.48±0.08 (R)[lower-alpha 1] · 14.5[1] · 14.663±0.004 (R)[4] · 14.76±0.26[6] · 14.97±0.094[2][7]

    (9992) 1997 TG19 is a stony asteroid and eccentric Mars-crosser, approximately 4 kilometers in diameter. It was discovered on 8 October 1997, by Japanese astronomers Tetsuo Kagawa and Takeshi Urata at Gekko Observatory near Shizuoka, Japan.[8]

    Orbit and classification

    Orbit of (9992) 1997 TG19 (blue), compared to the inner planets and Jupiter (outermost)

    The stony S-type asteroid orbits the Sun at a distance of 1.5–2.8 AU once every 3 years and 2 months (1,169 days). Its orbit has an eccentricity of 0.29 and an inclination of 3° with respect to the ecliptic.[1] The first used observation was made at the Cerro El Roble Station in 1974, extending the asteroid's observation arc by 23 prior to its discovery.[8]

    Physical characteristics

    Lightcurves

    Between 2006 and 2013, three rotational lightcurves for this asteroid were obtained from photometric observations made at the Hunters Hill Observatory, Australia, the Ondřejov Observatory, Czech Republic, and the U.S. Palomar Transient Factory, California. They gave a well-defined, concurring rotation period of 5.7402±0.0005 hours (best result) with a brightness amplitude of 0.42, 0.40 and 0.27 in magnitude, respectively (U=3/3/2).[lower-alpha 1][4][5]

    Diameter and albedo

    According to the survey carried out by the Japanese Akari satellite, the asteroid's surface has an albedo of 0.13 and a diameter of 4.75 kilometers.[3] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 3.1 kilometers, as the higher the body's albedo (reflectivity), the shorter its diameter, at a constant absolute magnitude (brightness).[2]

    Numbering and naming

    This minor planet was numbered by the Minor Planet Center on 2 February 1999.[9] As of 2018, it has not been named.[8]

    Notes

    1. 1 2 3 Pravec (2006) web: rotation period 5.7408±0.0009 hours with a brightness amplitude of 0.0009 mag. Summary figures at Collaborative Asteroid Lightcurve Link (CALL) for (9992) and Pravec − Results from Asteroid Photometry Project at Ondřejov Observatory

    References

    1. 1 2 3 4 5 "JPL Small-Body Database Browser: 9992 (1997 TG19)" (2017-01-28 last obs.). Jet Propulsion Laboratory. Retrieved 26 May 2017.
    2. 1 2 3 4 5 6 "LCDB Data for (9992)". Asteroid Lightcurve Database (LCDB). Retrieved 4 July 2016.
    3. 1 2 3 4 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. Retrieved 4 July 2016.
    4. 1 2 3 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 4 July 2016.
    5. 1 2 Higgins, David; Pravec, Petr; Kusnirak, Peter; Galad, Adrian; Kornos, Leos; Pray, Donald; et al. (December 2006). "Asteriod lightcurve analysis at Hunters Hill Observatory and collaborating stations - autumn 2006". The Minor Planet Bulletin. 33 (4): 89–91. Bibcode:2006MPBu...33...89H. ISSN 1052-8091. Retrieved 4 July 2016.
    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. Retrieved 4 July 2016.
    7. ↑ Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012). "Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations". Icarus. 221 (1): 365–387. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026. Retrieved 4 July 2016.
    8. 1 2 3 "9992 (1997 TG19)". Minor Planet Center. Retrieved 4 July 2016.
    9. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.
    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.