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The (dynamical, astrometrical) method for computing the mass is based on the analysis of orbital perturbations during close encounters between the massive asteroid (perturber) and (several) smaller minor planets (test asteroids / bodies).  

Object Test asteroid(s) Mass (Solar Mass | kg) Reference Note
(11) Parthenope (089149) 2001 UD34 (2.5 ± 0.5) E-12 | (5.0 ± 1.0) E18 Kretlow 2015 2
(16) Psyche (13206) 1997 GC22 (2.5 ± 0.2) E-11 | (5.0 ± 0.4) E19 Kretlow 2005  
(29) Amphitrite (987) Wallia, (6904) McGill (5.9 ± 0.6) E-12 | (1.2 ± 0.2) E19 Kretlow 2005  
(29) Amphitrite (6904) McGill (7.4 ± 0.5) E-12 | (1.5 ± 0.1) E19 Kretlow 2013 1
(76) Freia (83565) 2001 SS213 (4.7 ± 1.4) E-12 | (9.4 ± 2.8) E18 Kretlow 2015 2
(121) Hermione (278) Paulina, (5750) Kandatai (3.3 ± 1.1) E-12 | (6.6 ± 2.2) E18 Kretlow 2005  
(121) Hermione (278) Paulina, (5750) Kandatai (2.4 ± 0.4) E-12 | (4.8 ± 0.8) E18 Kretlow 2014 1
(476) Hedwig (187901) 2000 SB317 (6.2 ± 2.7) E-13 | (1.2 ± 0.5) E18 Kretlow 2014  
(804) Hispania (1002) Olbersia (2.2 ± 0.9) E-12 | (4.4 ± 1.8) E18 Kretlow 2005  

1: Recalculation using more observations and extended arc span.
2: (Re)calculation with observation debiasing (Chesley et al. (2010)).

Last edited: September 17, 2020, 14:17

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