Vervollst�ndigung der Analyse der CH-Banden

Gerö, L.

doi:10.1007/bf01339264

Cited by 77 publications

(23 citation statements)

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“…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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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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“…We adopted line positions of the bands measured by Bernath et al (1991). Bembenek et al (1990) and Gero (1941) also presented line positions of the band, but the differences of the line positions among these papers are negligibly small for our purpose. Atype doublet separations occur in the A and X states, but the splits are noticeable only in the X state levels.…”

Section: Modelingmentioning

confidence: 99%

“…1 of Schleicher and A'Hearn (1982). The line positions of this band were mainly adopted from tables of Gero (1941). Bernath et al (1991) also presented the line positions of the B-X band in their Table III, but the identification of branches does not seem right and a line for j = 1.5 in the R2 branch (R1 in Table III A.…”

Section: Modelingmentioning

confidence: 99%

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High-Resolution Spectroscopy of the A-X and B-X System of CH in Comet Austin (1990 V).

Kim

Brown²,

Spinrad³

1997

J. geomagn. geoelec

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We analyzed the A-X(0-0) band of CH, which appears in high-resolution spectra of comet Austin (1990 V), in order to understand fluorescence and collisional processes that influence the rotational structure of the A-X(0-0) band. Some of the weak lines of the A-X (0-0) band are clearly resolved, which have not been previously resolved with relatively low-resolution spectroscopy. We unambiguously confirmed the B-X (0-0) band lines around 3890 A, which had been suspected previously, but it had not been clearly identified because of strong adjacent CN and C3 bands. In order to analyze the cometary spectra we have conducted two different fluorescence calculations: a single-cycle fluorescence and fluorescent equilibrium. The fluorescent equilibrium model includes infrared and ultraviolet fluorescence processes as well as electron and neutral collisional effects, and therefore the model is a function of cometocentic distance. We found that single-cycle fluorescence models with a Boltzmann distribution in the X state fit the observed spectra better than the fluorescent equilibrium models. However, single-cycle fluorescence models with two different temperatures (130 K for F1 state and 250 K for F2 state) in the X state fit the Austin spectra significantly better than the single-cycle fluorescence model with the same temperature (150 K) for F1 and F2 states. This suggests that we are observing two different Boltzmann distributions of nascent, shortlife CH radicals right after they were produced by photodissociations of parent molecules. We presented g-factors of the A-X (0-0) and B-X (0-0) bands as a function of heliocentric velocity based on single-cycle fluorescence models with a 150 K distribution in the X state. We have calculated the expected intensity of the fundamental band (v" = 1 --+ 0) of CH and discussed the detectability of this band near 2730 cm-1. We also discussed possible parent molecules of CH and long lifetimes of the parent molecules, which may explain extensive emissions of CH up to 105 km from the nucleus despite its short lifetime.

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“…Laboratory analysis of the A-X and B-X systems of the CH in emission was accomplished in the works of Gerö (1941), the B-X and C-X systems were measured by Herzberg & Johns (1960); see also Herzberg (1950) as a review. The extensive study of the CH molecule was also presented by Lien (1984).…”

Section: Introductionmentioning

confidence: 99%

On the CH B‐X (1, 0) band in translucent clouds

et al. 2011

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We present observations of CH B-X (1, 0) band toward 13 translucent sightlines. The given precise positions (at 3627.403, 3633.289, 3636.222Å) are derived by means of shifting our spectra to the rest velocity frame using B-X (0, 0) features (at 3878, 3886 and 3890Å). The proposed oscillator strengths (equal to 0.00035, 0.00104, 0.00069, respectively) are based on f -values of the CH B-X (0, 0) system, i.e. 0.00110, 0.00320, 0.00210.

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Vervollst�ndigung der Analyse der CH-Banden

Cited by 77 publications

References 0 publications

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

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

High-Resolution Spectroscopy of the A-X and B-X System of CH in Comet Austin (1990 V).

On the CH B‐X (1, 0) band in translucent clouds

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