Analysis of the 4050-Å Group of the C_{3} Molecule.

Gausset, L.; Herzberg, G.; Lagerqvist, A; Rosen, B.P.

doi:10.1086/148262

Cited by 272 publications

(138 citation statements)

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“…The rest wavelengths for C 3 have been adapted from Gausset et al (1965). Becker et al (1979) have derived an electronic oscillator strength f el = 0.0246 from experimental lifetime measurements of electronically excited C 3 ( 1 Π u ).…”

Section: Observations and Resultsmentioning

confidence: 99%

Interstellar C$_\mathsf{3}$ toward HD 210121

Roueff¹,

Felenbok²,

Black³

et al. 2002

A&A

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Abstract.We report the detection of the 405 nm band of interstellar C3 in absorption toward HD 210121. The abundance of triatomic carbon is approximately 1/17 of that of diatomic carbon in the same diffuse molecular cloud. Rotational levels of C3 up to J = 14 are seen in this cloud. The rotational excitation of C3 in the interstellar medium may reflect a competition between inelastic collisions, formation and destruction of the molecule, and radiative pumping in the far-infrared. The abundance of C3 is compared with chemical models. Attention is called to molecular properties that need to be better determined.

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Section: Observations and Resultsmentioning

confidence: 99%

Interstellar C$_\mathsf{3}$ toward HD 210121

Roueff¹,

Felenbok²,

Black³

et al. 2002

A&A

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“…The study gave the wavenumbers of the different rotational lines of the 4050Å group, an identification of the different vibrational levels which are involved, and the basic vibrational and rotational constants of the vibrational states. As one of the main results, Gausset et al (1965) concluded that the bending frequency ν 2 is very small, with a value of about 63 cm −1 in the X 1 Σ + g electronic ground state. The small value implies that a multitude of vibrational levels are significantly populated, even at low temperatures.…”

Section: The C 3 Radicalmentioning

confidence: 95%

“…The pioneering work was published by Gausset et al (1965). That paper was based on the laboratory data available then.…”

Section: The C 3 Radicalmentioning

confidence: 99%

A fluorescence model of the C₃radical in comets

Rousselot¹,

Arpigny

Rauer³

et al. 2001

A&A

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Abstract. Theoretical resonance fluorescence calculations are presented of the triatomic C3 radical and are compared with observations of the C3 emission in comets Hale-Bopp and de Vico. A theoretical model of the C3 vibration-rotational structure in theThe model takes into account the detailed structure of the bending mode ν2 which is responsible for the emission of the 4050Å group. A total of 1959 levels are considered, with 515 levels in the ground state. The main effort is to model high-resolution spectra of the 4050Å emission in comets C/1995 O1 Hale-Bopp and 122P/1995 S1 de Vico. The agreement between observed and theoretical spectra is good for a value of the dipole moment derivative of dµ dr ≈ 2.5 DebyeÅ −1 . The modeled C3 emission exhibits a pronounced Swings effect.

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“…The rich C 3 emission around 4050Å has eight certainly identifiable peaks which are partly blended with weaker emissions of N + 2 , CH + , CO + , and CO + 2 (see Wyckoff & Theobald 1989). In our spectra, there is some evidence for C 3 also contributing to the emissions at wavelengths shorter than CN (0 − 0) (see Gausset et al 1965;Valk et al 1989). Finally, the CH radical is represented by its (0 − 0) AX band.…”

Section: Spectramentioning

confidence: 52%

“…Molecular bands. To identify the emission features in the cometary spectra they were compared with theoretical and laboratory wavelengths and observed spectra (Gerö 1941;Mrozowski 1947a,b;Swings & Haser 1956;Gausset et al 1965;Brocklehurst et al 1972;McCallum & Nicholls 1972;Zucconi & Festou 1985;Arpigny et al 1986a,b;Magnani & A'Hearn 1986;Jockers et al 1987;Wyckoff & Theobald 1989;Valk et al 1992;Kim & A'Hearn 1993, pers. communication;Lutz et al 1993).…”

Section: Derivation Of Absolute Intensitiesmentioning

confidence: 99%

Spatial distribution of neutral and ionic constituents in comet P/Halley

Umbach

Jockers

Geyer

1998

Astron. Astrophys. Suppl. Ser.

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Abstract. Multislit spectra of comet P/Halley were obtained on April 10, 1986, using a focal reducer with a field of ≈ 0.5• angular diameter. The number and arrangement of the slits allowed a reconstruction of the spatial distribution of principal neutral and ionic coma constituents within a frame of about 4 10 5 × 4 10 5 km 2 at the comet. Radial profiles and two-dimensional maps for the dust continuum, CN, C 3 , CH, CO + , and especially CO + 2 , are presented in absolute intensity and column density units, respectively. Scale lengths and production rates for the radicals were determined within the Haser model. The molecular ions are not only restricted to the plasma tail but are also present in the sunward coma. Instead of forming a peak at the nucleus like the neutral radicals the ion column densities decrease rapidly in the solar direction and form a plateau extending from the nucleus into the antisolar direction. The distribution of CO + 2 shows a stronger decrease in the tailward direction than that of CO + .

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Analysis of the 4050-Å Group of the C_{3} Molecule.

Cited by 272 publications

References 0 publications

Interstellar C$_\mathsf{3}$ toward HD 210121

Interstellar C$_\mathsf{3}$ toward HD 210121

A fluorescence model of the C₃radical in comets

Spatial distribution of neutral and ionic constituents in comet P/Halley

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Analysis of the 4050-Å Group of the C_{3} Molecule.

Cited by 272 publications

References 0 publications

Interstellar C$_\mathsf{3}$ toward HD 210121

Interstellar C$_\mathsf{3}$ toward HD 210121

A fluorescence model of the C3radical in comets

Spatial distribution of neutral and ionic constituents in comet P/Halley

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Resources

About

A fluorescence model of the C₃radical in comets