微隕石
微隕石 是在地球 表面收集到來自地球之外的小天體,大小範圍從50微米至2毫米。微隕石是進入地球大氣層而倖存下來的流星塵 。它們從大小、組成都與隕石 不同,並且數量、種類更為豐富,其中也包括較小的星際塵埃 的顆粒(IDPs)[ 1] ,是宇宙塵的一部分。流星體以高速(至少11Km/s)進入地球的大氣層,經過加熱和大氣的磨擦和壓縮。目前已經在地球上蒐集到,來自地球之外個別微隕石的質量在10−9 和 10−4 公克之間[ 2] 。 弗雷德·惠普爾 首先創造了微隕石這個名稱來描述落在地球上如灰塵大小的天體[ 3] 。有時,隕石和微隕石在進入地球大氣層時是被看見的流星 ,但不論它們能否墜落到地球表面被找到,隕石和微隕石依然都存在著。
介紹
微隕石(MM)的紋理會因為原始結構在進入大氣層時的加熱過程,隨著它們的初始速度和進入角度的函數而改變。它們的範圍從保留原始礦物學 未熔解的顆粒(圖1a、b)到部分熔解的微粒(圖1c、d)和完全熔解成圓形的宇宙球體(圖1e、f、g、h),其中一些經過汽化階段已經失去了很大部分的質量(圖1i)。分類是依據它們的組成和經歷的溫度[ 4] [ 5] 。
圖1.不同的微隕石截面分類:a)未溶解的微細顆粒;b)未熔解的粗糙顆粒;c) Scoriaceous; d) Relict-grain Bearing; e) Porphyritic; f) Barred olivine; g) Cryptocrystalline; h) Glass; i) CAT; j) G-type; k) I-type; and l) Single mineral. 除了G和I型的,所有的都富含矽酸鹽,稱為石質微隕石。尺度棒是50µm。
圖2.石質宇宙球體的光學顯微鏡影像。
由顯微分析顯示微隕石確實是來自地球之外:
估計每年有30,000 ± 20,000 噸 (t/年)[ 2] 的宇宙塵進入上層大氣層,但估計只有少於10%(2700 ± 1400t/yr)的能夠成為顆粒降落到地球表面。因此,微隕石的沉積量大約比隕石的量高出50倍,而隕石的量是50t/yr[ 13] ,並且每年有為數龐大的微粒(~1017 > 10 µ m)進入大氣層,這表明收集的微隕石塵埃微粒來自太陽系的所有天體,包括小行星、彗星,和來自我們的月球和火星的片段碎屑。大微隕石的收集能提供的訊息包括大小、組成、大氣的熱效應和在地球增生的物質類型,對個別微隕石的詳細研究可以洞察它們的起源、原始的碳 、胺基酸 和包含的前太陽顆粒[ 14] 。
收集場所
微隕石的收集來自深海沉積物 、沉積岩、和極地沉積物;目前的收集主要來自極地的冰和雪。由於微隕石在地球表面的低濃度,必須在能夠濃縮這些材料的環境中尋找它們。
海洋沉積物
在1873年至1876年,英國皇家海軍挑戰者號 首先從深海收集熔化的微隕石(宇宙球體)。在1891年,Murray和Renard發現"兩種微隕石族群:第一種是黑色的磁球體,有或沒有金屬的核心;第二種,有著結晶的結構,棕色的類似隕石球粒的球體"[ 15] 。在1883年,他們建議這些球體是來自地球之外,因為他們發現這些顆粒遠不同於地球上其它粒子,它們不像當時從熔爐中山產出來的磁球,而且它們的鎳-鐵 (Fe-Ni)金屬核心也不像在火成岩中發現的金屬鐵。這些球體在緩慢累積的沉積物中有最大的豐度,特別是沉積在碳酸鹽補償深度之下的紅黏土,這些發現支持起源於隕石[ 16] 。除了這些球體和鐵-鎳金屬核心,一些大於300µm的球體核心包含鉑族元素[ 17] 。
自從HMS Challenger 的第一次收集之後,宇宙球體已經使用岩心、砂心、蛤殼狀挖泥器、磁雪撬等從海洋沉積物中反覆的收集到[ 18] 。其中的磁雪橇,被稱為"宇宙淤泥的耙子",從太平洋 海床頂部的紅黏土收集到數以千計的10cm宇宙球體[ 19] 。
陸地沉積物
相關條目
參考資料
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外部連結