Most C-complex asteroids have albedo values less than 0.1, but there are some high-albedo (bright) C-complex asteroids with albedo values exceeding 0.1. To reveal the nature and origin of bright C-complex asteroids, we conducted spectroscopic observations of the asteroids in visible and near-infrared wavelength regions. As a result, the bright B-, C-, and Ch-type (Bus) asteroids, which are subclasses of the Bus C-complex, are classified as DeMeo C-type asteroids with concave curvature, B-, Xn-, and K-type asteroids. Analogue meteorites and material (CV/CK chondrites, enstatite chondrites/achondrites, and salts) associated with these spectral types of asteroids are thought to be composed of minerals and material exposed to high temperatures. A comparison of the results obtained in this study with the SDSS photometric data suggests that salts may have occurred in the parent bodies of 24 Themis and 10 Hygiea, as well as 2 Pallas. The bright C-complex asteroids in other C-complex families were likely caused by impact heating. Bright C-complex asteroids that do not belong to any families are likely to be impact metamorphosed carbonaceous chondrites, CV/CK chondrites, or enstatite chondrites/achondrites.

中文翻译：

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明亮的C复合小行星的性质

大多数 C 复合小行星的反照率值小于 0.1，但也有一些高反照率（明亮）C 复合小行星的反照率值超过 0.1。为了揭示明亮的 C 复合小行星的性质和起源，我们在可见光和近红外波长区域对小行星进行了光谱观测。因此，明亮的 B-、C-和 Ch-型 (Bus) 小行星是 Bus C-complex 的子类，被归类为具有凹曲率、B-、Xn-和K型小行星。与这些光谱类型的小行星相关的类似陨石和材料（CV/CK 球粒陨石、顽火球粒陨石/无球粒陨石和盐）被认为是由暴露于高温的矿物质和材料组成。将本研究中获得的结果与 SDSS 光度数据进行比较表明，24 Themis 和 10 Hygiea 以及 2 Pallas 的母体中可能出现了盐分。其他 C-complex 家族中明亮的 C-complex 小行星很可能是由撞击加热引起的。不属于任何家族的明亮 C 复合小行星很可能是撞击变质的碳质球粒陨石、CV/CK 球粒陨石或顽火石球粒陨石/无球粒陨石。