Astronomy:144 Vibilia

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Short description: Main-belt asteroid
144 Vibilia
000144-asteroid shape model (144) Vibilia.png
3D convex shape model of 144 Vibilia
Discovery[1]
Discovered byC. H. F. Peters
Discovery siteLitchfield Obs.
Discovery date3 June 1875
Designations
(144) Vibilia
Pronunciation/vɪˈbɪliə/[4]
Named afterVibilia
(Roman goddess of traveling)[2]
A875 LA
Minor planet categorymain-belt · Vibilia[3]
AdjectivesVibilian
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
|{{{apsis}}}|helion}}3.2796 AU
|{{{apsis}}}|helion}}2.0350 AU
2.6573 AU
Eccentricity0.2342
Orbital period4.33 yr (1,582 days)
Mean anomaly230.96°
Mean motion0° 13m 39s / day
Inclination4.8123°
Longitude of ascending node76.204°
294.36°
Physical characteristics
Dimensions131.36±33.30 km[5]
134.59±50.58 km[6]
141.34±2.76 km[7]
142.20±1.76 km[8]
142.38±2.6 km (IRAS:15)[9]
Mass(5.30±1.20)×1018 kg[7]
Mean density2.4+0.7−0.5 g/cm3[10]
3.58±0.84 g/cm3[7]
Rotation period13.810 h[11]
13.819±0.002 h[12]
13.824±0.001 h[13]
13.82516±0.00005 h[14]
13.88±0.02 h[13]
Geometric albedo0.05±0.01[5]
0.05±0.06[6]
0.0597±0.002 (IRAS:15)[9]
0.060±0.002[8]
C (Tholen), Ch (SMASS)
C[15]
B–V = 0.727[1]
U–B = 0.402[1]
Absolute magnitude (H)7.91[1][5][8][9] · 7.92±0.02[12][15][16] · 8.03±0.21[17] · 8.03[6]


144 Vibilia is a carbonaceous asteroid from the central region of the asteroid belt, approximately 140 kilometers in diameter. It was discovered on 3 June 1875, by German–American astronomer Christian Peters at Litchfield Observatory of the Hamilton College in Clinton, New York, United States.[18] Peters named it after Vibilia, the Roman goddess of traveling, because he had recently returned from a journey across the world to observe the transit of Venus. Peters also discovered 145 Adeona on the same night. The official naming citation was published by Paul Herget in The Names of the Minor Planets in 1955 (H 19).[2]

Orbit and classification

Vibilia is the largest member and namesake of the Vibilia family, a small asteroid family with 180 known members.[3][19]:23 It orbits the Sun in the central main-belt at a distance of 2.0–3.3 AU once every 4 years and 4 months (1,582 days). Its orbit has an eccentricity of 0.23 and an inclination of 5° with respect to the ecliptic.[1] The asteroid's observation arc begins in May 1905, at Heidelberg Observatory, 30 years after its official discovery observation. It never received a provisional designation.[18]

144 Vibilia has been observed to occult a star eleven times between 1993 and 2018. Eight of these events yielded two or more chords across the asteroid."Occult v4.5.5". http://www.lunar-occultations.com/iota/occult4.htm. 

Physical characteristics

Vibilia is a dark C-type asteroid in the Tholen taxonomy. It is also characterized as a hydrated Ch-subtype in the SMASS classification.[1] This means it probably has a primitive carbonaceous composition.

13-cm radar observations of this asteroid from the Arecibo Observatory between 1980 and 1985 were used to produce a diameter estimate of 131 km.[20] Carry gives a diameter of 141.34 kilometers.[7] According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Vibilia measures between 131.36 and 142.38 kilometers in diameter and its surface has an albedo between 0.05 0.06.[5][6][9][8] The Collaborative Asteroid Lightcurve Link (CALL) adopts the results obtained by IRAS, that is, an albedo of 0.0597 and a diameter of 142.38 kilometers. CALL uses an absolute magnitude of 7.92.[15]

Based upon radar data, the near surface solid density of Vibilia is 2.4 g cm−3. The density had been calibrated against that of 433 Eros; the uncalibrated figure is 3.2 g/cm3.[10] Carry gives a density of 3.58±0.84 g/cm3 with a low porosity.[7]

Several well-defined rotational lightcurves of Vibilia have been obtained from photometric observations since the 1980s. Lightcurve analysis gave a rotation period between 13.810 and 13.88 hours with a brightness amplitude between 0.13 and 0.20 magnitude (U=3/3/3/3).[11][12][13] In 2016, an international study modeled a lightcurve from various photometric data sources. It gave a period of 13.82516 hours. The team also determined two spin axis of (248.0°, 56.0°) and (54.0°, 48.0°) in ecliptic coordinates (λ, β) (U/Q=n.a.).[14]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "JPL Small-Body Database Browser: 144 Vibilia". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2000144. Retrieved 9 July 2017. 
  2. ↑ 2.0 2.1 Schmadel, Lutz D. (2007). "(144) Vibilia". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 28. doi:10.1007/978-3-540-29925-7_145. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 Broz, M.; Morbidelli, A.; Bottke, W. F.; Rozehnal, J.; Vokrouhlický, D.; Nesvorný, D. (March 2013). "Constraining the cometary flux through the asteroid belt during the late heavy bombardment". Astronomy and Astrophysics 551: 16. doi:10.1051/0004-6361/201219296. Bibcode: 2013A&A...551A.117B. 
  4. ↑ Noah Webster (1884) A Practical Dictionary of the English Language
  5. ↑ 5.0 5.1 5.2 5.3 Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T. et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal 814 (2): 13. doi:10.1088/0004-637X/814/2/117. Bibcode: 2015ApJ...814..117N. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015ApJ...814..117N. Retrieved 8 July 2017. 
  6. ↑ 6.0 6.1 6.2 6.3 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. doi:10.3847/0004-6256/152/3/63. Bibcode: 2016AJ....152...63N. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Carry, B. (December 2012). "Density of asteroids". Planetary and Space Science 73 (1): 98–118. doi:10.1016/j.pss.2012.03.009. Bibcode: 2012P&SS...73...98C.  See Table 1 on page 20.
  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 22 October 2019. 
  10. ↑ 10.0 10.1 Magri, C.; Consolmagno, G. J.; Ostro, S. J.; Benner, L. A. M.; Beeney, B. R. (December 2001). "Radar constraints on asteroid regolith compositions using 433 Eros as ground truth". Meteoritics and Planetary Science 36 (12): 1697–1709. doi:10.1111/j.1945-5100.2001.tb01857.x. Bibcode: 2001M&PS...36.1697M. http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?2001M%26PS...36.1697M&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf. Retrieved 9 July 2017. 
  11. ↑ 11.0 11.1 Zappala, V.; Scaltriti, F.; di Martino, M. (November 1983). "Photoelectric photometry of 21 asteroids". Icarus 56 (2): 325–344.ResearchsupportedbytheConsiglioNazionaledelleRicerche. doi:10.1016/0019-1035(83)90042-8. ISSN 0019-1035. Bibcode: 1983Icar...56..325Z. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1983Icar...56..325Z. Retrieved 8 July 2017. 
  12. ↑ 12.0 12.1 12.2 Harris, A. W.; Young, J. W. (October 1989). "Asteroid lightcurve observations from 1979-1981". Icarus 81 (2): 314–364. doi:10.1016/0019-1035(89)90056-0. ISSN 0019-1035. Bibcode: 1989Icar...81..314H. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1989Icar...81..314H. Retrieved 8 July 2017. 
  13. ↑ 13.0 13.1 13.2 Behrend, Raoul. "Asteroids and comets rotation curves – (144) Vibilia". Geneva Observatory. http://obswww.unige.ch/~behrend/page1cou.html#000144. Retrieved 8 July 2017. 
  14. ↑ 14.0 14.1 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. 
  15. ↑ 15.0 15.1 15.2 "LCDB Data for (144) Vibilia". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=144%7CVibilia. Retrieved 8 July 2017. 
  16. ↑ 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. doi:10.1016/j.icarus.2012.07.026. Bibcode: 2012Icar..221..365P. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2012Icar..221..365P. Retrieved 8 July 2017. 
  17. ↑ 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. doi:10.1016/j.icarus.2015.08.007. Bibcode: 2015Icar..261...34V. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015Icar..261...34V. Retrieved 8 July 2017. 
  18. ↑ 18.0 18.1 "144 Vibilia". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=144. Retrieved 8 July 2017. 
  19. ↑ Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. Bibcode: 2015aste.book..297N. 
  20. ↑ Ostro, S. J.; Campbell, D. B.; Shapiro, I. I. (August 1985). "Mainbelt asteroids - Dual-polarization radar observations". Science 229 (4712): 442–446. doi:10.1126/science.229.4712.442. ISSN 0036-8075. PMID 17738665. Bibcode: 1985Sci...229..442O. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1985Sci...229..442O. Retrieved 9 July 2017. 

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