The bandspectrum of CO+

“…The data used for their calculations were based on a compilation of nearly two dozen empirical and theoretical papers. Line positions (given in cm −1 ) were taken from Schmid & Gerö (1933), Bulthuis (1934), Narahari Rao (1950a), and Herzberg (1950. Oscillator strengths were drawn from Joshi (1966) and Jain (1972).…”

Section: Co +mentioning

confidence: 99%

Knowledge Gaps in the Cometary Spectra of Oxygen-Bearing Molecular Cations

Fortenberry,

Bodewits,

Pierce

2021

Preprint

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Molecular cations are present in various astronomical environments, most notably in cometary atmospheres and tails where sunlight produces exceptionally bright near-UV to visible transitions. Such cations typically have longer-wavelength and brighter electronic emission than their corresponding neutrals. A robust understanding of their near-UV to visible properties would allow these cations to be used as tools for probing the local plasma environments or as tracers of neutral gas in cometary environments. However, full spectral models are not possible for characterization of small, oxygen containing molecular cations given the body of molecular data currently available. The five simplest such species (H 2 O + , CO + 2 , CO + , OH + , and O + 2 ) are well characterized in some spectral regions but are lacking robust reference data in others. Such knowledge gaps hinder fully quantitative models of cometary spectra, specifically, hindering accurate estimates of physical-chemical processes originating with the most common molecules in comets. Herein the existing spectral data are collected for these molecules and highlight the places where future work is needed, specifically where the lack of such data would greatly enhance the understanding of cometary evolution.

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“…The cases y"=y'-&y and y"=(+y for vibrational levels v>0 of the B2 and states are investigated on the basis of the obtained from Rao values Ay. In both cases, mean values of ' (for the B state), close to 0.0192, are obtained using the module values A'y=I 'y'-'y" I of the (1,2) and (1,3) bands. For that reason, the value y=O.0192 is attributed to all vibrational levels of the B2 state.…”

Section: Parameter Y Of the B2 And X2 Statesmentioning

confidence: 99%

Creation of the CO+ spectrum for analysis of Halley's Comet spectrum

1999

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The solar wind-comet interaction, one of the basic processes investigated in the cometary physics, may be judged by the ion's behavior. CO is one of the most abundant cometary atmosphere species. A synthetic spectrum of CO was created to analyze Halley's comet spectra. The values of some molecular constants were specified in order to improve the accuracy of the computations. It was established that the more appropriate value of the spin-rotational interaction parameter y for the B2 state is 0.0192. The use of different values of y for the higher vibrational levels (v>O) of the X and B states didn't help for a more precise result. That's why it is recommended to use the same value y for all vibrational levels of a given state. The value -122.0 was determined for the spin-orbital interaction parameter A of the A2'it state. The molecular model, needed to create a spectrum which adequately reproduces the total CO glow has been specified: v0÷4 for X2E state, v=O÷6 for A2ir state, '=O÷2 for B2E state and rotational levels up to N=12 for an optimal theoretical spectrum and up to N=8 for analysis of Halley's comet spectra registered by the three-channel spectrometer on board the Vega-2.

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The bandspectrum of CO+

Cited by 7 publications

References 5 publications

The band spectrum of carbon monoxide

The band spectrum of carbon monoxide

Knowledge Gaps in the Cometary Spectra of Oxygen-Bearing Molecular Cations

Creation of the CO+ spectrum for analysis of Halley's Comet spectrum

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