{'fraction_non_alphanumeric': 0.01832460732984293, 'fraction_numerical': 0.0017452006980802793, 'mean_word_length': 5.517045454545454, 'pattern_counts': {'":': 0, '<': 0, '<?xml version=': 0, '>': 0, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 0, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
The Use of Auger Spectroscopy for the Elemental Analysis of Presolar Silicate Grains

Presolar silicate grains, formed in the outflows of evolved stars and in the ejecta of stellar explosions (supernovae), survived the formation of the solar system and are found in low abundances in primitive extraterrestrial materials. They are recognized by their isotopic signatures, which differ substantially from those observed in other solar system materials. These grains can be studied in the laboratory to gain a better understanding of stellar evolution and nucleosynthesis of the elements. They also provide information about conditions in the stellar sources in which they formed and the environments they have traversed subsequent to formation, including the interstellar medium (ISM), the early solar nebula and the parent bodies of the meteorites in which they are found. The isotopic composition of a presolar grain provides information about its stellar origin [1], but additional elemental and/or mineralogical information can constrain the conditions under which a grain condensed, and is necessary for comparison with astronomical data [2].