C2 Bands Research Articles

Time and species dependent ambient air’s effects on carbon clusters generated during femtosecond laser ablation of highly oriented pyrolytic graphite

Near infrared femtosecond laser is employed to ablate highly oriented pyrolytic graphite (HOPG) in ambient air and in vacuum respectively. The recorded transient emission spectra of the ablated plume with a time resolution of 2 ns indicate that the effects of air on the plume are dependent on both time and species. This finding provides important insights into the generation and decay mechanisms of different carbon radicals or clusters. At 1 or 2 ns after the laser pulse strikes the target, air weakens the Swan bands of C2 compared with the case in vacuum, an effect that may be caused by the quenching collisions between air molecules and C2 radicals. This result shows that C2 may be mainly generated by direct spallation from the target surface at the early stage of ablation. Emission spectra at large time delays present that the existence time of the Swan bands in air is longer than the lifetime of the upper electronic state of the Swan system, suggesting that the air-involved three-body recombination and collisional excitation that enhance the generation of emitting C2 overcome quenching collisions at large time delays. A spectral band at ~416 nm assigned to the transition from 1Σ u + to X 1Σ g + of C15 is more intense in air than in vacuum, indicating that C15 clusters are generated at least partially by the combination of smaller clusters in air. It is also found that air-assisted heat transfer makes the temperature of carbon clusters decrease more quickly in air than in vacuum, leading to a much shorter lifetime of the continuum in air.

The Formation of Gas Bubbles by Processing of Liquid n-Heptane in the Microwave Discharge

Numerical modeling of the process of formation of gas bubbles during initiation of the microwave discharge in liquid n-heptane at atmospheric pressure has been performed. The developed model has an axial symmetry. The model is based on joint solution of the Maxwell equations, Navier–Stokes equation, heat equation, continuity equations for electrons (written in the ambipolar diffusion approximation) and the n-heptane concentration (including its thermal decomposition and dissociation by electron impact) and the Boltzmann equation for free electrons of the plasma. The calculations allowed to describe the dynamics of the formation of gas bubbles in the liquid, to evaluate the role of electron impact in the decomposition of n-heptane, and to estimate the characteristic times of various processes in the system. The results of new experiments are compared with the simulation results. On the basis of this comparison one could explain the presence in the spectra of the discharge only bands of C2.

LOW PRESSURE CH2Cl2 PLASMA DISCHARGE

Glow discharge of dichloromethane (DCM) was investigated employing Optical Emission Spectroscopy (OES), while the electron temperature and electron density were measured using a double Langmuir probe. Deposits formed were characterized by Scanning Electron Microscopy (SEM), X-ray Photo Fluorescence Spectroscopy (XPS) and Fourier Transform Infrared Spectroscopy (FTIR). The species identified by OES were the molecular bands of C2, C3, CH, H2, CH+, HCl+, Cl and C+. The material deposited displays a growing behavior. SEM observation shows several features which correspond to coalesce and growth mechanism. The characterization of the material deposited can explain the different stages of deposits that are formed on the electrode surface. Several factors are concerned in the complexity of the process, regarding the interaction of species formed during the plasma discharge. Involving several bonds types such as: C=C, C=C-CH2-Cl, C-C and CH.

Optical emission spectra analysis of thermal plasma treatment of poly(vinyl chloride)

Abstract Decomposition of poly(vinyl chloride) (PVC) was investigated in radiofrequency thermal plasma in neutral, oxidative and reductive conditions. Optical emission spectroscopy (OES) was applied for the characterization of the plasma column. OES was used to identify active plasma components such as excited atoms, ions, radicals and molecules. The spectra were dominated by molecular C2, CN, OH, and CH bands, and atomic H, Ar, C, Cl and O lines. Emission intensities of main species were monitored versus various experimental parameters. The rotational-vibrational temperatures determined from different bimolecular species were considered in the range of 2000–6400 K. Solid soot samples were collected and purified to investigate the possibility of graphene formation as a by-product of the decomposition process.

Organic molecules in translucent interstellar clouds.

Absorption spectra of translucent interstellar clouds contain many known molecular bands of CN, CH+, CH, OH, OH+, NH, C2 and C3. Moreover, one can observe more than 400 unidentified absorption features, known as diffuse interstellar bands (DIBs), commonly believed to be carried by complex, carbon-bearing molecules. DIBs have been observed in extragalactic sources as well. High S/N spectra allow to determine precisely the corresponding column densities of the identified molecules, rotational temperatures which differ significantly from object to object in cases of centrosymmetric molecular species, and even the 12C/13C abundance ratio. Despite many laboratory based studies of possible DIB carriers, it has not been possible to unambiguously link these bands to specific species. An identification of DIBs would substantially contribute to our understanding of chemical processes in the diffuse interstellar medium. The presence of substructures inside DIB profiles supports the idea that DIBs are very likely features of gas phase molecules. So far only three out of more than 400 DIBs have been linked to specific molecules but none of these links was confirmed beyond doubt. A DIB identification clearly requires a close cooperation between observers and experimentalists. The review presents the state-of-the-art of the investigations of the chemistry of interstellar translucent clouds i.e. how far our observations are sufficient to allow some hints concerning the chemistry of, the most common in the Galaxy, translucent interstellar clouds, likely situated quite far from the sources of radiation (stars).

Photometric studies of comet C/2009 P1 (Garradd) before the perihelion

The results of the photometric observations of comet C/2009 P1 (Garradd) performed at the 60-cm Zeiss-600 telescope of the Terskol observatory have been analyzed. During the observations, the comet was at the heliocentric and geocentric distances of 1.7 and 2.0 AU, respectively. The CCD images of the comet were obtained in the standard narrowband interference filters suggested by the International research program for comet Hale-Bopp and correspondingly designated the 'Hale-Bopp (HB) set'. These filters were designed to isolate the BC ($\lambda$4450/67 {\AA}), GC ($\lambda$5260/56 {\AA}) and RC ($\lambda$7128/58 {\AA}) continua and the emission bands of C2 ($\lambda$5141/118 {\AA}), CN ($\lambda$3870/62 {\AA}), and C3 ($\lambda$4062/62 {\AA}). From the photometric data, the dust production rate of the comet and its color index and color excess were determined. The concentration of C2, CN, and C3 molecules and their production rates along the line of sight were estimated. The obtained results show that the physical parameters of the comet are close to the mean characteristics typicalof the dynamically new comets.

Analysis of high-temperature thermoelectric properties of p-type CoSb3 within a two-valence-band and two-conduction-band model

Experimental data on the thermoelectric properties of p-type CoSb3 reported by Caillat et al. [J. Appl. Phys. 80, 4442 (1996)] have been analyzed, assuming not only a pair of the first valence (v1) and the first conduction (c1) bands but also the second valence (v2) and the second conduction (c2) bands. By taking into account the excitation of carriers into the v2 and the c2 bands, the behavior of the Hall coefficient as well as that of the Seebeck coefficient at high temperatures is well explained. By taking into account the nonparabolicity of the v1 band, the temperature dependence of mobility is well explained with assuming scattering due to acoustic phonons, nonpolar and polar optical phonons, and ionized impurities. Furthermore, various material parameters of CoSb3, such as the band-gap energy, effective masses, and deformation potentials, have been deduced from fitting the calculation to the experimental data on the temperature dependences of the Hall coefficient, the mobility, and the Seebeck coefficient. Among them, the band-gap energy and the effective mass of the v1 band have been corrected from the original values estimated by Caillat et al. In addition, it is shown that the experimental data on the hole-concentration dependences of both the room-temperature Seebeck coefficient and the cyclotron mass are well reproduced by the theoretical calculation using the deduced values for the nonparabolic v1 band.

Diamondoid synthesis in atmospheric pressure adamantane–argon–methane–hydrogen mixtures using a continuous flow plasma microreactor

Due to their small size, low-power consumption and potential for integration with other devices, microplasmas have been used increasingly for the synthesis of nanomaterials. Here, we have investigated the possibility of using dielectric barrier discharges generated in continuous flow glass microreactors for the synthesis of diamondoids, at temperatures of 300 and 320 K, and applied voltages of 3.2–4.3 kVp–p, at a frequency of 10 kHz. The microplasmas were generated in gas mixtures containing argon, methane, hydrogen and adamantane, which was used as a precursor and seed. The plasmas were monitored by optical emission spectroscopy measurements and the synthesized products were characterized by gas chromatography—mass spectrometry (GC–MS). Depending on the gas composition, the optical emission spectra contained CH and C2 bands of varying intensities. The GC–MS measurements revealed that diamantane can be synthesized by microplasmas generated at atmospheric pressure, and that the yields highly depend on the gas composition and the presence of carbon sources.

THE TRANSIENT MOLECULAR ENVELOPE IN THE OUTFLOW OF THE NOVA V2676 Oph DURING ITS EARLY PHASE

Novae are generally considered to be hot astronomical objects which show effective temperatures of 10,000 K or higher at their visual maximum. However, theoretical predictions suggest that the outer envelope of the nova outflow can become cool enough to form molecules which would be dissociated at such high temperatures. We detected strong C2 and CN absorption bands in the optical spectrum of the nova V2676 Oph, a very slow nova with dust formation. This is the first report of the detection of C2, and the second of CN, in novae during an outburst. Although, based on previous studies, such simple molecules are predicted form in the envelope of the outflow, there are few reports of their detection thus far. The presence of the molecular envelope is considered to be very transient, with a duration of only a few days, in the case of V2676 Oph.

Multibubble sonoluminescence as a tool to study the mechanism of formic acid sonolysis

Sonoluminescence spectra collected from 0.1 to 3.0M aqueous solutions of formic acid sparged with argon show the OH(A2Σ+−X2Πi) and C2(d3Πg→a3Πu) emission bands and a broad continuum typical for multibubble sonoluminescence. The overall intensity of sonoluminescence and the sonochemical yield of HCOOH degradation vary in opposite directions: the sonoluminescence is quenched while the sonochemical yield increases with HCOOH concentration. By contrast, the concentration of formic acid has a relatively small effect on the intensity of C2 Swan band. It is concluded that C2 emission originates from CO produced by HCOOH degradation rather than from direct sonochemical degradation of HCOOH. The intensity of C2 band is much stronger at high ultrasonic frequency compared to 20kHz ultrasound which is in line with higher yields of CO at high frequency. Another product of HCOOH sonolysis, carbon dioxide, strongly quenches sonoluminescence, most probably via collisional non-radiative mechanism.

NORMAL AND OUTLYING POPULATIONS OF THE MILKY WAY STELLAR HALO AT [Fe/H] <–2

From detailed abundance analysis of >100 Hamburg/ESO candidate extremely metal-poor (EMP) stars we find 45 with [Fe/H] < -3.0 dex. We identify a heretofore unidentified group: Ca-deficient stars, with sub-solar [Ca/Fe] ratios and the lowest neutron-capture abundances; the Ca-deficient group comprises ~ 10% of the sample, excluding Carbon stars. Our radial velocity distribution shows that the carbon-enhanced stars with no s-process enhancements, CEMP-no, and which do not show C2 bands are not preferentially binary systems. Ignoring Carbon stars, approximately 15% of our sample are strong (> 5 sigma) outliers in one, or more, elements between Mg and Ni; this rises to ~19% if very strong (>10 sigma) outliers for Sr and Ba are included. Examples include: HE0305-0554 with the lowest [Ba/H] known; HE1012-1540 and HE2323-0256, two (non-velocity variable) C-rich stars with very strong [Mg,Al/Fe] enhancements; and HE1226-1149 an extremely r-process rich star.

Experimental validation of local thermal equilibrium in a MW plasma torch for hydrogen production

In this paper, experimental and numerical studies are made to investigate local thermal equilibrium in a microwave plasma torch at atmospheric pressure for hydrogen and carbon black production from methane dissociation. The microwave induced plasma can be operated up to 2 kW power at 2.45 GHz frequency. Methane is dissociated in argon, air or nitrogen plasma and optical emission spectroscopy is used to characterize the plasma. C2, CN and OH ro-vibrational bands are used for rotational and vibrational temperature estimation while stark broadening of H-line is used for electron temperature calculation. Temperatures are determined at varying operating parameters of microwave power, axial gas flow rate, and methane flow rate. The rotational (heavy particle), vibrational, and electron temperatures are found to be equal to 5000 ± 500 K. The plasma is thus at local thermodynamic equilibrium.

C2 and Diffuse Interstellar Bands

AbstractC2, the simplest multicarbon molecule is a useful astronomical tool, because the analysis of its lines allows to determine the physical conditions in interstellar clouds. C2 abundances give information about the chemistry of interstellar clouds, especially on the pathway to the formation of long-chain carbon molecules, which may be connected with carriers of diffuse interstellar bands (Douglas 1977, Thorburn et al. 2003). Here we summarize all relations between C2 and diffuse interstellar bands (DIBs).

Spectral studies of comet C/2001 Q4 (NEAT)

The paper presents the results of the spectral observations of comet C/2001 Q4 (NEAT) acquired with the Zeiss-600 telescope of the Andrushevka astronomical observatory in May 2004. The spectrum of the comet was obtained in the range of 3600–8200 A. We identified a number of emission features in the spectrum of comet C/2001 Q4 (NEAT). The emission bands of C2, C3, CN, CH, NH2, H2O+ were detected in the spectrum of the comet, and their intensities were determined. The ratios of gas-production rates Q(C2)/Q(CN) = 0.23, Q(C3)/Q(CN) = −0.79, and Q(NH2)/Q(CN) = −0.029 were determined with the Haser model.

Red clump stars of the Milky Way – laboratories of extra-mixing

In this work we present the main atmospheric parameters, carbon, nitrogen and oxygen abundances, and 12C/13C ratios determined in a sample of 28 Galactic clump stars. Abundances of carbon were studied using the C2 band at 5086.2 {\AA}. The wavelength interval 7980-8130 {\AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300 {\AA}. The mean abundances of C, N and O abundances in the investigated clump stars support our previous estimations that, compared to the Sun and dwarf stars of the Galactic disc, carbon is depleted by about 0.2 dex, nitrogen is enhanced by 0.2 dex and oxygen is close to abundances in dwarfs. The 12C/13C and C/N ratios for galactic red clump stars analysed were compared to the evolutionary models of extra-mixing. The steeper drop of 12C/13C ratio in the model of thermohaline mixing by Charbonnel & Lagarde better reflects the observational data at low stellar masses than the more shallow model of cool bottom processing by Boothroyd & Sackmann. For stars of about 2 Msun masses a modelling of rotationally induced mixing should be considered with rotation of about 250 km s-1 at the time when a star was at the hydrogen-core-burning stage.

THE GALACTIC R CORONAE BOREALIS STARS: THE C2SWAN BANDS, THE CARBON PROBLEM, AND THE12C/13C RATIO

Observed spectra of R Coronae Borealis (RCB) and hydrogen-deficient carbon (HdC) stars are analyzed by synthesizing the C2 Swan bands (1,0), (0,0), and (0,1) using our detailed line list and the Uppsala model atmospheres. The (0,1) and (0,0) C2 bands are used to derive the 12C abundance, and the (1,0) 12C13C band to determine the 12C/13C ratios. The carbon abundance derived from the C2 Swan bands is about the same for the adopted models constructed with different carbon abundances over the range: 8.5 (C/He = 0.1%), to 10.5 (C/He = 10%). Carbon abundances derived from C I lines are about a factor of 4 lower than the carbon abundance of the adopted model atmosphere over the same C/He interval, as reported by Asplund et al. (2000), who dubbed the mismatch between adopted and derived C abundance the 'carbon problem'. In principle, the carbon abundances obtained from C2 Swan bands and that assumed for the model atmosphere can be equated for a particular choice of C/He that varies from star to star. Then, the carbon problem for C2 bands is eliminated. However, such C/He ratios are in general less than those of the EHe stars, the seemingly natural relatives to the RCB and HdC stars. A more likely solution to the C2 carbon problem may lie in a modification of the model atmosphere's temperature structure. The derived carbon abundances and the 12C/13C ratios are discussed in light of the double degenerate (DD) and the final flash (FF) scenarios.

Time-resolved LIBS of atomic and molecular carbon from coal in air, argon and helium

Laser ablation chemical analysis of a coal sample was studied by LIBS (laser-induced breakdown spectroscopy). Ablation was performed using a 266 nm Nd:YAG laser in different gas environments (air, argon and helium) at atmospheric pressure. We present characteristics of spectra measured from coal with special attention to atomic and molecular carbon including CI, C2 and CN. The influence of the ambient gas on the laser-induced coal plasma was studied by using time-resolved analysis. Atomic iron emission lines were employed to construct Boltzmann plots for the plasma excitation temperature. Computer simulations of C2 spectra were used to deduce the molecular rotational temperature. Electron density and total atomic and molecular number density are reported to describe emission differences of atomic and molecular carbon in the different gas environments. These data demonstrate that the plasma excitation temperature is the primary factor contributing to differences among the atomic carbon emission in the gas environments. Reactions between the plasma species and ambient gas, and the total molecular number are main factors influencing molecular carbon emission. Finally, the influence of laser energy on the rotational temperature was studied in the air environment to demonstrate that the rotational temperature derived from C2 band emission can be utilized to correct plasma fluctuations.

Experimental study on the characteristics of molecular emission spectroscopy for the analysis of solid materials containing C and N

Solid materials with different structure containing C and N were analyzed by laser-induced breakdown spectroscopy (LIBS). Comparing the emission molecular species in different atmosphere (air and argon), it can be determined that whether the molecular species are directly vaporized from sample or generated through dissociation or the interaction between plasma and air molecules. The results showed that the characteristic of C2 bands emission is similar with that of neutral atomic carbon emission CI in different atmosphere (air and argon). While the characteristic of CN bands emission is more complicated and it has great relationship with the existence of CN radicals, the interaction between plasma and air ambient, and the recombination of excited partials.

Suppression of carbon dust agglomeration and volatile molecular formation in C–H–N reactive molecular system

Chemical erosion of carbon materials and dust formation in low-temperature and neutral particle-dominated plasmas were investigated using high-pressure inductively coupled plasmas. Experiments were performed with Ar/H2/N2 mixture plasma irradiation to graphite targets. The addition of just a few percent of nitrogen gas to hydrogen led to significant suppression of carbon dust formation on the graphite target. From optical emission spectroscopy, CN band spectra were observed strongly in Ar/H2/N2 plasmas with a decrease of CH and C2 band emission intensity. These results showed that CN bond formation, which caused chemical erosion of carbon by producing volatile CN, HCN, and C2N2 particles, might have been a key suppression mechanism of the carbon particle aggregation.

Centrosymmetric molecules as possible carriers of diffuse interstellar bands★

In this paper, we present new data with interstellar C2 (Phillips bands A-X), from observations made with the Ultraviolet-Visual Echelle Spectrograph of the European Southern Observatory. We have determined the interstellar column densities and excitation temperatures of C2 for nine Galactic lines. For seven of these, C2 has never been observed before, so in this case the still small sample of interstellar clouds (26 lines of sight), where a detailed analysis of C2 excitation has been made, has increased significantly. This paper is a continuation of previous works where interstellar molecules (C2 and diffuse interstellar bands) have been analysed. Because the sample of interstellar clouds with C2 has increased, we can show that the width and shape of the profiles of some diffuse interstellar bands (6196 and 5797 A) apparently depend on the gas kinetic and rotational temperatures of C2; the profiles are broader because of the higher values of the gas kinetic and rotational temperatures of C2. There are also diffuse interstellar bands (4964 and 5850 A) for which this effect does not exist.