主带中的玄武岩物质：两个（或多个）母体的故事？
Basaltic material in the main belt: a tale of two (or more) parent bodies?
摘要：
主带中的大多数玄武质天体都与已知最大的差异化小行星灶神星动态相连。其他的，由于它们目前的轨道参数，不能很容易地动态链接到灶神星。对于所有位于2.5天文单位以外的玄武质小行星来说，这一点尤其正确，那里与木星的平均运动共振为3：1。为了调查中部和外部主带（MOV）中是否存在其他V型小行星，我们开始了一项观测活动，在可见光范围内对MOV候选者进行光谱表征。我们在2015年至2016年期间观察了来自TNG和ESO-NTT的18个玄武岩候选者。我们使用我们最近的统计分析中采用的相同方法推导出光谱参数，并将我们的数据与轨道参数进行比较，以寻找主带中可能的MOV集群，这是一个新的玄武岩家族的症状。我们的分析似乎指出，MOV显示不同的光谱参数相对于其他玄武岩主体带，这可以解释不同的矿物比灶神星;此外，其中一些属于Eos家庭，这表明另一个玄武岩祖先的可能性。这可能会对早期太阳系的温度梯度以及我们目前对分化过程的理解产生强烈的影响。
英文摘要：
The majority of basaltic objects in the main belt are dynamically connected to Vesta, the largest differentiated asteroid known. Others, due to their current orbital parameters, cannot be easily dynamically linked to Vesta. This is particularly true for all the basaltic asteroids located beyond 2.5 au, where lies the 3:1 mean motion resonance with Jupiter. In order to investigate the presence of other V-type asteroids in the middle and outer main belt (MOVs) we started an observational campaign to spectroscopically characterize in the visible range MOV candidates. We observed 18 basaltic candidates from TNG and ESO - NTT between 2015 and 2016. We derived spectral parameters using the same approach adopted in our recent statistical analysis and we compared our data with orbital parameters to look for possible clusters of MOVs in the main belt, symptomatic for a new basaltic family. Our analysis seemed to point out that MOVs show different spectral parameters respect to other basaltic bodies in the main belt, which could account for a diverse mineralogy than Vesta; moreover, some of them belong to the Eos family, suggesting the possibility of another basaltic progenitor. This could have strong repercussions on the temperature gradient present in the early Solar System, and on our current understanding of differentiation processes.
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