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<p>Three molecules, SiCSi, SiC<sub>2</sub>, and SiC are considered to play significant role in the formation of SiC-dust around the carbon-stars. Precise collisional rate coefficients for transitions among 78&#xa0;rotational levels in SiCSi due to collisions with para‑H<sub>2</sub> (<i>j</i> = 0), for kinetic temperatures up to 50 K, are now available. Using these collisional rate coefficients, we have investigated the MASER and dasar lines of SiCSi, by solving a&#xa0;set of 78&#xa0;statistical equilibrium equations coupled with 235 radiative transfer equations (Sobolev analysis). Six, out of 235 radiative transitions have shown MASER action, whereas 13&#xa0;lines are found as dasar lines. The results are compared with those obtained by using the scaled values of the collisional rate coefficients. Significant differences have been found between the two sets of results. It highlights the importance of collisional rate coefficients.</p>

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MASER and dasar lines of SiCSi using the large number of collisional rate coefficients in CS approximation

  • 期刊论文

  • 发表日期：

    2026年7月1日

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  • S. Chandra

摘要

Three molecules, SiCSi, SiC2, and SiC are considered to play significant role in the formation of SiC-dust around the carbon-stars. Precise collisional rate coefficients for transitions among 78 rotational levels in SiCSi due to collisions with para‑H2 (j = 0), for kinetic temperatures up to 50 K, are now available. Using these collisional rate coefficients, we have investigated the MASER and dasar lines of SiCSi, by solving a set of 78 statistical equilibrium equations coupled with 235 radiative transfer equations (Sobolev analysis). Six, out of 235 radiative transitions have shown MASER action, whereas 13 lines are found as dasar lines. The results are compared with those obtained by using the scaled values of the collisional rate coefficients. Significant differences have been found between the two sets of results. It highlights the importance of collisional rate coefficients.