Electron paramagnetic resonance forbidden transitions from hydrogen in polycrystalline diamond films

Holder, S. L.; Rowan, L. G.; Krebs, J. J.

doi:10.1063/1.110942

Cited by 43 publications

(16 citation statements)

References 11 publications

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“…17 More recently, the signal has been described as a central line and two hyperfine satellites related to nearby hydrogen nuclei. 18,19 The substitutional N-donor-related resonance could be detected on the high-quality CVD layer with 10 ppm nitrogen. On samples with higher N content, the resonance could only be observed under illumination with band-gap UV light ͓LESR, see Fig.…”

Section: Experiments Resultsmentioning

confidence: 99%

Nitrogen-related dopant and defect states in CVD diamond

et al. 1996

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Subbandgap absorption of chemical-vapor-deposition diamond films, with nitrogen contents varying from 10 to 132 ppm has been explored by the constant-photoconductivity method ͑CPM͒, photothermal-deflection spectroscopy ͑PDS͒ and electron spin resonance ͑ESR͒. The spectra measured by PDS increase monotonically and are structureless with increasing photon energies indicating absorption due to amorphous carbon and graphite. The CPM data show distinct features, with absorption bands at hϭ1.6, 4.0, and 4.7 eV in the nominally undoped film, and 2.4 and 4.7 eV in nitrogen-rich layers respectively. The CPM spectra of the doped films are comparable to photoconductivity data of synthetic Ib diamond. The defect densities involved increase with increasing nitrogen content. From ESR, a vacancy-related defect density (gϭ2.0028) is deduced. Paramagnetic nitrogen (gϭ2.0024) can be detected in the high-quality CVD layer or by illuminating the nitrogenrich samples with photon energies larger than the band gap.

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Section: Experiments Resultsmentioning

confidence: 99%

Nitrogen-related dopant and defect states in CVD diamond

et al. 1996

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“…Recently, the satellite lines from the neighboring 1 H were observed in EPR spectra of hydrogen and deuterium atoms in solid mixtures of 4 He and hydrogen [28]. In polycrystalline diamond films, prepared by the CVD method, hydrogen trapped in the lattice also gives rise to satellite lines against a background of the carbon EPR spectrum which has the typical width of about 0.5 mT in X-band [29]. …”

Section: Introductionmentioning

confidence: 99%

Hyperfine interactions of narrow-line trityl radical with solvent molecules

Trukhan

Yudanov

Tormyshev

et al. 2013

Journal of Magnetic Resonance

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The electron nuclear dipolar interactions responsible for some dynamic nuclear polarization (DNP) mechanisms also are responsible for the presence formally in CW EPR spectra of forbidden satellite lines in which both the electron spin and a nuclear spin flip. Such lines arising from 1H nuclei are easily resolved in CW EPR measurements of trityl radicals, a popular family of DNP reagents. The satellite lines overlap some of the hyperfine features from 13C in natural abundance in the trityl radical, but their intensity can be easily determined by simple simulations of the EPR spectra using the hyperfine parameters of the trityl radical. Isotopic substitution of 2H for 1H among the hydrogens of the trityl radical and/or the solvent allows the dipolar interactions from the 1H on the trityl radical and from the solvent to be determined. The intensity of the dipolar interactions, integrated over all the 1H in the system, is characterized by the traditional parameter called reff. For the so-called Finland trityl in methanol, the reff values indicate that collectively the 1H in the unlabeled solvent have a stronger integrated dipolar interaction with the unpaired electron spin of the Finland trityl than do the 1H in the radical and consequently will be a more important DNP route. Although reff has the dimensions of distance, it does not correspond to any simple physical dimension in the trityl radical because the details of the unpaired electron spin distribution and the hydrogen distribution are important in the case of trityls.

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“…Instead, the meteoritic diamonds display a single central line with "shoulders" (marked with arrows) and a slightly higher g value of 2.0029 2 0.0005 (despite the large error, the higher g value is for real; cf., Rohrer et al., 1996). The "shoulders" are unresolved sidebands caused by H atoms as they are often observed in CVD-diamonds (Jia et al, 1993;Holder et al, 1994). Zhou et al (1996) named this EPR defect HI, and it is most likely composed o f a H atom in the vicinity of a C atom with a dangling bond (Jia et al, 1993;Holder et al, 1994;Zhou et al, 1996).…”

Section: Electron Paramagnetic Resonance Measurementsmentioning

confidence: 99%

“…The "shoulders" are unresolved sidebands caused by H atoms as they are often observed in CVD-diamonds (Jia et al, 1993;Holder et al, 1994). Zhou et al (1996) named this EPR defect HI, and it is most likely composed o f a H atom in the vicinity of a C atom with a dangling bond (Jia et al, 1993;Holder et al, 1994;Zhou et al, 1996). Although Zhou et al (1996) suggest that the HI centre is near the surface, its stability upon annealing at 51200 "C for extended periods of time strongly suggests that the H is not only adsorbed on the crystallite surface (Jia et al, 1993;Talbot-Posonby et al, 1998).…”

Section: Electron Paramagnetic Resonance Measurementsmentioning

confidence: 99%

Infrared, ultraviolet, and electron paramagnetic resonance measurements on presolar diamonds: Implications for optical features and origin

Braatz¹,

Ott²,

Henning³

et al. 2000

Meteorit & Planetary Scien

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Abstract-Infrared (IR) and ultraviolet (UV) absorption spectra were obtained for diamonds from the Allende and Murchison meteorites. In addition, and for the first time, electron paramagnetic resonance spectra were measured. The IR and UV data confirm the suspicion of Russell et al. (1996) that N in presolar diamonds predominantly appears in the form of dispersed N atoms, as is the case for terrestrial type Ib diamonds.In accordance with other observations, our electron paramagnetic resonance measurements suggest a high H content in presolar diamonds. The presolar diamonds most likely originated in a H-rich region, an environment in which nanometer-sized diamonds may be more stable than graphite (Badziag et al., 1990). This adds t o the evidence-previously based mainly on the twin microstructures of presolar diamonds (Daulton et al., 1996) and the absence of graphite with the same isotopic composition as presolar diamonds (Anders and Zinner, 1 9 9 3 t f o r a homogeneous nucleation of presolar diamonds from a gas phase.Based on our results for detection of diamonds in space, we suggest searching for the N-induced IR and UV absorption features of type Ib diamonds. Other characteristic diamond features that could also be used to detect diamonds in space are the (XH,) IR absorption features due to H-coated diamonds, as they are described by Allamandola et af. (1993) and the IR multiphonon absorption features of the diamond lattice. The multiphonon features are very weak (Edwards, 1985), but their intensity increases somewhat with increasing temperature (Collins and Fan, 1954), so perhaps a search for them is not totally hopeless.

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Electron paramagnetic resonance forbidden transitions from hydrogen in polycrystalline diamond films

Cited by 43 publications

References 11 publications

Nitrogen-related dopant and defect states in CVD diamond

Nitrogen-related dopant and defect states in CVD diamond

Hyperfine interactions of narrow-line trityl radical with solvent molecules

Infrared, ultraviolet, and electron paramagnetic resonance measurements on presolar diamonds: Implications for optical features and origin

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