A three-dimensional model of 808 Merxia based on its light curve
|Discovered by||Luigi Carnera|
|Discovery site||Heidelberg Observatory|
|Discovery date||11 October 1901|
|MPC designation||(808) Merxia|
|main belt, merxia family|
|Epoch 31 July 2016 (JD 2457600.5)|
|Uncertainty parameter 0|
|Observation arc||114.45 yr (41803 d)|
|Aphelion||3.0921 AU (462.57 Gm)|
|Perihelion||2.3990 AU (358.89 Gm)|
|2.7456 AU (410.74 Gm)|
|4.55 yr (1661.7 d)|
|0° 12m 59.94s / day|
|Earth MOID||1.41983 AU (212.404 Gm)|
|Jupiter MOID||2.09197 AU (312.954 Gm)|
|Jupiter Tisserand parameter||3.331|
|30.631 h (1.2763 d)|
The spectrum of this object indicates that it is an S-type asteroid with both low and high calcium forms of pyroxene on the surface, along with less than 20% olivine. The high-calcium form of pyroxene forms 40% or more of the total pyroxene present, indicating a history of igneous rock deposits. This suggests that the asteroid underwent differentiation by melting, creating a surface of basalt rock.
808 Merxia is the namesake of the Merxia family of asteroids that share similar orbital elements and physical properties. The members of this family, including 808 Merxia, most likely formed from the breakup of a basalt object, which in turn was spawned from a larger parent body that had previously undergone igneous differentiation. Other members of this family include 1662 Hoffmann, 2042 Sitarski, 2504 Gaviola, and 3363 Bowen.
- "JPL Small-Body Database Browser: 808 Merxia". Jet Propulsion Laboratory. Retrieved 4 May 2016.
- Sunshine, Jessica M.; et al. (August 2004), "High-calcium pyroxene as an indicator of igneous differentiation in asteroids and meteorites", Meteoritics & Planetary Science, 39 (8), pp. 1343–1357, Bibcode:2004M&PS...39.1343S, doi:10.1111/j.1945-5100.2004.tb00950.x.
- Lightcurve plot of (808) Merxia, Antelope Hills Observatory
- 808 Merxia at the JPL Small-Body Database
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