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(145451) 2005 RM43, provisionally known as 2005 RM43, is a trans-Neptunian object that resides in the scattered disc region beyond the Kuiper belt. It was discovered on 9 September 2005, by American astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica at Apache Point Observatory in Sunspot, New Mexico. It measures approximately 500-600 kilometers in diameter.[2][8]

(145451) 2005 RM43
Hubble Space Telescope image of 2005 RN43 taken in 2008
Discovery[1]
Discovered byA. C. Becker
A. W. Puckett
J. M. Kubica
Discovery siteApache Point Obs.
Discovery date9 September 2005
Designations
MPC designation
(145451) 2005 RM43
Minor planet category
SDO[2]
Orbital characteristics[1]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 2
Observation arc14983 days (41.02 yr)
Earliest precovery date17 November 1976
Aphelion144.140 AU (21.5630 Tm)
Perihelion35.079 AU (5.2477 Tm)
Semi-major axis
89.610 AU (13.4055 Tm)
Eccentricity0.60854
Orbital period (sidereal)
848.28 yr (309834 d)
Mean anomaly
6.19°
Mean motion
0° 0m 4.183s / day
Inclination28.819°
Longitude of ascending node
84.61°
Argument of perihelion
318.10°
Physical characteristics
Mean diameter
≈644 km (occultation)[3]
524+96
−103 km[4]
458 km (lower limit)[5]
Mean density
>0.56 g/cm3[2]
Synodic rotation period
6.71 h (0.280 d)
Geometric albedo
0.102[4]
Spectral type
V–R=0.33±0.02 (neutral)[4]
B0−V0=0.590[6]
B-R=0.99[2]
Apparent magnitude
20.4[7]
Absolute magnitude (H)
4.52±0.01[4]
4.4[1] · 4.8[8]

    Description


    Precovery image of 2005 RM43 taken by the Siding Spring Observatory in 1976[9]
    Precovery image of 2005 RM43 taken by the Siding Spring Observatory in 1976[9]

    2005 RM43 is considered likely to be a dwarf planet by both Brown and Tancredi.[8][10] Based on an absolute magnitude of 4.4, the body's diameter could be anywhere in the range of 350 to 800 kilometres (km), depending on its albedo, the surface reflectivity of the object.[11] Johnston's Archive gives an estimate of 584 km, based on an assumed albedo of 0.09.[2] Brown estimates a diameter of 524 km, based on an absolute magnitude of 4.8 and an assumed albedo of 0.08. A stellar occultation by 2005 RM43 in December 2018 gave a minimum diameter of 458 km.[5]

    In 2018, two stellar occultations by 2005 RM43 were observed on 3 February and 24 December.[3] Observations of the February occultation yielded a single chord length of 456 km (283 mi).[12] Observations of the December occultation yielded two positive chords, which suggest an approximate diameter of 644 km (400 mi) for 2005 RM43.[13]

    It has been observed 303 times over 17 oppositions, with precovery images dating back to 1976.[1][14] The orbit is well determined with an uncertainty parameter of 2.[1]


    See also



    References


    1. "JPL Small-Body Database Browser: 145451 (2005 RM43)" (2017-11-25 last obs). Retrieved 2 February 2019.
    2. Wm. Robert Johnston. "List of Known Trans-Neptunian Objects". Johnston's Archive. Archived from the original on 2 February 2019. Retrieved 2 February 2019.
    3. "TNO Results". ERC Lucky Star Project. Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA). Retrieved 13 July 2020.
    4. Farkas-Takács, A.; Kiss, Cs.; Vilenius, E.; Marton, G.; Müller, T. G.; Mommert, M.; et al. (28 February 2020). "TNOs are Cool! A Survey of the transneptunian Region XV. Physical characteristics of 23 resonant transneptunian and scattered disk objects". Astronomy & Astrophysics. A23: 638. arXiv:2002.12712. Bibcode:2020A&A...638A..23F. doi:10.1051/0004-6361/201936183. S2CID 216193564.
    5. Frappa, E. "2018 European Asteroidal Occultation Results". euraster.net. Retrieved 2 February 2019.
    6. David L. Rabinowitz; Bradley E. Schaefer; Martha W. Schaefer; Suzanne W. Tourtellotte (2008). "The Youthful Appearance of the 2003 EL61 Collisional Family". The Astronomical Journal. 136 (4): 1502–1509. arXiv:0804.2864. Bibcode:2008AJ....136.1502R. doi:10.1088/0004-6256/136/4/1502. S2CID 117167835.
    7. AstDyS. "(145451) 2005RM43 - Observation prediction". Department of Mathematics, University of Pisa. Retrieved 2 February 2019.
    8. Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Archived from the original on 2 February 2019. Retrieved 2 February 2019.
    9. Lowe, Andrew. "(145451) 2005 RM43 Precovery Images". andrew-lowe.ca.
    10. Tancredi, G. (2010). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Icy Bodies of the Solar System: Proceedings IAU Symposium No. 263, 2009. 263: 173. Bibcode:2010IAUS..263..173T. doi:10.1017/S1743921310001717.
    11. Bruton, D. "Conversion of Absolute Magnitude to Diameter for Minor Planets". Stephen F. Austin State University.
    12. "Occultation by 2005 RM43 in 03 02 2018" (PDF). ERC Lucky Star Project. Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA). 3 February 2018. Retrieved 13 July 2020.
    13. "Occultation by 2005 RM43 in 23 DEC 2018" (PDF). ERC Lucky Star Project. Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA). 24 December 2018. Retrieved 13 July 2020.
    14. "(145451) = 2005 RM43". Minor Planet Center. Retrieved 2 February 2019.



    На других языках

    [de] (145451) 2005 RM43

    (145451) 2005 RM43 ist ein großes transneptunisches Objekt, welches bahndynamisch als Scattered Disc Object eingestuft wird. Aufgrund seiner Größe ist der Asteroid ein Zwergplanetenkandidat.
    - [en] (145451) 2005 RM43

    [ru] (145451) 2005 RM43

    (145451) 2005 RM43 — транснептуновый объект, расположенный в зоне рассеянного диска[4] за пределами пояса Койпера. Обнаружен 9 сентября 2005 года группой учёных в обсерватории солнечных пятен Апаче-Пойнт, Нью-Мексико.


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