Silicaceous Type

As a solar system forms, a population of asteroids might form close enough to the young and active sun so that they become differentiated bodies.  These Silicaceous asteroids are heated sufficiently by the electromagnetic currents so that minerals will become separated, much like the process experienced by larger worlds due to their internal heating.  As the sun begins to stabilize and cool down, what is left is a rocky body that typically has an olivine crust surrounding a nickel-iron alloy core.

Silicaceous asteroids are not that highly prized as sources of mineral wealth, although in some cases if the core is exposed via some ancient impact, then mining operations could be considered.  Most of these bodies are thus ignored, save as building material, or the occasional use as a manned or unmanned outpost.


The cratered surfaces of Silicaceous asteroids are a common sight in nearly any solar system.

Quick Facts

Classification Notes:  Before the advent of the PCL, these bodies were typically known as S-class, or stony-iron asteroids.

Asteroids of Note:  In the Sol System, Eros was the first Silicaceous asteroid to be studied in depth, as well as to be landed upon, both feats completed by the same unmanned probe.  In the 12 Ophiuchi System, the asteroid designated PC-393, 1.3 kilometers in diameter, grazed the atmosphere of Yellowstone, and was actually captured as a temporary moon for three local years before being ejected from orbit and sent into the sun by the planet's gravity.

 

 

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ArcBuilder Universe concept John M. and Margo L. Dollan 2002-2004
This Page first uploaded May 1, 2004
Most recent update for this page May 1, 2004