molecules:ism:hc7n

Differences

This shows you the differences between two versions of the page.

Link to this comparison view

Both sides previous revision Previous revision
Next revision		 Previous revision
Last revisionBoth sides next revision
molecules:ism:hc7n [2019/04/25 13:39] – muellermolecules:ism:hc7n [2020/08/12 12:36] – mueller
Line 2: Line 2:
  
 H. W. Kroto, C. Kirby, D. R. M. Walton, L. W. Avery, N. W. Broten, J. M. MacLeod, and T. Oka,\\ H. W. Kroto, C. Kirby, D. R. M. Walton, L. W. Avery, N. W. Broten, J. M. MacLeod, and T. Oka,\\
-**[[http://cdsads.u-strasbg.fr/abs/1978ApJ...219L.133K|The Detection of Cyanohexatriyne, H(C≡C)<sub>3</sub>CN, in Heile's Cloud 2]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1978ApJ...219L.133K|The Detection of Cyanohexatriyne, H(C≡C)<sub>3</sub>CN, in Heile's Cloud 2]]**\\
 //Astrophys. J.// **219**, L133–L137 (1978)\\ //Astrophys. J.// **219**, L133–L137 (1978)\\
 reported the first detection of this cyanopolyyne in two transitions (//J// = 9 – 8 and 21 – 20 near 10.15 and 23.69 GHz, respectively) in Heile's Cloud 2 employing the 46 m radio telecope of the Algonquin Radio Observatory. reported the first detection of this cyanopolyyne in two transitions (//J// = 9 – 8 and 21 – 20 near 10.15 and 23.69 GHz, respectively) in Heile's Cloud 2 employing the 46 m radio telecope of the Algonquin Radio Observatory.
Line 8: Line 8:
 More recently, the Effelsberg 100 m telecope was used to study the circumstellar shell of the famous carbon star CW Leo:\\ More recently, the Effelsberg 100 m telecope was used to study the circumstellar shell of the famous carbon star CW Leo:\\
 G. Winnewisser and C. M. Walmsley,\\ G. Winnewisser and C. M. Walmsley,\\
-**[[http://cdsads.u-strasbg.fr/abs/1978A%26A....70L..37W|The Detection of HC<sub>5</sub>N and HC<sub>7</sub>N in IRC +10216]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1978A%26A....70L..37W|The Detection of HC<sub>5</sub>N and HC<sub>7</sub>N in IRC +10216]]**\\
 //Astron. Astrophys.// **70**, L37–L39 (1978).\\ //Astron. Astrophys.// **70**, L37–L39 (1978).\\
 The //J// = 21 – 10 transition near 23.688 GHz was detected for the larger polyyne. The //J// = 21 – 10 transition near 23.688 GHz was detected for the larger polyyne.
Line 14: Line 14:
 The molecule has also been detected with the Effelsberg 100 m telescope in the circumstellar envelope of the carbon-rich post-AGB star V1610 Cyg, which is somewhat better known as CRL 2688, by\\ The molecule has also been detected with the Effelsberg 100 m telescope in the circumstellar envelope of the carbon-rich post-AGB star V1610 Cyg, which is somewhat better known as CRL 2688, by\\
 Nguyen-Q-Rieu, D. Graham, and V. Bujarrabal,\\ Nguyen-Q-Rieu, D. Graham, and V. Bujarrabal,\\
-**[[http://cdsads.u-strasbg.fr/abs/1984A%26A...138L...5N|Ammonia and Cyanotriacetylene in the Envelopes of CRL 2688 and IRC +10216]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1984A%26A...138L...5N|Ammonia and Cyanotriacetylene in the Envelopes of CRL 2688 and IRC +10216]]**\\
 //Astron. Astrophys.// **138**, L5–L8 (1984). //Astron. Astrophys.// **138**, L5–L8 (1984).
  
Line 25: Line 25:
 **[[https://doi.org/10.1093/mnras/stx2972|Detection of HC<sub>5</sub>N and HC<sub>7</sub>N Isotopologues in TMC-1 with the Green Bank Telescope]]**\\ **[[https://doi.org/10.1093/mnras/stx2972|Detection of HC<sub>5</sub>N and HC<sub>7</sub>N Isotopologues in TMC-1 with the Green Bank Telescope]]**\\
 //Mon. Not. R. Astron. Soc.// **474**, 5068–5075 (2018); by\\ //Mon. Not. R. Astron. Soc.// **474**, 5068–5075 (2018); by\\
-A. M. Burkhardt, E. Herbst, S. V. Kalenskii, M. C. McCarthy, A. J. Remijan, and B. A. McGuire.+A. M. Burkhardt, E. Herbst, S. V. Kalenskii, M. C. McCarthy, A. J. Remijan, and B. A. McGuire.\\
  
 +J. R. Pardo, C. Bermúdez, C. Cabezas, M. Agúndez, J. D. Gallego, J. P. Fonfría, L. Velilla-Prieto, G. Quintana-Lacaci, B. Tercero, M. Guélin, and J. Cernicharo\\
 +reported on the\\
 +**[[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).\\
 +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.\\
  
----- 
  
-Contributor(s): H. S. P. Müller; 04, 2012; 01, 2018.+----
  
 +Contributor(s): H. S. P. Müller; 04, 2012; 01, 2018; 08, 2020.
  
 ---- ----
  
  
  • molecules/ism/hc7n.txt
  • Last modified: 2020/08/12 12:42
  • by mueller