Wikipedia

900 Rosalinde

For the satellite of Uranus, see Rosalind (moon).

900 Rosalinde (prov. designation: A918 PJ or 1918 EC) is an elongated background asteroid from the inner regions of the asteroid belt, that has a mean-diameter of approximately 19 kilometers (12 miles). It was discovered on 10 August 1918, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany.[1] The lengthy S/D-type asteroid has a rotation period of 16.6 hours. It was likely named after "Rosalinde", a character in the operetta Die Fledermaus by Johann Strauss II.[2]

900 Rosalinde
Modelled shape of Rosalinde from its lightcurve
Discovery [1]
Discovered byM. F. Wolf
Discovery siteHeidelberg Obs.
Discovery date10 August 1918
Designations
(900) Rosalinde
Named after
Character "Rosalinde" in the operetta Die Fledermaus (by Johann Strauss II)[2]
A918 PJ · 1918 EC
main-belt [1][3] · (inner)
background [4][5]
Orbital characteristics [3]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc101.46 yr (37,057 d)
Aphelion2.8758 AU
Perihelion2.0705 AU
2.4732 AU
Eccentricity0.1628
3.89 yr (1,421 d)
73.490°
0° 15m 12.24s / day
Inclination11.559°
182.26°
121.78°
Physical characteristics
Mean diameter
  • 18.78±1.4 km[6]
  • 19.56±0.31 km[7]
  • 19.618±0.057 km[8]
16.648±0.009 h[9]
  • 0.085±0.021[8]
  • 0.096±0.004[7]
  • 0.1008±0.017[6]
11.6[1][3]

Orbit and classification edit

Rosalinde is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements.[4][5] It orbits the Sun in the inner asteroid belt at a distance of 2.1–2.9 AU once every 3 years and 11 months (1,421 days; semi-major axis of 2.47 AU). Its orbit has an eccentricity of 0.16 and an inclination of 12° with respect to the ecliptic.[3] The body's observation arc begins at Heidelberg-Königstuhl State Observatory with its official discovery observation on 10 August 1918.[1]

Naming edit

This minor planet was probably named after the character "Rosalinde", Eisenstein's wife, in the operetta Die Fledermaus by Johann Strauss II (1825–1899), after whom 4559 Strauss was named. Rosalinde's maid in the operetta, "Adele", is likely the namesake chosen by Wolf for another asteroid, 812 Adele. Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about the discoverer's source of inspiration from private communications with Dutch astronomer Ingrid van Houten-Groeneveld, who worked as a young astronomer at the discovering Heidelberg Observatory.[2]

Physical characteristics edit

Rosalinde is an S-type/D-type in the SMASS-I spectral type-classification by Xu (1995), which surveyed and classified a total of 221 objects.[5] However, Rosalinde's classification, with its moderate albedo of 0.1 (see below) does not correspond to more modern taxonomies such as the Bus–Binzel SMASS classification (II), where the bright S-types and the dark D-types do not have intermediate albedos.

Rotation period edit

 
3D-model of Rosalinde based on its lightcurve

In June 2011, a rotational lightcurve of Rosalinde was obtained from photometric observations by Meaghann Stoelting and David DeGraffat at the Stull Observatory (784) of the Alfred University in New York. Lightcurve analysis gave a rotation period of 16.648±0.009 hours with a brightness variation of 0.33±0.02 magnitude (U=2+). Assuming an equatorial view, the observers also constrained the object's elongated shape to be at least 36% longer than wide.[9] The result supersedes a tentative period determination by French amateur astronomer René Roy from May 2007 (U=2).[11] Additional observation by the Spanish OBAS group gave a period of 16.70±0.01 hours with an amplitude of 0.28±0.02 magnitude (U=2/2).[12]

In 2016, a modeled lightcurve gave a concurring sidereal period of 16.6868±0.0002 hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), 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 (276.0°, 70.0°) and (90.0°, 39.0°) in ecliptic coordinates (λ, β).[10]

Diameter and albedo edit

According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Rosalinde measures (18.78±1.4), (19.56±0.31) and (19.618±0.057) kilometers in diameter and its surface has an albedo of (0.1008±0.017), (0.096±0.004) and (0.085±0.021), respectively.[6][7][8] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.0931 and calculates a diameter of 18.75 kilometers based on an absolute magnitude of 11.83.[13] Alternative mean-diameter measurements published by the WISE team include (18.191±5.124 km), (19.69±6.22 km) and (20.908±0.160 km) with corresponding albedos of (0.131±0.105), (0.13±0.08) and (0.0750±0.0106).[5][13] On 7 June 2015, an asteroid occultation gave a best-fit ellipse dimension of 19.0 × 19.0 kilometers. These timed observations are taken when the asteroid passes in front of a distant star.[5]

References edit

  1. ^ a b c d e "900 Rosalinde (A918 PJ)". Minor Planet Center. Retrieved 24 February 2020.
  2. ^ a b c Schmadel, Lutz D. (2007). "(900) Rosalinde". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 81. doi:10.1007/978-3-540-29925-7_901. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f "JPL Small-Body Database Browser: 900 Rosalinde (A918 PJ)" (2020-01-24 last obs.). Jet Propulsion Laboratory. Retrieved 24 February 2020.
  4. ^ a b "Asteroid 900 Rosalinde – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 24 February 2020.
  5. ^ a b c d e f g h "Asteroid 900 Rosalinde". Small Bodies Data Ferret. Retrieved 24 February 2020.
  6. ^ a b c 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 24 February 2020.
  7. ^ a b c 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)
  8. ^ a b c 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.
  9. ^ a b Stoelting, Meaghann; DeGraff, David R. (January 2016). "Lightcurve Results for Asteroids 900 Rosalinde, 4666 Dietz, and 6302 Tengukogen" (PDF). Minor Planet Bulletin. 43 (1): 44–45. Bibcode:2016MPBu...43...44S. ISSN 1052-8091. Archived from the original (PDF) on 3 October 2020. Retrieved 24 February 2020.
  10. ^ a b c 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.
  11. ^ Behrend, Raoul. "Asteroids and comets rotation curves – (900) Rosalinde". Geneva Observatory. Retrieved 24 February 2020.
  12. ^ Garceran, Alfonso Carreno; Aznar, Amadeo; Mansego, Enrique Arce; Rodriguez, Pedro Brines; de Haro, Juan Lozano; Silva, Alvaro Fornas; et al. (January 2016). "Nineteen Asteroids Lightcurves at Asteroids Observers (OBAS) - MPPD: 2015 April - September" (PDF). Minor Planet Bulletin. 43 (1): 92–97. Bibcode:2016MPBu...43...92G. ISSN 1052-8091. Archived from the original (PDF) on 3 October 2020. Retrieved 24 February 2020.
  13. ^ a b "LCDB Data for (900) Rosalinde". Asteroid Lightcurve Database (LCDB). Retrieved 24 February 2020.

External links edit

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