1078 Mentha

1078 Mentha
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 7 December 1926
Designations
MPC designation (1078) Mentha
Named after
 Mentha (flowering plant) [2]
1926 XB& · 1951 CF1
1952 LD · A917 CB [3]
A924 EP
main-belt · (inner) [4]
background [5]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 93.66 yr (34,208 days)
Aphelion 2.5832 AU
Perihelion 1.9555 AU
2.2693 AU
Eccentricity 0.1383
3.42 yr (1,249 days)
142.04°
0° 17m 17.88s / day
Inclination 7.3716°
93.851°
43.568°
Physical characteristics
Dimensions 9.94±0.28 km[6]
12.619±0.242 km[7]
13.59±3.01 km[8]
13.660±0.134 km[9]
13.675 km[10]
13.68 km (taken)[4]
15.37±2.11 km[11]
82.870±0.2341 h[12]
85±2 h[13]
0.126±0.259[11]
0.1641[10]
0.1819±0.0375[9]
0.262±0.041[7]
0.31±0.18[8]
0.343±0.020[6]
Tholen = S [1][4]
B–V = 0.889[1]
U–B = 0.490[1]
11.33±0.11[14] · 11.455±0.002 (R)[12] · 11.60[8] · 11.80[1][6][9] · 11.9[4] · 11.9±0.2[10][13] · 11.94[11]

    1078 Mentha, provisional designation 1926 XB, is a stony background asteroid from the inner regions of the asteroid belt, approximately 13 kilometers in diameter. It was discovered on 7 December 1926, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany.[15] Only in 1958, it was realized that this object was a rediscovery of an already numbered but lost asteroid (864 Aase).[3]

    The asteroid was named after the flowering plant of the mint family, Mentha.[2] It has a longer-than average spin rate of 85 hours and possibly an irregular, elongated shape.[4]

    Identification with former lost asteroid

    Sometimes, discovered objects turn out to be a rediscovery of a previously lost minor planet. This can be determined by calculating the "new" object's orbit (once it is firmly known) backwards and checking its past positions against those previously recorded for the lost object. Nowadays these identities between two objects are found before they are numbered.

    In 1958, however, French astronomer André Patry at Nice Observatory found such identity between Mentha, 1926 XB, and the lost minor planet 864 Aase, A917 CB, which had never been re-observed after its discovery by Max Wolf in 1917.[3] Since it was realized that Mentha and Aase were one and the same object, the Minor Planet Center resolved this conflict by keeping everything associated with "1078 Mentha", adding the two oppositional observations by Max Wolf from 1917, and completely vacated "864 Aase", reusing its name and number for another, unrelated discovery made by Reinmuth.[16]

    Orbit and classification

    Mentha is a non-family asteroid of the main belt's background population.[5] It orbits the Sun in the inner asteroid belt at a distance of 2.0–2.6 AU once every 3 years and 5 months (1,249 days; semi-major axis of 2.27 AU). Its orbit has an eccentricity of 0.14 and an inclination of 7° with respect to the ecliptic.[1]

    The asteroid was first observed as A917 CB at Heidelberg in February 1907 (which is the original discovery of 864 Aase, before vacated). The body's observation arc begins at Simeiz Observatory in March 1924, almost four years prior to its official discovery observation at Heidelberg.[15]

    Physical characteristics

    In the Tholen classification, Mentha is a common stony S-type asteroid.[1][4]

    Rotation period

    In February 1989, a first rotational lightcurve of Mentha was obtained from photometric observations by Polish astronomer Wiesław Wiśniewski. Lightcurve analysis gave a well-defined rotation period of 85 hours with a brightness variation of 0.87 magnitude (U=3).[13] In February 2013, a similar period of 82.870 hours with an amplitude of 0.65 magnitude was measured by astronomers at the Palomar Transient Factory in California (U=2).[12] A high brightness amplitude is typically indicative for an elongated rather than spherical shape. Its long period is close to that of slow rotators.

    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, Mentha measures between 9.94 and 15.37 kilometers in diameter and its surface has an albedo between 0.126 and 0.343.[6][7][8][9][10][11]

    The Collaborative Asteroid Lightcurve Link agrees with Petr Pravec's revised WISE data and takes an albedo of 0.1641 and a diameter of 13.68 kilometers based on an absolute magnitude of 11.9.[4]

    Naming

    This minor planet was named after Mentha, a flowering herb of the mint family.[2] The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 102).[2]

    Reinmuth's flowers

    Due to his many discoveries, Karl Reinmuth submitted a large list of 66 newly named asteroids in the early 1930s. The list covered his discoveries with numbers between (1009) and (1200). This list also contained a sequence of 28 asteroids, starting with 1054 Forsytia, that were all named after plants, in particular flowering plants (also see list of minor planets named after animals and plants).[17]

    References

    1. 1 2 3 4 5 6 7 8 "JPL Small-Body Database Browser: 1078 Mentha (1926 XB)" (2017-10-29 last obs.). Jet Propulsion Laboratory. Retrieved 29 November 2017.
    2. 1 2 3 4 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1078) Mentha. Springer Berlin Heidelberg. p. 92. ISBN 978-3-540-00238-3. Retrieved 29 November 2017.
    3. 1 2 3 Patry, A. (June 1958). "Identification: (864) Aase = (1078) Mentha". Minor Planet Circular (1763). Bibcode:1958MPC...1763...1P. Retrieved 29 November 2017.
    4. 1 2 3 4 5 6 7 "LCDB Data for (1078) Mentha". Asteroid Lightcurve Database (LCDB). Retrieved 29 November 2017.
    5. 1 2 "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 29 November 2017.
    6. 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 29 November 2017.
    7. 1 2 3 Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos" (PDF). The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 29 November 2017.
    8. 1 2 3 4 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. Retrieved 29 November 2017.
    9. 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" (PDF). The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 29 November 2017.
    10. 1 2 3 4 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 29 November 2017.
    11. 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 29 November 2017.
    12. 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 29 November 2017.
    13. 1 2 3 Wisniewski, W. Z.; Michalowski, T. M.; Harris, A. W.; McMillan, R. S. (March 1995). "Photoelectric Observations of 125 Asteroids". Abstracts of the Lunar and Planetary Science Conference. Bibcode:1995LPI....26.1511W. Retrieved 29 November 2017.
    14. ↑ 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 29 November 2017.
    15. 1 2 "1078 Mentha (1926 XB)". Minor Planet Center. Retrieved 29 November 2017.
    16. ↑ Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (864) Aase. Springer Berlin Heidelberg. pp. 78–79. ISBN 978-3-540-00238-3. Retrieved 29 November 2017.
    17. ↑ Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1054) Forsytia. Springer Berlin Heidelberg. p. 90. ISBN 978-3-540-00238-3. Retrieved 28 November 2017.
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