Surface C–H stretching features on meteoritic nanodiamonds

Jones, A. P.; D’Hendecourt, L.; Sheu, Sheh Yi; Chang, Huan‐Cheng; Cheng, Caleb; Hill, H. G. M.

doi:10.1051/0004-6361:20031708

Cited by 50 publications

(63 citation statements)

References 24 publications

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“…Typical sizes for the diamonds in HAEBE stars (∼50-100 nm) are 2 orders of magnitude larger than the nanodiamonds found in our solar system (e.g. Jones et al 2004). …”

Section: Conclusion and Discussionmentioning

confidence: 56%

“…Guillois et al 1999;Sheu et al 2002;Jones et al 2004;Mutschke et al 2004). Currently, the astronomical spectra can be reproduced from the absorption spectra of films of hydrogen-terminated diamonds (Sheu et al 2002).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…This process may have been important for planet formation, as the the radioactive decay of 60 Fe into 60 Ni was an important heat source for the early planetary melting and differentiation and keeping asteroids thermally active for much longer than would be possible from the decay of 26 Al alone. Infrared spectroscopy has shown that solar-system diamonds contain N and O, probably in chemical functional groups on their surfaces (Lewis et al 1989;Mutschke et al 1995;Andersen et al 1998;Jones et al 2004). However, the similarity of C-and N-isotopes of these diamonds and the solar system as a whole supports the idea that not all solar-system diamonds originate from supernovae and that the supernova contribution to the diamonds in our own solar system is probably not very large.…”

Section: In-situ Formation or Extraneous Origin?mentioning

confidence: 99%

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A survey for nanodiamond features in the 3 micron spectra of Herbig Ae/Be stars

Acke¹,

Ancker

2006

A&A

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Aims. We have carried out a survey of 60 Herbig Ae/Be stars in the 3 micron wavelength region in search for the rare spectral features at 3.43 and 3.53 micron. These features have been attributed to the presence of large, hot, hydrogen-terminated nanodiamonds. Only two Herbig Ae/Be stars, HD 97048 and Elias 3−1 are known to display both these features. Methods. We have obtained medium-resolution spectra (R ∼ 2500) with the ESO near-IR instrument ISAAC in the 3.15−3.65 micron range.Results. In our sample, no new examples of sources with prominent nanodiamond features in their 3 micron spectra were discovered. Less than 4% of the Herbig targets show the prominent emission features at 3.43 and/or 3.53 µm. Both features are detected in our spectrum of HD 97048. We confirm the detection of the 3.53 µm feature and the non-detection of the 3.43 µm feature in MWC 297. Furthermore, we report tentative 3.53 µm detections in V921 Sco, HD 163296 and T CrA. The sources which display the nanodiamond features are not exceptional in the group of Herbig stars with respect to disk properties, stellar characteristics, or disk and stellar activity. Moreover, the nanodiamond sources are very different from each other in terms of these parameters. We do not find evidence for a recent supernova in the vicinity of any of the nanodiamond sources. We have analyzed the PAH 3.3 µm feature and the Pfund δ hydrogen emission line, two other spectral features which occur in the 3 micron wavelength range. We reinforce the conclusion of previous authors that flared-disk systems display significantly more PAH emission than self-shadowed-disk sources. The Pf δ line detection rate is higher in self-shadowed-disk sources than in the flareddisk systems. Conclusions. We discuss the possible origin and paucity of the (nano)diamond features in Herbig stars. Different creation mechanisms have been proposed in the literature, amongst others in-situ and supernova-induced formation. Our data set is inconclusive in proving or disproving either formation mechanism.

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“…Typical sizes for the diamonds in HAEBE stars (∼50-100 nm) are 2 orders of magnitude larger than the nanodiamonds found in our solar system (e.g. Jones et al 2004). …”

Section: Conclusion and Discussionmentioning

confidence: 56%

Section: Conclusion and Discussionmentioning

confidence: 99%

Section: In-situ Formation or Extraneous Origin?mentioning

confidence: 99%

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A survey for nanodiamond features in the 3 micron spectra of Herbig Ae/Be stars

Acke¹,

Ancker

2006

A&A

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“…They can also form in shocks, as indicated by their discovery in meteorites subjected to high pressures (Lewis et al 1987). Laboratory experiments show that most of the emission appears in emission bands given the very low value of Q abs at other wavelengths (diamond is well-known to be transparent in the IR), but, on the other hand, the presence of emission bands at 3.43 µm and 3.53 µm is clear for large diamond particles only and would not appear for very small ones (Jones et al 2004), so that we no longer predict the presence of such spectral features in NGC 1068.…”

Section: Nano-diamonds: Interesting Candidatesmentioning

confidence: 97%

Near-infrared adaptive optics dissection of the core of NGC 1068 with NAOS-CONICA

Gratadour

Rouan²,

Mugnier

et al. 2006

A&A

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We present an update analysis of recent near-infrared adaptive optics observations of NGC 1068 obtained with NAOS-CONICA at VLT/UT4. Ks, L and M bands images were deconvolved using MISTRAL, a regularized algorithm based on a maximum a posteriori estimation of the object. Two regularization methods, one including a new maximum likelihood estimation of the object Power Spectral Density, and an edge preserving one, have been tested and converge to consistent results. The deconvolved images show a coherent evolution of the IR emission from 2.2 to 4.8 µm. Deconvolution brings new elements: a) it strengthens the very peculiar nature of the four parallel elongated nodules previously discovered along the jet, which appear unresolved perpendicular to their long axis; b) it underlines the strong correlation between UV clouds and IR features, and c) it provides a more accurate multi-wavelength registration of the actual active nucleus. The overall aspect of the central 1 ×1 IR emission seems to point to the jet as a major mechanism to shape the NLR. For each identified structure, we derive a color temperature now based on three bands (M, L and K), before and after deconvolution, confirming the need for clumps of dust at unexpectedly high and almost constant temperature (about 500 K) up to 70 pc north of the nucleus. We explore several mechanisms to explain the color temperature and show that shocks, induced for instance by the interaction of the jet with a giant cloud, is unlikely to be the dominating mechanism to heat the dust. We detail our model of transient heating of Very Small Grains and show that it can provide a consistent explanation of the K, L, M colors and their lack of variation with distance when 0.6 nm diamond-like grains are heated by 4 to 8 eV UV photons. However, we do not exclude the possibility that part of the excitation could come from shocks. At Ks, deconvolution reinforces the previous claim that the central core is partially resolved along the N-S direction: the best fit to our data is an elliptical Gaussian extended along PA = −16 with a 2.1 pc FWHM along this direction. This result agrees with the predictions of the radiative transfer model we previously developed to interpret the spectroscopic behavior at K, and is consistent with VLTI/VINCI measurements. Several questions are raised by this study: a) is the jet dominant in shaping the NLR of this AGN? b) what is the real state of the dust in the environment of the core; c) is the simple doughnut torus model able to explain IR emission of the central source with a morphology that appears increasingly complex at small scale?

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“…Clearly, for such materials to explain the IR emission bands their sizes would have to be comparable to those invoked for PAHs or very small carbon grains (e.g., see Jones & d'Hendecourt 2000, for a calculation of typical nanodiamond temperatures in the ISM). These IR emission features could also arise from the amorphous, carbonaceous outer layers on nanodiamonds (Jones & d'Hendecourt 2000), though measurements of the IR spectra of chemically processed, meteoritic diamonds do not resemble the above-mentioned bands (Mutschke etal 1995;Sheu et al 2002;Jones et al 2004). …”

Section: Componentmentioning

confidence: 99%

Dust destruction in the ISM: a re-evaluation of dust lifetimes

Jones

Nuth

2011

A&A

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200

224

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Context. There is a long-standing conundrum in interstellar dust studies relating to the discrepancy between the time-scales for dust formation from evolved stars and the apparently more rapid destruction in supernova-generated shock waves. Aims. We re-examine some of the key issues relating to dust evolution and processing in the interstellar medium. Methods. We use recent and new constraints from observations, experiments, modelling and theory to re-evaluate dust formation in the interstellar medium (ISM). Results. We find that the discrepancy between the dust formation and destruction time-scales may not be as significant as has previously been assumed because of the very large uncertainties involved. Conclusions. The derived silicate dust lifetime could be compatible with its injection time-scale, given the inherent uncertainties in the dust lifetime calculation. The apparent need to re-form significant quantities of silicate dust in the tenuous interstellar medium may therefore not be a strong requirement. Carbonaceous matter, on the other hand, appears to be rapidly recycled in the ISM and, in contrast to silicates, there are viable mechanisms for its re-formation in the ISM.

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Surface C–H stretching features on meteoritic nanodiamonds

Cited by 50 publications

References 24 publications

A survey for nanodiamond features in the 3 micron spectra of Herbig Ae/Be stars

A survey for nanodiamond features in the 3 micron spectra of Herbig Ae/Be stars

Near-infrared adaptive optics dissection of the core of NGC 1068 with NAOS-CONICA

Dust destruction in the ISM: a re-evaluation of dust lifetimes

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