This shows you the differences between two versions of the page.
Both sides previous revision Previous revision | |
molecules:ism:hc7n [2020/08/12 12:36] – mueller | molecules:ism:hc7n [2020/08/12 12:42] (current) – mueller |
---|
**[[https://doi.org/10.1051/0004-6361/202038571|Detection of Vibrationally Excited HC<sub>7</sub>N and HC<sub>9</sub>N in IRC +10216]]**\\ | **[[https://doi.org/10.1051/0004-6361/202038571|Detection of Vibrationally Excited HC<sub>7</sub>N and HC<sub>9</sub>N in IRC +10216]]**\\ |
//Astron. Astrophys.// **640**, Art. No. L13 (2020).\\ | //Astron. Astrophys.// **640**, Art. No. L13 (2020).\\ |
The authors carried out an unbiased molecular with the Yebes 40 m dish between 31 and 50 GHz toward the circumstellar envelope of the famous C-rich AGB star CW Leonis. Numerous transitions of HC<sub>7</sub>N in its lowest excited state //v//<sub>15</sub> = 1 were detected despite a rotational temperature of around 25 K. The derived HC<sub>5</sub>N to HC<sub>7</sub>N ratio is extremely low, roughly 2.4. The derived HC<sub>7</sub>N to HC<sub>9</sub>N ratio is still very low, roughly 7.7.\\ | The authors carried out an unbiased molecular line survey with the Yebes 40 m dish between 31 and 50 GHz toward the circumstellar envelope of the famous C-rich AGB star CW Leonis. Numerous transitions of HC<sub>7</sub>N in its lowest excited state //v//<sub>15</sub> = 1 were detected despite a rotational temperature of around 25 K. The derived HC<sub>5</sub>N to HC<sub>7</sub>N ratio is extremely low, roughly 2.4. The derived HC<sub>7</sub>N to HC<sub>9</sub>N ratio is still very low, roughly 7.7.\\ |
| |
| |