1433 Geramtina,provisional designation1937 UC,is a stony Gefionasteroidfrom the central regions of theasteroid belt,approximately 14 kilometers in diameter. It was discovered by Belgian astronomerEugène Delporteat theRoyal Observatory of Belgiumin Uccle on 30 October 1937.[11]
| Discovery[1] | |
|---|---|
| Discovered by | E. Delporte |
| Discovery site | Uccle Obs. |
| Discovery date | 30 October 1937 |
| Designations | |
| (1433) Geramtina | |
Named after | Sister of Bror Asplind[2] (Swedish astronomer) |
| 1937 UC·1951 XH 1967 EH·1974 TX1 | |
| main-belt·(outer)[3] Gefion[4][5]·background[6] | |
| Orbital characteristics[1] | |
| Epoch4 September 2017 (JD2458000.5) | |
| Uncertainty parameter0 | |
| Observation arc | 79.92 yr (29,191 days) |
| Aphelion | 3.2757AU |
| Perihelion | 2.3162 AU |
| 2.7960 AU | |
| Eccentricity | 0.1716 |
| 4.68yr(1,708 days) | |
| 19.222° | |
| 0° 12m38.88s/ day | |
| Inclination | 8.2369° |
| 321.57° | |
| 93.975° | |
| Physical characteristics | |
| Dimensions | 12.687±0.209km[7] 14.22 km(calculated)[3] 14.574±0.247km[8] |
| 14h[9] | |
| 0.1910±0.0170[8] 0.20(assumed)[3] 0.251±0.027[7] | |
| SMASS=S[1][3]·S[10] | |
| 11.43±0.23[10]·11.60[1][3][7][8] | |
The asteroid was named "Geramtina" after the sister of Swedish astronomer Bror Asplind.Geramtinahas anordinary chondriticcomposition and has been considered a candidate for being the parent body of theH chondrites.However, results are inconclusive, and recentHCManalysis suggest thatGeramtinais a Gefionianinterloperrather than a core member of the family. The asteroid has a tentativerotation periodof 14 hours.
Orbit and classification
editGeramtinais a core member of theGefion family(516), which is also known as Minerva family.[4][5]However, it is a non-familyasteroid of the main belt'sbackground populationaccording to Nesvorny's application of the body'sproper orbital elementsto thehierarchical clustering method(synthetic),[6]suggesting thatGeramtinais aninterloperrather than a core member.
It orbits the Sun in thecentralmain-belt at a distance of 2.3–3.3AUonce every 4 years and 8 months (1,708 days). Its orbit has aneccentricityof 0.17 and aninclinationof 8°with respect to theecliptic.[1]The body'sobservation arcbegins with its official discovery observation at Uccle in 1937.[11]
Physical characteristics
editSpectral type
editIn theSMASS classification,Geramtinais a common, stonyS-type asteroid.[1]The photometric survey byPan-STARRShas also characterized the asteroid as an S-type.[10]
Mineralogy
editThe spectra ofGeramtinatogether with4182 Mount Lockehave been studies in a mineralogical assessment to test whether these considered core members of the Gefion family might be the source of theL chondrites,a common group ofmeteorites,due to their dynamical and compositional characteristics.[4]Spectra obtained with the 3-meterNASA IRTF telescope,however, were inconclusive and suggest thatGeramtinamight as well be aH chondriterather than an L chondrite, but allows for the determination of a general S(IV)ordinary chondriticcomposition. The researchers also acknowledged that the Gefion family space has a high abundance ofinterloperswhich needs to be ruled out first.[4]
Rotation period
editIn October 2007, a rotationallightcurveofGeramtinawas obtained from photometric observations at the National Undergraduate Research Observatory, NURO, in Flagstaff, Arizona. Lightcurve analysis gave a tentativerotation periodof 14 hours (monomodal solution) with a brightness amplitude of 0.07magnitude(U=2-).[9]Alternatively, it has a bimodal period solution of 28 hours, which is considered more likely by the observers, but ignored by the Asteroid Lightcurve Data Base.[3][9]
Diameter and albedo
editAccording to the survey carried out by theNEOWISEmission of NASA'sWide-field Infrared Survey Explorer,Geramtinameasures 12.687 and 14.574 kilometers in diameter and its surface has analbedoof 0.251 and 0.1910, respectively.[7][8]
TheCollaborative Asteroid Lightcurve Linkassumes a standard albedo of stony asteroids 0.20 and calculates a diameter of 14.22 kilometers based on anabsolute magnitudeof 11.6.[3]
Naming
editThisminor planetwas named by Swedish astronomer Bror Ansgar Asplind (1890–1954) after his sister. The name "Geramtina" is a constructed name. Bror Asplind computed the orbits of several discoveries made at Uccle Observatory in preparation of the6th IAU General Assemblyin Stockholm in 1938. The official naming citation was mentioned inThe Names of the Minor PlanetsbyPaul Hergetin 1955 (H 129).[2]
References
edit- ^abcdef"JPL Small-Body Database Browser: 1433 Geramtina (1937 UC)".Jet Propulsion Laboratory(2017-10-01 last obs.).Retrieved26 October2017.
- ^abSchmadel, Lutz D. (2007). "(1433) Geramtina".Dictionary of Minor Planet Names – (1433) Geramtina.Springer Berlin Heidelberg.p. 115.doi:10.1007/978-3-540-29925-7_1434.ISBN978-3-540-00238-3.
- ^abcdefg"LCDB Data for (1433) Geramtina".Asteroid Lightcurve Database (LCDB).Retrieved26 October2017.
- ^abcdRoberts, V. R.; Gaffey, Michael J.; Fieber-Beyer, Sherry K. (March 2013)."Mineralogical Assessment of two Gefion Family Asteroids: 1433 Geramtina and 4182 Mount Locke"(PDF).44th Lunar and Planetary Science Conference.p. 2713.Bibcode:2013LPI....44.2713R.Retrieved26 October2017.
- ^ab"Asteroid 1433 Geramtina – Proper Elements".AstDyS-2, Asteroids – Dynamic Site.Retrieved29 October2019.
- ^ab"Small Bodies Data Ferret".Nesvorny HCM Asteroid Families V3.0.Archived fromthe originalon 2 August 2017.Retrieved26 October2017.
- ^abcdMasiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012)."Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids".The Astrophysical Journal Letters.759(1): 5.arXiv:1209.5794.Bibcode:2012ApJ...759L...8M.doi:10.1088/2041-8205/759/1/L8.S2CID46350317.Retrieved26 October2017.
- ^abcdMainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results".The Astrophysical Journal.741(2): 25.arXiv:1109.6407.Bibcode:2011ApJ...741...90M.doi:10.1088/0004-637X/741/2/90.S2CID118700974.
- ^abcJohnson, Thomas; Pech, Katherin; van Schilfgaarde, Ryan; Chase, Matt; Burns, M. Shane (October 2008)."Lightcurve Analysis of 102 Miriam, 1433 Geramtina, and 2648 Owa".The Minor Planet Bulletin.35(4): 151–152.Bibcode:2008MPBu...35..151J.ISSN1052-8091.Retrieved26 October2017.
- ^abcVeres, 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.arXiv:1506.00762.Bibcode:2015Icar..261...34V.doi:10.1016/j.icarus.2015.08.007.S2CID53493339.Retrieved26 October2017.
- ^ab"1433 Geramtina (1937 UC)".Minor Planet Center.Retrieved26 October2017.
External links
edit- Asteroid Lightcurve Database (LCDB),query form (infoArchived16 December 2017 at theWayback Machine)
- Dictionary of Minor Planet Names,Google books
- Asteroids and comets rotation curves, CdR– Observatoire de Genève, Raoul Behrend
- Discovery Circumstances: Numbered Minor Planets (1)-(5000)– Minor Planet Center
- 1433 GeramtinaatAstDyS-2, Asteroids—Dynamic Site
- 1433 Geramtinaat theJPL Small-Body Database
