Reinvestigations of the A2Δ-X2Π band system in the CH radical

Bembenek, Z.; Kępa, R.; Para, Andrzej; Rytel, M.; Zachwieja, M.; Janjić, J.D.; Marx, Erich

doi:10.1016/0022-2852(90)90238-l

Cited by 44 publications

(27 citation statements)

References 26 publications

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“…The results concerning the calculation of wavelengths are in good accordance with experimental values of Fagerhölm [14] , Gerö [15] and Bembenek et al [16]. An analysis of the simulated spectrum shows that some spectral lines (10 < N < 24) are well isolated and can be therefore used as "thermometric lines".…”

Section: Resultssupporting

confidence: 87%

Diagnostics of a Hydrocarbon Plasma Jet Using the A²Δ-X²Π System of CH

et al. 1998

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We study the intensity distribution of the A 2Δ-Χ 2Π system of CH molecule at 430 nm in a low pressure plasma jet. This system shows an overlap of vibrational bands with Δν = 0. By comparing simulated and experimental emission spectra, we obtain rotational and vibrational temperatures using Boltzmann plots or some thermometer functions. The thermometer . functions are the integrated intensities of line-like transitions composed of several rotational transitions. The result of the Boltzmann plots and the thermometer functions method that we propose are in good agreement.

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Section: Resultssupporting

confidence: 87%

Diagnostics of a Hydrocarbon Plasma Jet Using the A²Δ-X²Π System of CH

et al. 1998

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“…In Table I, the equilibrium geometry results for the rotational g-factor of 12 C 1 H + , 12 C 2 H + , 13 C 1 H + , and 13 C 2 H + at the SCF-LR, CASSCF-LR, and CCSD͑T͒ levels are collected. In Table II, corresponding results for the spin-rotation constants of 13 C, 1 H, and 2 H are shown.…”

Section: Resultsmentioning

confidence: 99%

“…[1][2][3] To confirm this identification, its electronic, vibrational, and rotational transitions have also been studied in the laboratory. [4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19] Apart from its astrophysical importance, the CH + ion has also attracted much attention such as BH and AlH due to their unusual magnetic properties [20][21][22][23][24][25][26][27][28][29][30][31][32][33] similar to temperature independent paramagnetism, antishielding, a large spin-rotation constant of the carbon atom, and a large and negative rotational g-factor, which are rarely found in closed shell molecules.…”

Section: Introductionmentioning

confidence: 99%

“…18 The measured spin-rotation constant was found to agree well with a calculated value of Sauer and Paidarová. 32 Their approach consisted of vibration-rotational averaging a spin-rotation radial function for 13 CH + calculated with the coupled-cluster singles and doubles polarization propagator approximation ͑CCSDPPA͒, 34 which is a precursor to the second-order polarization propagator approximation with coupled-cluster singles and doubles amplitudes method ͓SOPPA͑CCSD͔͒. 35 However, no analogous ab initio calculation of the rotational g-factor has so far been published, which would be sufficiently accurate for a comparison with experimental values.…”

Section: Introductionmentioning

confidence: 99%

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Communication: Rotational g-factor and spin-rotation constant of CH+

Sauer

2010

The Journal of Chemical Physics

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The rotational g-factor and spin-rotation constants of the methylidynium ion CH + have been calculated for the first time with a large multiconfigurational self-consistent field wave function and at the coupled-cluster singles and doubles level augmented by a perturbative triples correction. The results for an equilibrium internuclear distance as well as for the v =0, J = 1 vibration-rotational state are presented.

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“…We compiled the CN line list using laboratory measured wavelengths and by calculating line oscillator strengths from measured molecular constants and band oscillator strengths (Knowles et al 1988;Rehfuss et al 1992;Prasad et al 1992;Davis et al 2005;Ram et al 2006). The CH line list was compiled in the same way using wavelengths, molecular constants, and band oscillator strengths by Krupp (1974); Bembenek et al (1990). The CN and CH B − X systems are strongly perturbed by relatively weak external magnetic fields: the complete Paschen-Back effect (PBE) starts at 77 G and 305 G for the CN and CH bands, respectively (Berdyugina et al 2005).…”

Section: Simulationsmentioning

confidence: 99%

Comparison of solar photospheric bright points between Sunrise observations and MHD simulations

Riethmüller

Solanki

Berdyugina

et al. 2014

A&A

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Bright points (BPs) in the solar photosphere are thought to be the radiative signatures (small-scale brightness enhancements) of magnetic elements described by slender flux tubes or sheets located in the darker intergranular lanes in the solar photosphere. They contribute to the ultraviolet (UV) flux variations over the solar cycle and hence may play a role in influencing the Earth's climate. Here we aim to obtain a better insight into their properties by combining high-resolution UV and spectro-polarimetric observations of BPs by the Sunrise Observatory with 3D compressible radiation magnetohydrodynamical (MHD) simulations. To this end, full spectral line syntheses are performed with the MHD data and a careful degradation is applied to take into account all relevant instrumental effects of the observations. In a first step it is demonstrated that the selected MHD simulations reproduce the measured distributions of intensity at multiple wavelengths, line-of-sight velocity, spectral line width, and polarization degree rather well. The simulated line width also displays the correct mean, but a scatter that is too small. In the second step, the properties of observed BPs are compared with synthetic ones. Again, these are found to match relatively well, except that the observations display a tail of large BPs with strong polarization signals (most likely network elements) not found in the simulations, possibly due to the small size of the simulation box. The higher spatial resolution of the simulations has a significant effect, leading to smaller and more numerous BPs. The observation that most BPs are weakly polarized is explained mainly by the spatial degradation, the stray light contamination, and the temperature sensitivity of the Fe i line at 5250.2 Å. Finally, given that the MHD simulations are highly consistent with the observations, we used the simulations to explore the properties of BPs further. The Stokes V asymmetries increase with the distance to the center of the mean BP in both observations and simulations, consistent with the classical picture of a production of the asymmetry in the canopy. This is the first time that this has been found also in the internetwork. More or less vertical kilogauss magnetic fields are found for 98% of the synthetic BPs underlining that basically every BP is associated with kilogauss fields. At the continuum formation height, the simulated BPs are on average 190 K hotter than the mean quiet Sun, the mean BP field strength is found to be 1750 G, and the mean inclination is 17 • , supporting the physical flux-tube paradigm to describe BPs. On average, the synthetic BPs harbor downflows increasing with depth. The origin of these downflows is not yet understood very well and needs further investigation.

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Reinvestigations of the A2Δ-X2Π band system in the CH radical

Cited by 44 publications

References 26 publications

Diagnostics of a Hydrocarbon Plasma Jet Using the A²Δ-X²Π System of CH

Diagnostics of a Hydrocarbon Plasma Jet Using the A²Δ-X²Π System of CH

Communication: Rotational g-factor and spin-rotation constant of CH+

Comparison of solar photospheric bright points between Sunrise observations and MHD simulations

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Reinvestigations of the A2Δ-X2Π band system in the CH radical

Cited by 44 publications

References 26 publications

Diagnostics of a Hydrocarbon Plasma Jet Using the A2Δ-X2Π System of CH

Diagnostics of a Hydrocarbon Plasma Jet Using the A2Δ-X2Π System of CH

Communication: Rotational g-factor and spin-rotation constant of CH+

Comparison of solar photospheric bright points between Sunrise observations and MHD simulations

Contact Info

Product

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Diagnostics of a Hydrocarbon Plasma Jet Using the A²Δ-X²Π System of CH

Diagnostics of a Hydrocarbon Plasma Jet Using the A²Δ-X²Π System of CH