725 Amanda

Last updated

725 Amanda
000725-asteroid shape model (725) Amanda.png
Modelled shape of Amanda from its lightcurve
Discovery  [1]
Discovered by J. Palisa
Discovery site Vienna Obs.
Discovery date21 October 1911
Designations
(725) Amanda
PronunciationGerman: [aːˈmandaː] [2]
Named after
Amanda Schorr, wife of Richard Schorr (1867–1951)
(German astronomer) [3]
A911 UQ ·2016 FH6
1911 ND
Orbital characteristics   [4]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc 104.58 yr (38,198 d)
Aphelion 3.1422 AU
Perihelion 2.0022 AU
2.5722 AU
Eccentricity 0.2216
4.13 yr (1,507 d)
114.51°
0° 14m 20.04s / day
Inclination 3.7902°
68.679°
323.36°
Physical characteristics
3.749  h [12]
  • (145.0°, −63.0°) (λ1/β1) [6]
  • (320.0°, −70.0°) (λ2/β2) [6]

    725 Amanda ( prov. designation:A911 UQor1911 ND) is a dark background asteroid, approximately 22 kilometers (14 miles) in diameter, that is located in the central regions of the asteroid belt. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 21 October 1911. [1] The carbonaceous C-type asteroid (CSU/C0) has a short rotation period of 3.7 hours. It was named after Amanda Schorr, wife of German astronomer Richard Schorr (1867–1951). [3]

    Contents

    Orbit and classification

    Amanda is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. [5] [6] [7] It orbits the Sun in the central asteroid belt at a distance of 2.0–3.1  AU once every 4 years and 2 months (1,507 days; semi-major axis of 2.57 AU). Its orbit has an eccentricity of 0.22 and an inclination of 4° with respect to the ecliptic. [4] The body's observation arc begins at Vienna Observatory on 29 September 1915, almost four years after its official discovery observation. [1]

    Naming

    This minor planet was named after Amanda Ruth Smith, born to John and Ruth Smith of Jackson, MS.(May 1980). Amanda(human) was named for the song "Amanda" by Waylon Jennings. Her mother always said that she chose that name because she, like the song verse was always "Amanda light of my life." [3] In 2010, Ruth Smith made the first ever arrangement with NASA to legally purchase the minor planet, "Amanda U1911" for an undisclosed sum of money(USD) and exclusively owns all rights to it. Amanda Ruth Smith (human) was given a certified certificate of ownership by NASA with the serial number "SHMILY-12.0522."©

    Physical characteristics

    In the Tholen classification, Amanda's spectral type is closest to that of a carbonaceous C-type asteroid, yet also somewhat similar to a stony S-type with an "unusual" spectrum (CSU). [4] In the taxonomy by Barucci (1987), the asteroid is a dark C-type (C0). [6]

    Rotation period and poles

    Lightcurve-based 3D-model of Amanda 725Amanda (Lightcurve Inversion).png
    Lightcurve-based 3D-model of Amanda

    A rotational lightcurve of Amanda was obtained from photometric observations by European astronomers at the La Silla Observatory before 1995. Lightcurve analysis gave a well-defined rotation period of 3.749 hours with a brightness variation of 0.35 magnitude ( U=3 ). [12]

    In October 2010, French amateur astronomer Maurice Audejean ( B92 ) determined a concurring period of (3.7431±0.0003) hours with an amplitude of (0.42±0.01) magnitude ( U=3 ), [13] while in August 2018, a further observation by the TESS-team reported a period of (3.74301±0.00005) hours and an amplitude of (0.27±0.05) magnitude ( U=2 ). [14]

    In 2016, a modeled lightcurve gave a sidereal period of 3.74311±0.00002 hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers, as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys ( 950 ). The study also determined two spin axes of (145.0°, −63.0°) and (320.0°, −70.0°) in ecliptic coordinates (λ, β). [15]

    Diameter and albedo

    According to the surveys carried out by the Japanese Akari satellite, the Infrared Astronomical Satellite IRAS, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Amanda measures (20.49±0.28), (21.51±2.2) and (23.687±0.215) in diameter and its surface has an albedo of (0.082±0.003), (0.0721±0.017) and (0.068±0.015), respectively. [8] [9] [10] [11]

    The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0824 and calculates a diameter of 21.56 kilometers based on an absolute magnitude of 11.66. [16] Alternative mean-diameters published by the WISE team include (19.53±6.07  km ), (21.68±6.40 km), (23.286±0.149 km) and (30.73±4.85 km) with a corresponding albedo of (0.08±0.04), (0.055±0.037), (0.0509±0.0052) and (0.03±0.03). [6] [16]

    Related Research Articles

    460 Scania is a background asteroid and a slow rotator from the central regions of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory on 22 October 1900. The uncommon K-type asteroid has an exceptionally long rotation period of 164.1 hours and measures approximately 21 kilometers in diameter. It was named after the Swedish region of Scania, where a meeting was held by the Astronomische Gesellschaft in 1904.

    716 Berkeley is a background asteroid from the central regions of the asteroid belt. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 30 July 1911. The stony S-type asteroid has a rotation period of 15.6 hours and measures approximately 21 kilometers in diameter. It was named after the city of Berkeley, California, where the discoverer's colleague Armin Otto Leuschner (1868–1953) was the director of the local observatory.

    717 Wisibada is a dark background asteroid from the outer regions of the asteroid belt. It was discovered on 26 August 1911, by German astronomer Franz Kaiser at the Heidelberg-Königstuhl State Observatory in southwest Germany. The D-type asteroid measures approximately 29 kilometers in diameter with no rotation period yet determined. It was named after the discoverer's birthplace, the city of Wiesbaden in Hesse, Germany.

    <span class="mw-page-title-main">722 Frieda</span> Bright background asteroid and slow rotator

    722 Frieda is a bright background asteroid and slow rotator from the inner regions of the asteroid belt. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 18 October 1911. The stony S-type asteroid has a notably long rotation period of 131.1 hours and measures approximately 9 kilometers in diameter. It was named after Frieda Hillebrand, daughter of Austrian astronomer Karl Hillebrand (1861–1939), and grand-daughter of Edmund Weiss (1837–1917) who had been the director of the discovering observatory.

    745 Mauritia is a dark background asteroid from the outer regions of the asteroid belt, approximately 24 kilometers in diameter. It was discovered on 1 March 1913, by German astronomer Franz Kaiser at the Heidelberg-Königstuhl State Observatory in Germany. The presumed carbonaceous C-type asteroid has a rotation period of 9.9 hours. It was named after Saint Maurice, patron of the Saint Mauritius church in the city of Wiesbaden, where the discoverer was born.

    <span class="mw-page-title-main">748 Simeïsa</span> Hilda asteroid

    748 Simeïsa is a very large Hilda asteroid from the outermost regions of the asteroid belt, approximately 104 kilometers in diameter. It was discovered on 14 March 1913, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The dark P-type asteroid has a rotation period of 11.9 hours and a shape that is reminiscent of a tetrahedron. It was the first asteroid discovery made in Russia and named after the discovering observatory and its nearby Crimean town, Simeiz.

    783 Nora is a dark background asteroid from the inner regions of the asteroid belt. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 18 March 1914. The carbonaceous C-type asteroid has a longer-than average rotation period of 55.5 hours and measures approximately 40 kilometers in diameter. It was likely named after Nora Helmer, principal character in the play A Doll's House by Norwegian poet Henrik Ibsen.

    786 Bredichina is a carbonaceous and very large background asteroid, approximately 104 kilometers in diameter, located in the outer region of the asteroid belt. It was discovered by German astronomer Franz Kaiser at the Heidelberg-Königstuhl State Observatory on 20 April 1914. The elongated C-type asteroid has a longer than average rotation period of 29.4 hours. It was named after Russian astronomer Fyodor Bredikhin (1831–1904).

    794 Irenaea is a dark background asteroid from the outer regions of the asteroid belt. It was discovered on 27 August 1914, by Austrian astronomer Johann Palisa at the Vienna Observatory. The presumed C-type asteroid has a rotation period of 9.1 hours and measures approximately 36 kilometers in diameter. It was likely named after Irene Hillebrand, daughter of Austrian astronomer Edmund Weiss (1837–1917).

    866 Fatme is a large background asteroid, approximately 86 kilometers in diameter, located in the outer region of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory on 25 February 1917. The X-type asteroid has a short rotation period of 5.8 hours. It was named after "Fatme", a character in the opera Abu Hassan by Carl Maria von Weber (1786–1826).

    1018 Arnolda, provisional designation 1924 QM, is a stony asteroid from the central regions of the asteroid belt, approximately 16 kilometers in diameter. It was discovered on 3 March 1924, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid was named after physicist Arnold Berliner.

    1113 Katja, provisional designation 1928 QC, is a background asteroid from the outer regions of the asteroid belt, approximately 39 kilometers in diameter. It was discovered by Pelageya Shajn at the Simeiz Observatory in 1928, and named after Ekaterina Iosko, a staff member at the discovering observatory.

    1194 Aletta, provisional designation 1931 JG, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 55 kilometers in diameter. It was discovered on 13 May 1931, by South African astronomer Cyril Jackson at Johannesburg Observatory in South Africa. It was later named after the discoverer's wife Aletta Jackson.

    <span class="mw-page-title-main">1555 Dejan</span> Asteroid from the background population of the central regions of the asteroid belt

    1555 Dejan, provisional designation 1941 SA, is an asteroid from the background population of the central regions of the asteroid belt, approximately 22 kilometers in diameter. It was discovered on 15 September 1941, by Belgian astronomer Fernand Rigaux at the Royal Observatory of Belgium in Uccle. The asteroid was named after Dejan Đurković, son of Serbian astronomer Petar Đurković.

    <span class="mw-page-title-main">1274 Delportia</span>

    1274 Delportia, provisional designation 1932 WC, is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 10 kilometers in diameter. It was discovered on 28 November 1932, by Belgian astronomer Eugène Delporte at Uccle Observatory in Belgium. It was named after the discoverer himself.

    <span class="mw-page-title-main">1277 Dolores</span>

    1277 Dolores is a carbonaceous background asteroid from the central regions of the asteroid belt, approximately 27 kilometers in diameter. It was discovered on 18 April 1933, by Soviet astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The asteroid was named after Spanish communist Dolores Ibárruri.

    1421 Esperanto, provisional designation 1936 FQ, is a dark background asteroid from the outer regions of the asteroid belt, approximately 55 kilometers in diameter. It was discovered on 18 March 1936, by Finnish astronomer Yrjö Väisälä at the Iso-Heikkilä Observatory in Turku, southwest Finland. The presumed C-type asteroid has a rotation period of nearly 22 hours. It was named for the artificial language Esperanto.

    <span class="mw-page-title-main">1283 Komsomolia</span> Main-belt asteroid

    1283 Komsomolia is a metallic background asteroid and potentially slow rotator from the outer regions of the asteroid belt. Discovered by Vladimir Albitsky in 1925, it was later named after Komsomol, a political youth organization of the former Soviet Union. The M-type asteroid has roughly a rotation period 96 hours of and measures approximately 30 kilometers in diameter.

    1989 Tatry, provisional designation 1955 FG, is a carbonaceous Vestian asteroid and tumbling slow rotator from the inner regions of the asteroid belt, approximately 16 kilometers in diameter.

    <span class="mw-page-title-main">1236 Thaïs</span>

    1236 Thaïs is a dark background asteroid from the inner regions of the asteroid belt. The rare T-type asteroid has a notably long rotation period of 72 hours and measures approximately 18 kilometers. It was discovered on 6 November 1931, by Soviet astronomer Grigory Neujmin at Simeiz Observatory on the Crimean peninsula, and named after the ancient Greek prostitute Thaïs.

    References

    1. 1 2 3 4 5 "725 Amanda (A911 UQ)". Minor Planet Center. Retrieved 15 June 2020.
    2. ↑ (German Names)
    3. 1 2 3 Schmadel, Lutz D. (2007). "(725) Amanda". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 70. doi:10.1007/978-3-540-29925-7_726. ISBN   978-3-540-00238-3.
    4. 1 2 3 4 5 6 7 8 "JPL Small-Body Database Browser: 725 Amanda (A911 UQ)" (2020-04-28 last obs.). Jet Propulsion Laboratory . Retrieved 15 June 2020.
    5. 1 2 "Asteroid 725 Amanda – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 15 June 2020.
    6. 1 2 3 4 5 6 "Asteroid 725 Amanda – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 15 June 2020.
    7. 1 2 Zappalà, V.; Bendjoya, Ph.; Cellino, A.; Farinella, P.; Froeschle, C. (1997). "Asteroid Dynamical Families". NASA Planetary Data System: EAR-A-5-DDR-FAMILY-V4.1. Retrieved 15 June 2020.} (PDS main page)
    8. 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. (online, AcuA catalog p. 153)
    9. 1 2 3 4 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T . Retrieved 15 June 2020.
    10. 1 2 3 4 Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R.; et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System. Bibcode:2016PDSS..247.....M . Retrieved 15 June 2020.
    11. 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". The Astrophysical Journal. 791 (2): 11. arXiv: 1406.6645 . Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. S2CID   119293330.
    12. 1 2 3 di Martino, Mario; Dotto, E.; Barucci, M. A.; Fulchignoni, M.; Rotundi, A. (May 1994). "Photoelectric photometry of ten small and fast spinning asteroids". Icarus. 109 (1): 210–218. Bibcode:1994Icar..109..210D. doi:10.1006/icar.1994.1087. ISSN   0019-1035. Archived from the original on 2 February 2017. Retrieved 15 June 2020.
    13. ↑ Behrend, Raoul. "Asteroids and comets rotation curves – (725) Amanda". Geneva Observatory. Retrieved 15 June 2020.
    14. ↑ Pál, András; Szakáts, Róbert; Kiss, Csaba; Bódi, Attila; Bognár, Zsófia; Kalup, Csilla; et al. (March 2020). "Solar System Objects Observed with TESS—First Data Release: Bright Main-belt and Trojan Asteroids from the Southern Survey". The Astrophysical Journal Supplement Series. 247 (1): 26. arXiv: 2001.05822 . Bibcode:2020ApJS..247...26P. doi: 10.3847/1538-4365/ab64f0 . ISSN   0067-0049.
    15. ↑ Hanuš, J.; Ďurech, J.; Brož, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution". Astronomy and Astrophysics. 551: A67. arXiv: 1301.6943 . Bibcode:2013A&A...551A..67H. doi:10.1051/0004-6361/201220701. ISSN   0004-6361. S2CID   118627434.
    16. 1 2 "LCDB Data for (725) Amanda". Asteroid Lightcurve Database (LCDB). Retrieved 15 June 2020.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.