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사회과학
자연과학
공학
의약학
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예술체육학
복합학
DBpia AI
AI 에이전트
AI 아이디어
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Citeasy
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지원사업
학술연구/단체지원/교육 등 연구자 활동을 지속하도록 DBpia가 지원하고 있어요.
커뮤니티
연구자들이 자신의 연구와 전문성을 널리 알리고, 새로운 협력의 기회를 만들 수 있는 네트워킹 공간이에요.
초록·키워드
Context. Interstellar molecules are excellent tools for studying the physical and chemical environments of massive star-forming regions. In particular, the vibrationally excited HC 3 N (HC 3 N*) lines are the key tracers for probing hot cores environments. Aims. We present the Atacama Large Millimeter/submillimeter Array (ALMA) 3 mm observations of HC 3 N* lines in 60 hot cores and investigate how the physical conditions affect the excitation of HC 3 N* transitions. Methods. We used the XCLASS for line identification. Under the assumption of local thermodynamic equilibrium, we derived the rotation temperature and column density of HC 3 N* transitions in hot cores. Additionally, we calculated the H 2 column density and number density, along with the abundance of HC 3 N* relative to H 2 , to enable a comparison of the physical properties of hot cores with different numbers of HC 3 N* states. Results. We have detected HC 3 N* lines in 52 hot cores, 29 of which show more than one vibrationally excited state. Hot cores with higher gas temperatures have more detections of these vibrationally excited lines. The excitation of HC 3 N* requires dense environments, and its spatial distribution is affected by the presence of UC H II regions. The observed column density of HC 3 N* contributes to the number of HC 3 N* states in hot-core environments. Conclusions. After analyzing the various factors influencing HC 3 N* excitation in hot cores, we conclude that the excitation of HC 3 N* is mainly driven by mid-IR pumping, while collisional excitation is ineffective.
인공지능 문자 인식 모델을 통해 추출된 텍스트로, 일부 오타나 오류가 포함될 수 있으나 지속적으로 개선 중입니다.
오류를 발견하셨다면 해당 부분을 드래그한 후 ' 를 통해 신고해주세요.
오류를 발견하셨다면 해당 부분을 드래그한 후 ' 를 통해 신고해주세요.
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