9971 Ishihara

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9971 Ishihara
009971-asteroid shape model (9971) Ishihara.png
Shape model of Ishihara from its lightcurve
Discovery  [1]
Discovered by K. Endate
K. Watanabe
Discovery site Kitami Observatory
Discovery date16 April 1993
Designations
(9971) Ishihara
Named after
Takahiro Ishihara
(Japanese astronomer) [2]
1993 HS ·1991 YC2
1996 EU1
main-belt   [1] [3]  · Flora   [4]
Orbital characteristics   [3]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 24.91 yr (9,097 days)
Aphelion 2.4465 AU
Perihelion 1.9164 AU
2.1814 AU
Eccentricity 0.1215
3.22 yr (1,177 days)
158.69°
0° 18m 21.24s / day
Inclination 2.7482°
20.550°
246.01°
Physical characteristics
Dimensions4.986±0.053  km [5]
5.012±0.069 km [6]
6.715±0.0036  h [7]
6.71574±0.00001 h [8]
(42.0°, 76.0°) (λ1/β1) [8]
0.2328±0.0281 [6]
0.235±0.027 [5]
S (assumed) [4]
13.7 [6]  ·13.9 [3]  ·13.852±0.006(R) [7]  ·14.3 [4]

    9971 Ishihara (prov. designation: 1993 HS) is a stony Flora asteroid from the inner regions of the asteroid belt, approximately 5 kilometers (3.1 miles) in diameter. It was discovered by Japanese amateur astronomers Kin Endate and Kazuro Watanabe at Kitami Observatory on 16 April 1993, [1] and named after Takahiro Ishihara, president of the astronomical society at Hiroshima. [2]

    Contents

    Orbit and classification

    Orbit of Ishihara (blue), inner planets and Jupiter (outermost) AnimatedOrbitOf9971Ishihara.gif
    Orbit of Ishihara (blue), inner planets and Jupiter (outermost)

    Ishihara is a member of the Flora family, one of the largest families of stony asteroids in the asteroid belt. It orbits the Sun in the inner main-belt at a distance of 1.9–2.4  AU once every 3 years and 3 months (1,177 days). Its orbit has an eccentricity of 0.12 and an inclination of 3° with respect to the ecliptic. [3] It was first identified as 1991 YC2 at Karl Schwarzschild Observatory in 1991, extending the body's observation arc by approximately 2 years prior to its official discovery at Kitami. [1]

    Naming

    This minor planet was named after Takahiro Ishihara (born 1961), an observer of comets, communicator of astronomy, and former president of the astronomical society at Hiroshima (1987–1997). [2] The official naming citation was published by the Minor Planet Center on 6 January 2003 ( M.P.C. 47298). [9]

    Physical characteristics

    Rotation and poles

    In January 2012, a rotational lightcurve of Ishihara was obtained from photometric observations by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 6.715±0.0036 hours with a brightness amplitude of 1.06 in magnitude, which indicates that the body has a non-spheroidal shape ( U=2 ). [7]

    A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database (LPD), gave a concurring period of 6.71574 hours ( U=n.a. ), as well as a spin axis of (42.0°, 76.0°) in ecliptic coordinates (λ, β). [8]

    Diameter and albedo

    According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Ishihara measures 4.986 and 5.012 kilometers in diameter and its surface has an albedo of 0.235 and 0.2328, respectively. [5] [6] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – derived from 8 Flora, a S-type asteroid and the family's largest member and namesake – and calculates a diameter of 3.74 kilometers with an absolute magnitude of 14.3. [4]

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    References

    1. 1 2 3 4 "9971 Ishihara (1993 HS)". Minor Planet Center. Retrieved 10 April 2017.
    2. 1 2 3 Schmadel, Lutz D. (2006). "(9971) Ishihara [2.18, 0.12, 2.7]". Dictionary of Minor Planet Names – (9971) Ishihara, Addendum to Fifth Edition: 2003–2005. Springer Berlin Heidelberg. p. 49. doi:10.1007/978-3-540-34361-5_391. ISBN   978-3-540-34361-5.
    3. 1 2 3 4 "JPL Small-Body Database Browser: 9971 Ishihara (1993 HS)" (2016-11-23 last obs.). Jet Propulsion Laboratory . Retrieved 22 June 2017.
    4. 1 2 3 4 "LCDB Data for (9971) Ishihara". Asteroid Lightcurve Database (LCDB). Retrieved 10 April 2017.
    5. 1 2 3 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: 1109.4096 . Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68 . Retrieved 10 April 2017.
    6. 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.
    7. 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 10 April 2017.
    8. 1 2 3 Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: 6. arXiv: 1601.02909 . Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573 . Retrieved 10 April 2017.
    9. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 10 April 2017.
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