The composition of the Trojan asteroids
The composition of the Trojan asteroids
复制标题
特洛伊小行星的组成
作者：
J. Gradie;J. Veverka
物理学研究表明，大多数小行星表面覆盖着低视反射率（pv = 0.04）的物质，这些物质在0.4到1.1微米之间具有平坦的、几乎没有特征的反射光谱（参考文献1）。这一大类天体，即C类小行星，从小行星带的内部区域到外部区域，小行星所占比例逐渐增大，这一趋势被解释为原始太阳星云中的有效凝结温度随着与原太阳2距离的增加而降低的证据。我们建议在这里，非常低的反射率和红色光谱的一些特洛伊小行星可以解释的存在下，干酪根样的有机化合物。含有这些类型的碳质物质的物质，而不是那些在更熟悉的碳质球粒陨石基质中发现的物质，可能是外太阳系的主要岩石冷凝物，因此可能是彗星核的典型岩石成分。
Physical studies have shown that most asteroids are covered with material of low visual albedo (pv∼0.04) having flat, nearly featureless reflection spectra between 0.4 and 1.1 µm (ref. 1). This large class of objects, the C asteroids, accounts for a progressively larger fraction of minor planets as one goes from the inner to the outer regions of the asteroid belt, a trend which has been interpreted as evidence of a decrease in effective condensation temperature in the original solar nebula with increasing distance from the proto-Sun2. We suggest here that the very low albedos and red spectra of some Trojan asteroids can be explained by the presence of kerogen-like organic compounds. Materials containing these types of carbonaceous substances, rather than those found in the more familiar carbonaceous chondrite matrix, may have been the primary rocky condensate in the outer Solar System and may therefore be typical of the rocky component of comet nuclei.