一个富钙铝包裹体中~ 7 Be同位素记录的来源
On the origin of 7Be isotopic records in a Calcium, Aluminium, -rich inclusion
摘要：
太阳系形成和早期演化研究中的一个主要问题是识别现已灭绝的短寿命核素的来源，并确定我们太阳系的从头算同位素组成（参考文献1）。一种寿命很短的现已灭绝的放射性核素10 Be，是由碳和氧的火花反应产生的，这一假说导致了早期太阳系辐射增强的假说（参考文献2-8）。最近有人提出了另一种方案，即在低质量恒星（11.8 Msun）的核心坍缩超新星中通过中微子过程产生10 Be（t1/2 = 138.6 +-01.6万年（参考文献9）），这可以解释在早期太阳系中观测到的10 Be丰度。在这里，我们报告了解决过剩的7 Li/6Li高达~ 21.5%的B1型钙，铝丰富的夹杂物（CAI）从Efremovka陨石与9 Be/6Li，暗示在原位衰变的7 Be。7 Be的特征半衰期为53.12+- 0.07天（参考文献11），它在原地衰变为7 Li，需要在ESS中进行多次增强辐照。7 Be的短半衰期限制了太阳高能粒子与星云气体和固体相互作用产生的7 Be，并限制了CAIs的谱系和年代。在太阳前主序阶段的I类或II类终相期间，太阳组成的CAI的前体固体/气体被超级耀斑（Lx=10 exp（32）erg/sec）照射，有力地解释了CAI中的同位素性质、独特的岩相特征和扩散率约束。
英文摘要：
A prime question in the formation and early evolution of the Solar system studies is to discern the source(s) of short-lived now extinct nuclides and to determine the ab-initio isotopic composition of our Solar System (ref. 1). The proposed genesis of a short-lived now extinct radionuclide,10Be, by spallation reactions of carbon and oxygen led to the hypothesis of enhanced irradiation in the early Solar system (ref. 2-8). An alternative scenario of production of 10Be (t1/2 =1.386 +- 0.016 million years (ref.9)) by neutrino process in a low mass star (11.8Msun) core collapse supernova has been recently suggested (ref. 10) that can explain the observed abundance of 10Be in the early Solar System. Here, we report well resolved excesses in 7Li/6Li of up to ~21.5 percent in a Type B1 Ca,-Al rich inclusion (CAI) from the Efremovka meteorite that correlate with 9Be/6Li, suggestive of in situ decay of 7Be. The in situ decay of 7Be, with characteristic half-life of 53.12+- 0.07 days (ref. 11) to 7Li, entails multiple episodes of enhanced irradiation in the ESS. The short half-life of 7Be limits its production by interaction of Solar energetic particles with the nebular gas and solids and provides constraints on genealogy and chronology of CAIs. Irradiation of precursor solids/gas of CAIs of Solar composition by a superflare (Lx=10 exp(32) erg/sec) during the terminal phase of class I or II of pre-main sequence stages of the Sun cogently explains the isotopic properties, distinctive petrographic features, and diffusivity constraints in the CAI.
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