molecules:ism:hc2nh

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molecules:ism:hc2nh [2019/02/25 22:38] – external edit 127.0.0.1molecules:ism:hc2nh [2019/04/26 15:38] – mueller
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 The first member of this group, not really qualifying for "poly", acetylene, HC<sub>2</sub>H, itself, was detected in absorption at Kitt Peak toward the circumstellar shell of CW Leo, aka IRC +10216. The unresolved //Q//-branch of the ν<sub>4</sub> + ν<sub>5</sub> band was detected at 4091.0 cm<sup>–1</sup> by:\\ The first member of this group, not really qualifying for "poly", acetylene, HC<sub>2</sub>H, itself, was detected in absorption at Kitt Peak toward the circumstellar shell of CW Leo, aka IRC +10216. The unresolved //Q//-branch of the ν<sub>4</sub> + ν<sub>5</sub> band was detected at 4091.0 cm<sup>–1</sup> by:\\
 S. T. Ridgway, D. N. B. Hall, R. S. Wojslaw, S. G. Kleinmann, and D. A. Weinberger,\\ S. T. Ridgway, D. N. B. Hall, R. S. Wojslaw, S. G. Kleinmann, and D. A. Weinberger,\\
-**[[http://dx.doi.org/10.1038/264345a0|Circumstellar Acetylene in the Infrared Spectrum of IRC +10<sup>o</sup>216]]**\\+**[[https://doi.org/10.1038/264345a0|Circumstellar Acetylene in the Infrared Spectrum of IRC +10<sup>o</sup>216]]**\\
 //Nature// **264**, 345–346 (1976). //Nature// **264**, 345–346 (1976).
  
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 J. Cernicharo, A. M. Heras, A. G. G. M. Tielens, J. R. Pardo, F. Herpin, M. Guélin, and L. B. F. M. Waters,\\ J. Cernicharo, A. M. Heras, A. G. G. M. Tielens, J. R. Pardo, F. Herpin, M. Guélin, and L. B. F. M. Waters,\\
-**[[http://dx.doi.org/10.1086/318871|//Infrared Space Observatory's// Discovery of C<sub>4</sub>H<sub>2</sub>, C<sub>6</sub>H<sub>2</sub>, and Benzene in CRL 618]]**\\+**[[https://doi.org/10.1086/318871|//Infrared Space Observatory's// Discovery of C<sub>4</sub>H<sub>2</sub>, C<sub>6</sub>H<sub>2</sub>, and Benzene in CRL 618]]**\\
 //Astrophys. J.// **546**, L123–L126 (2001);\\ //Astrophys. J.// **546**, L123–L126 (2001);\\
 report the detection of butadiyne, HC<sub>4</sub>H, aka diacetylene, and hexatriyne, HC<sub>6</sub>H, aka as triacetylene, employing mid-infrared absorption spectroscopy. The unresolved //Q//-branches of the cold ν<sub>8</sub> band of butadiyne along with hot bands were detected at 15.9 μm. Close by, at 16.1 μm, the //Q//-branch of ν<sub>11</sub> band of hexatriyne is seen. report the detection of butadiyne, HC<sub>4</sub>H, aka diacetylene, and hexatriyne, HC<sub>6</sub>H, aka as triacetylene, employing mid-infrared absorption spectroscopy. The unresolved //Q//-branches of the cold ν<sub>8</sub> band of butadiyne along with hot bands were detected at 15.9 μm. Close by, at 16.1 μm, the //Q//-branch of ν<sub>11</sub> band of hexatriyne is seen.
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 A separate report;\\ A separate report;\\
 J. Cernicharo, A. M. Heras, J. R. Pardo, A. G. G. M. Tielens, M. Guélin, E. Dartois, R. Neri, and L. B. F. M. Waters;\\ J. Cernicharo, A. M. Heras, J. R. Pardo, A. G. G. M. Tielens, M. Guélin, E. Dartois, R. Neri, and L. B. F. M. Waters;\\
-**[[http://dx.doi.org/10.1086/318872|Methylpolyynes and Small Hydrocarbons in CRL 618]]**\\+**[[https://doi.org/10.1086/318872|Methylpolyynes and Small Hydrocarbons in CRL 618]]**\\
 //Astrophys. J.// **546**, L127–L130 (2001);\\ //Astrophys. J.// **546**, L127–L130 (2001);\\
 identifies one combination band each for butadiyne and hexatriyne. The spectrum around 8 μm is rather complex as is the model which contains many species. Inspection of laboratory spectroscopic literature is useful. A complex feature at almost exactly 8 μm is largely attributable to the strong, unresolved //R//-branch of ν<sub>6</sub> + ν<sub>8</sub> band of butadiyne. Features at 8.08 and 8.14 μm can be attributed to the unresolved //R//- and //P//-branches of the respective strong ν<sub>8</sub> + ν<sub>11</sub> band of hexatriyne, both overlapping the //P//-branch of the butadiyne band. identifies one combination band each for butadiyne and hexatriyne. The spectrum around 8 μm is rather complex as is the model which contains many species. Inspection of laboratory spectroscopic literature is useful. A complex feature at almost exactly 8 μm is largely attributable to the strong, unresolved //R//-branch of ν<sub>6</sub> + ν<sub>8</sub> band of butadiyne. Features at 8.08 and 8.14 μm can be attributed to the unresolved //R//- and //P//-branches of the respective strong ν<sub>8</sub> + ν<sub>11</sub> band of hexatriyne, both overlapping the //P//-branch of the butadiyne band.
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 The spectral same region was also studied under high resolution by:\\ The spectral same region was also studied under high resolution by:\\
 J. P. Fonfría, J. Cernicharo, M. J. Richter, J. H. Lacy,\\ J. P. Fonfría, J. Cernicharo, M. J. Richter, J. H. Lacy,\\
-**[[http://dx.doi.org/10.1088/0004-637X/728/1/43|The Abundances of Polyacetylenes towards CRL618]]**\\+**[[https://doi.org/10.1088/0004-637X/728/1/43|The Abundances of Polyacetylenes towards CRL618]]**\\
 //Astrophys. J.// **728**, Art. No. 43 (2011),\\ //Astrophys. J.// **728**, Art. No. 43 (2011),\\
 revealing clear evidence for several hot bands associated with these rather strong combination bands.\\ revealing clear evidence for several hot bands associated with these rather strong combination bands.\\
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 Earlier, the two fundamental vibrations ν<sub>8</sub> of butadiyne at 15.9 μm and of ν<sub>11</sub> of hexatriyne at 16.1 μm, see also above, were observed toward a Nova like star by\\ Earlier, the two fundamental vibrations ν<sub>8</sub> of butadiyne at 15.9 μm and of ν<sub>11</sub> of hexatriyne at 16.1 μm, see also above, were observed toward a Nova like star by\\
 A. Evans, V. H. Tyne, J. Th. van Loon, B. Smalley, T. R. Geballe, R. D. Gehrz, C. E. Woodward, A. A. Zijlstra, E. Polomski, M. T. Rushton, S. P. S. Eyres, S. G. Starrfield, J. Krautter, and R. M. Wagner,\\ A. Evans, V. H. Tyne, J. Th. van Loon, B. Smalley, T. R. Geballe, R. D. Gehrz, C. E. Woodward, A. A. Zijlstra, E. Polomski, M. T. Rushton, S. P. S. Eyres, S. G. Starrfield, J. Krautter, and R. M. Wagner,\\
-**[[http://dx.doi.org/10.1111/j.1745-3933.2006.00246.x|The //Spitzer// Infrared Spectrometer View of V4334 Sgr (Sakurai’s Object)]]**\\+**[[https://doi.org/10.1111/j.1745-3933.2006.00246.x|The //Spitzer// Infrared Spectrometer View of V4334 Sgr (Sakurai’s Object)]]**\\
 //Mon. Not. R. Astron. Soc.// **373**, L75–L79 (2006). //Mon. Not. R. Astron. Soc.// **373**, L75–L79 (2006).
  
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