Differences
This shows you the differences between two versions of the page.
molecules:ism:c2h [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:c2h [2019/10/21 17:18] (current) – mueller | ||
---|---|---|---|
Line 3: | Line 3: | ||
The ethynyl radical in its < | The ethynyl radical in its < | ||
K. D. Tucker, M. L. Kutner, and P. Thaddeus,\\ | K. D. Tucker, M. L. Kutner, and P. Thaddeus,\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
// | // | ||
before it was actually detected in the laboratory. The identification was based on hyperfine parameters obtained from electron-spin resonance measurements of ethynyl isolated in argon matrices. The molecule is rather ubiquitous as it has been detected in several star-forming regions such as W3, Orion A, Sgr B2, Sgr A, of which several include photon-dominated regions (PDRs), most notably M17 SW. It has also been detected in the circumstellar envelope of the carbon-rich late-type star CW Leo, also known as IRC +10216. | before it was actually detected in the laboratory. The identification was based on hyperfine parameters obtained from electron-spin resonance measurements of ethynyl isolated in argon matrices. The molecule is rather ubiquitous as it has been detected in several star-forming regions such as W3, Orion A, Sgr B2, Sgr A, of which several include photon-dominated regions (PDRs), most notably M17 SW. It has also been detected in the circumstellar envelope of the carbon-rich late-type star CW Leo, also known as IRC +10216. | ||
A. Wootten, E. P. Bozyan, D. P. Garrett, R. B. Loren, and R. L. Snell reported on the\\ | A. Wootten, E. P. Bozyan, D. P. Garrett, R. B. Loren, and R. L. Snell reported on the\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
// | // | ||
The radical was also observed in the diffuse medium by:\\ | The radical was also observed in the diffuse medium by:\\ | ||
L.-Å. Nyman,\\ | L.-Å. Nyman,\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
C< | C< | ||
F. Combes, F. Boulanger, P. J. Encrenaz, M. Gerin, M. Bogey, C. Demuynck, J. L. Destomb,\\ | F. Combes, F. Boulanger, P. J. Encrenaz, M. Gerin, M. Bogey, C. Demuynck, J. L. Destomb,\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
The detection of the < | The detection of the < | ||
A. H. Saleck, R. Simon, G. Winnewisser, | A. H. Saleck, R. Simon, G. Winnewisser, | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Can. J. Phys.// **72** 747–754 (1994). | //Can. J. Phys.// **72** 747–754 (1994). | ||
Three out of four observable fine structure components of the //N// = 3 – 2 rotational transition of vibrationally excited C< | Three out of four observable fine structure components of the //N// = 3 – 2 rotational transition of vibrationally excited C< | ||
E. D. Tenenbaum, J. L. Dodd, S. N. Milam, N. J. Woolf, and L. M. Ziurys,\\ | E. D. Tenenbaum, J. L. Dodd, S. N. Milam, N. J. Woolf, and L. M. Ziurys,\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
The features were detected in the outer part of the circumstellar envelope of CW Leo; hence, the detection must be facilitated by formation pumping or by IR pumping. | The features were detected in the outer part of the circumstellar envelope of CW Leo; hence, the detection must be facilitated by formation pumping or by IR pumping. | ||
Line 34: | Line 34: | ||
The // | The // | ||
J. J. Keady and K. H. Hinkle,\\ | J. J. Keady and K. H. Hinkle,\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
// | // | ||
The rotational temperature of 12.5 ± 1.5 K suggests a peak abundance about 1200 stellar radii away from CW Leo, and the line intensities indicate a high fractional abundance with respect to H< | The rotational temperature of 12.5 ± 1.5 K suggests a peak abundance about 1200 stellar radii away from CW Leo, and the line intensities indicate a high fractional abundance with respect to H< | ||
Line 42: | Line 42: | ||
Contributor(s): | Contributor(s): | ||
- | |||
---- | ---- | ||