Main-belt asteroid
128 Nemesis is a large 180 kmmain-belt asteroid , ofcarbonaceous composition. It rotates rather slowly, taking about 78 hours to complete one rotation.[ 3] [ 9] Nemesis is the largest member of the Nemesian asteroid family bearing its name. It was discovered byJ. C. Watson on 25 November 1872,[ 3] and named afterNemesis , the goddess of retribution inGreek mythology .
Diagram of Nemesis's orbit This object is orbiting theSun with aperiod of 4.56 years and aneccentricity (ovalness) of 0.13. Theorbital plane isinclined by 6.2° to theplane of the ecliptic . It is categorized as aC-type asteroid ,[ 10] indicating a primitivecarbonaceous composition. Based onIRAS data Nemesis is about 188 km in diameter and is around the 33rd largestmain-belt asteroid,[ 11] whileWISE measurements yield a size of ~163 km.[ 7] The 77.81‑hour[ 12] rotation period is the second longest for an asteroid more than 150 km in diameter.[ 13]
Between 2005 and 2021, Nemesis has been observed tooccult eight stars.
^a b "128 Nemesis" .Minor Planet Center . Retrieved14 September 2018 .^ "Nemesis" .Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription orparticipating institution membership required.) ^a b c d e f g h i "JPL Small-Body Database Browser: 128 Nemesis" (2017-10-31 last obs.).Jet Propulsion Laboratory . Retrieved14 September 2018 .^ Hornum (1993)Nemesis, the Roman state and the games ^ Peery (1963)Studies in the Renaissance , vol. 10 ^a b c d e P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis.Astronomy & Astrophysics 54, A56 ^a b Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos".The Astrophysical Journal .791 (2): 11.arXiv :1406.6645 .Bibcode :2014ApJ...791..121M .doi :10.1088/0004-637X/791/2/121 .S2CID 119293330 . ^a b c Carry, B. (December 2012), "Density of asteroids",Planetary and Space Science ,73 (1):98– 118,arXiv :1203.4336 ,Bibcode :2012P&SS...73...98C ,doi :10.1016/j.pss.2012.03.009 ,S2CID 119226456 . See Table 1.^a b Scaltriti, F.; Zappala, V.; Schober, H. J. (January 1979), "The rotations of 128 Nemesis and 393 Lampetia - The longest known periods to date",Icarus ,37 (1):133– 141,Bibcode :1979Icar...37..133S ,doi :10.1016/0019-1035(79)90121-0 . ^ DeMeo, Francesca E.; et al. (July 2009),"An extension of the Bus asteroid taxonomy into the near-infrared" (PDF) ,Icarus ,202 (1):160– 180,Bibcode :2009Icar..202..160D ,doi :10.1016/j.icarus.2009.02.005 , archived fromthe original (PDF) on 17 March 2014, retrieved8 April 2013 . See appendix A.^ "JPL Small-Body Database Search Engine: asteroids and orbital class (IMB or MBA or OMB) and diameter > 188.1 (km)" . JPL's Solar System Dynamics Group. Retrieved17 April 2012 .^ Pilcher, Frederick (July 2015), "New Photometric Observations of 128 Nemisis [sic ], 249 Ilse, and 279 Thule",The Minor Planet Bulletin ,42 (3): 190−192,Bibcode :2015MPBu...42..190P . ^ "JPL Small-Body Database Search Engine: diameter > 150 (km) and rot_per > 24 (h)" .JPL Solar System Dynamics . Retrieved6 June 2015 .