 Lightcurve-base 3D-model ofVibilia on the top with an image of the asteroid on the bottom. | |
| Discovery[1] | |
|---|---|
| Discovered by | C. H. F. Peters |
| Discovery site | Litchfield Obs. |
| Discovery date | 3 June 1875 |
| Designations | |
| (144) Vibilia | |
| Pronunciation | /vɪˈbɪliə/[2] |
Named after | Vibilia (Roman goddess of traveling)[3] |
| A875 LA | |
| main-belt · Vibilia[4] | |
| Adjectives | Vibilian |
| Orbital characteristics[1] | |
| Epoch 4 September 2017 (JD 2458000.5) | |
| Aphelion | 3.2796AU |
| Perihelion | 2.0350 AU |
| 2.6573 AU | |
| Eccentricity | 0.2342 |
| 4.33yr (1,582 days) | |
| 230.96° | |
| 0° 13m 39s / day | |
| Inclination | 4.8123° |
| 76.204° | |
| 294.36° | |
| Physical characteristics | |
| Dimensions | 131.36±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] |
Meandensity | 2.4+0.7 −0.5 g/cm3[10] 3.58±0.84 g/cm3[7] |
| 13.810h[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] | |
| 0.05±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] | |
| 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 carbonaceousasteroid from the central region of theasteroid belt, approximately 140 kilometers in diameter. It was discovered on 3 June 1875, by German–American astronomerChristian Peters atLitchfield Observatory of theHamilton College in Clinton, New York, United States.[18] Peters named it after Vibilia, theRoman goddess of traveling, because he had recently returned from a journey across the world to observe thetransit of Venus. Peters also discovered145 Adeona on the same night. The official naming citation was published byPaul Herget inThe Names of the Minor Planets in 1955 (H 19).[3]
Vibilia is the largest member and namesake of theVibilia family, a smallasteroid family with 180 known members.[4][19]: 23 It orbits the Sun in thecentral main-belt at a distance of 2.0–3.3 AU once every 4 years and 4 months (1,582 days). Its orbit has aneccentricity of 0.23 and aninclination of 5° with respect to theecliptic.[1] The asteroid's observation arc begins in May 1905, atHeidelberg Observatory, 30 years after its official discovery observation. It never received aprovisional designation.[18]
144 Vibilia has been observed tooccult astar eleven times between 1993 and 2018. Eight of these events yielded two or more chords across the asteroid."Occult v4.5.5". Archived fromthe original on 26 December 2018. Retrieved15 September 2018.
Vibilia is a darkC-type asteroid in theTholen taxonomy. It is also characterized as a hydrated Ch-subtype in theSMASS classification.[1] This means it probably has a primitivecarbonaceous composition.
13-cm radar observations of this asteroid from theArecibo 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 SatelliteIRAS, the JapaneseAkari satellite, and NASA'sWide-field Infrared Survey Explorer with its subsequentNEOWISE mission,Vibilia measures between 131.36 and 142.38 kilometers in diameter and its surface has analbedo between 0.05 0.06.[5][6][9][8] TheCollaborative 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 anabsolute magnitude of 7.92.[15]
Based upon radar data, the near surface solid density ofVibilia is 2.4 g cm−3. The density had been calibrated against that of433 Eros; the uncalibrated figure is 3.2 g/cm3.[10] Carry gives a density of3.58±0.84 g/cm3 with a low porosity.[7]
Several well-defined rotationallightcurves ofVibilia have been obtained from photometric observations since the 1980s. Lightcurve analysis gave arotation period between 13.810 and 13.88 hours with a brightness amplitude between 0.13 and 0.20magnitude (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 twospin axis of (248.0°, 56.0°) and (54.0°, 48.0°) inecliptic coordinates (λ, β) (U/Q=n.a.).[14]
