Astronomy:698 Ernestina

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698 Ernestina
000698-asteroid shape model (698) Ernestina.png
Modelled shape of Ernestina from its lightcurve
Discovery [1]
Discovered byJ. Helffrich
Discovery siteHeidelberg Obs.
Discovery date5 March 1910
Designations
(698) Ernestina
Named afterErnst Wolf
(son of Max Wolf)[2]
A910 ED · A908 WB
1910 JX
Minor planet categorymain-belt [1][3] · (outer)[4]
background [5][6][7]
Orbital characteristics [3]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc111.16 yr (40,601 d)
|{{{apsis}}}|helion}}3.1847 AU
|{{{apsis}}}|helion}}2.5490 AU
2.8669 AU
Eccentricity0.1109
Orbital period4.85 yr (1,773 d)
Mean anomaly269.92°
Mean motion0° 12m 10.8s / day
Inclination11.532°
Longitude of ascending node40.630°
98.687°
Physical characteristics
Mean diameter
Rotation period5.0363±0.0005 h[11]
Pole ecliptic latitude
  • (213.0°, −66.0°) (λ1/β1)[12]
  • (76.0°, −49.0°) (λ2/β2)[12]
Geometric albedo
Absolute magnitude (H)


698 Ernestina (prov. designation: A910 ED or 1910 JX) is a background asteroid, approximately 27 kilometers (17 miles) in diameter, located in the outer regions of the asteroid belt. It was discovered on 5 March 1910, by German astronomer Joseph Helffrich at the Heidelberg-Königstuhl State Observatory.[1] The presumed carbonaceous C-type asteroid has a rotation period of 5.0 hours. It was named after Ernst Wolf, son of German astronomer and prolific discoverer of minor planets, Max Wolf.[2]

Orbit and classification

Ernestina 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 outer asteroid belt at a distance of 2.5–3.2 AU once every 4 years and 10 months (1,773 days; semi-major axis of 2.87 AU). Its orbit has an eccentricity of 0.11 and an inclination of 12° with respect to the ecliptic.[3] The asteroid was first observed as 1908 WB at Heidelberg Observatory on 28 November 1908. The body's observation arc begins with its official discovery observation on 5 March 1910.[1]

Naming

This minor planet was named after Ernst Wolf, son of German astronomer Max Wolf (1863–1932), who has discovered many asteroids at Heidelberg including some of the first near-Earth objects and Jupiter trojans. The naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 71).[2]

Physical characteristics

Ernestina is an assumed carbonaceous C-type asteroid.[4] In a taxonomic classification based on MOVIS near-infrared colors, the asteroid's preliminary determined Cgx-type was ultimately rejected and its final class changed to "undefined" (U). MOVIS data has been obtained by the VISTA Hemisphere Survey using the VISTA telescope at Paranal Observatory in Chile.[13]

Rotation period

In October 2005, a rotational lightcurve of Ernestina was obtained from photometric observations by an international collaboration led by Donald Pray at Carbuncle Hill Observatory (912). Lightcurve analysis gave a well-defined rotation period of 5.0363±0.0005 hours with a brightness variation of 0.30±0.02 magnitude ({{{1}}}).[11] Alternative period determinations in ascending order include: 5.00±0.05 h by Gordana Apostolovska in 2011 ({{{1}}}),[4] 5.03654±0.00004 h by Laurent Bernasconi in 2002 ({{{1}}}),[14] 5.037±0.0008 h by astronomers at the Palomar Transient Factory in 2010 ({{{1}}}),[15] 5.0415±0.0006 h by René Roy in 2017 ({{{1}}}),[14] 5.0431±0.0002 h by David Polishook in 2005 ({{{1}}}),[16] and 5.07 h by Violeta Ivanova in 2002 ({{{1}}}).[17]

Poles

Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring sidereal period of (5.03660±0.00005) and (5.03661±0.00001) hours, respectively. Each modeled lightcurve also determined two spin axes of (213.0°, −66.0°) and (76.0°, −49.0°), as well as (282.0°, −79.0°) and (114.0°, −45.0°) in ecliptic coordinates (λ, β), respectively.[12][18]

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), Ernestina measures (26.74±0.63), (27.03±1.2) and (29.804±0.438) kilometers in diameter and its surface has an albedo of (0.130±0.007), (0.1269±0.012) and (0.095±0.016), respectively.[8][9][10] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1064 and a diameter of 26.92 kilometers based on an absolute magnitude of 10.9.[4] The WISE team also published an alternative mean-diameter (27.037±0.242 km) and an albedo of (0.116±0.022).[6]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 "698 Ernestina (A910 ED)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=698. 
  2. ↑ 2.0 2.1 2.2 Schmadel, Lutz D. (2007). "(698) Ernestina". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 68. doi:10.1007/978-3-540-29925-7_699. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 3.2 3.3 "JPL Small-Body Database Browser: 698 Ernestina (A910 ED)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2000698. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 "LCDB Data for (698) Ernestina". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=698. 
  5. ↑ 5.0 5.1 "Asteroid 698 Ernestina – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. https://newton.spacedys.com/astdys/index.php?pc=1.1.6&n=698. 
  6. ↑ 6.0 6.1 6.2 "Asteroid 698 Ernestina – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=698+Ernestina. 
  7. ↑ 7.0 7.1 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. https://sbnarchive.psi.edu/pds3/non_mission/EAR_A_5_DDR_FAMILY_V4_1/data/family.tab. Retrieved 15 March 2020.  (PDS main page)
  8. ↑ 8.0 8.1 8.2 8.3 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. doi:10.1093/pasj/63.5.1117. Bibcode: 2011PASJ...63.1117U.  (online, AcuA catalog p. 153)
  9. ↑ 9.0 9.1 9.2 9.3 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. https://sbnarchive.psi.edu/pds3/iras/IRAS_A_FPA_3_RDR_IMPS_V6_0/data/diamalb.tab. Retrieved 20 July 2020. 
  10. ↑ 10.0 10.1 10.2 10.3 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. https://sbnarchive.psi.edu/pds3/non_mission/EAR_A_COMPIL_5_NEOWISEDIAM_V1_0/data/neowise_mainbelt.tab. Retrieved 20 July 2020. 
  11. ↑ 11.0 11.1 Pray, Donald P.; Galad, Adrian; Gajdos, Stefan; Vilagi, Jozef; Cooney, Walt; Gross, John et al. (December 2006). "Lightcurve analysis of asteroids 53, 698, 1016, 1523, 1950, 4608, 5080 6170, 7760, 8213, 11271, 14257, 15350 and 17509". Minor Planet Bulletin 33 (4): 92–95. ISSN 1052-8091. Bibcode: 2006MPBu...33...92P. http://www.minorplanet.info/MPB/issues/MPB_33-4.pdf. 
  12. ↑ 12.0 12.1 12.2 Hanus, J.; Durech, J.; Oszkiewicz, D. A.; Behrend, R.; Carry, B.; Delbo, M. et al. (February 2016). "New and updated convex shape models of asteroids based on optical data from a large collaboration network". Astronomy and Astrophysics 586: 24. doi:10.1051/0004-6361/201527441. Bibcode: 2016A&A...586A.108H. 
  13. ↑ 13.0 13.1 Popescu, M.; Licandro, J.; Carvano, J. M.; Stoicescu, R.; de León, J.; Morate, D. et al. (September 2018). "Taxonomic classification of asteroids based on MOVIS near-infrared colors". Astronomy and Astrophysics 617: A12. doi:10.1051/0004-6361/201833023. ISSN 0004-6361. Bibcode: 2018A&A...617A..12P.  (VizieR online cat, record)
  14. ↑ 14.0 14.1 Behrend, Raoul. "Asteroids and comets rotation curves – (698) Ernestina". Geneva Observatory. http://obswww.unige.ch/~behrend/page2cou.html#000698. 
  15. ↑ 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. doi:10.1088/0004-6256/150/3/75. Bibcode: 2015AJ....150...75W. 
  16. ↑ Polishook, D.; Brosch, N. (February 2009). "Photometry and spin rate distribution of small-sized main belt asteroids". Icarus 199 (2): 319–332. doi:10.1016/j.icarus.2008.10.020. Bibcode: 2009Icar..199..319P. 
  17. ↑ Ivanova, V. G.; Apostolovska, G.; Borisov, G. B.; Bilkina, B. I. (November 2002). "Results from photometric studies of asteroids at Rozhen National Observatory, Bulgaria". Asteroids, Comets, and Meteors: ACM 2002 500: 505–508. ISSN 1609-042X. Bibcode: 2002ESASP.500..505I. 
  18. ↑ Ďurech, J.; Hanuš, J.; Oszkiewicz, D.; Vančo, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics 587: A48. doi:10.1051/0004-6361/201527573. ISSN 0004-6361. Bibcode: 2016A&A...587A..48D. 

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