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Wan, Zhimin; Christian, James F.; Anderson, Scott L.

doi:10.1103/physrevlett.69.1352

Cited by 113 publications

(39 citation statements)

References 25 publications

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“…Except for very small atoms and their ions (H and He, but also N), opening the cage enough to allow the atom or its ion to escape requires injecting a lot of energy, typically a few tens of eV (see e.g. Wan et al 1992;Campbell & Rohmund 2000), which is not very different from what is needed to extract a C 2 molecule from the cage (discussed in Sect. 2.3.5).…”

Section: Basic Properties Of Endofullerenesmentioning

confidence: 99%

Interstellar fullerene compounds and diffuse interstellar bands

Omont

2016

A&A

103

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Recently, the presence of fullerenes in the interstellar medium (ISM) has been confirmed and new findings suggest that these fullerenes may possibly form from polycyclic aromatic hydrocarbons (PAHs) in the ISM. Moreover, the first confirmed identification of two strong diffuse interstellar bands (DIBs) with the fullerene, C + 60 , connects the long standing suggestion that various fullerenes could be DIB carriers. These new discoveries justify reassessing the overall importance of interstellar fullerene compounds, including fullerenes of various sizes with endohedral or exohedral inclusions and heterofullerenes (EEHFs). The phenomenology of fullerene compounds is complex. In addition to fullerene formation in grain shattering, fullerene formation from fully dehydrogenated PAHs in diffuse interstellar clouds could perhaps transform a significant percentage of the tail of low-mass PAH distribution into fullerenes including EEHFs. But many uncertain processes make it extremely difficult to assess their expected abundance, composition and size distribution, except for the substantial abundance measured for C + 60 . EEHFs share many properties with pure fullerenes, such as C 60 , as regards stability, formation/destruction and chemical processes, as well as many basic spectral features. Because DIBs are ubiquitous in all lines of sight in the ISM, we address several questions about the interstellar importance of various EEHFs, especially as possible carriers of diffuse interstellar bands. Specifically, we discuss basic interstellar properties and the likely contributions of fullerenes of various sizes and their charged counterparts such as C + 60 , and then in turn: 1) metallofullerenes; 2) heterofullerenes; 3) fulleranes; 4) fullerene-PAH compounds; 5) H 2 @C 60 . From this reassessment of the literature and from combining it with known DIB line identifications, we conclude that the general landscape of interstellar fullerene compounds is probably much richer than heretofore realized. EEHFs, together with pure fullerenes of various sizes, have many properties necessary to be suitably carriers of DIBs: carbonaceous nature; stability and resilience in the harsh conditions of the ISM; existing with various heteroatoms and ionization states; relatively easy formation; few stable isomers; spectral lines in the right spectral range; various and complex energy internal conversion; rich Jahn-Teller fine structure. This is supported by the first identification of a DIB carrier as C + 60 . Unfortunately, the lack of any precise information about the complex optical spectra of EEHFs and most pure fullerenes other than C 60 and about their interstellar abundances still precludes definitive assessment of the importance of fullerene compounds as DIB carriers. Their compounds could significantly contribute to DIBs, but it still seems difficult that they are the only important DIB carriers. Regardless, DIBs appear as the most promising way of tracing the interstellar abundances of various fullerene compounds if the breakthr...

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Section: Basic Properties Of Endofullerenesmentioning

confidence: 99%

Interstellar fullerene compounds and diffuse interstellar bands

Omont

2016

A&A

103

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“…Elemental carbon, including fullerenes, can react with impact-molten silicates to form CO and CO 2 that escape from the Moon, one explanation for the surprisingly small carbon contents of lunar fines and rocks. [75][76][77][78] Also, fullerenes can become destroyed on the Moon by thermal decomposition, [79][80][81] destruction by electrons and ions from the solar wind and cosmic rays [82][83][84][85][86] and become photo-or pressure-polymerized [87,88] in the harsh environment of the lunar regolith. Fullerene multimers, because of their very low solubilities in organic solvents, are very hard to detect.…”

Section: Fullerenes Were Not Found On the Moonmentioning

confidence: 99%

Terrestrial and Extraterrestrial Fullerenes

Heymann

Jenneskens

Jehlička

et al. 2003

Fullerenes, Nanotubes and Carbon Nanostructures

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This paper reviews reports of occurrences of fullerenes in circumstellar media, interstellar media, meteorites, interplanetary dust particles (IDPs), lunar rocks, hard terrestrial rocks from Shunga (Russia), Sudbury (Canada) and Mitov (Czech Republic), coal, terrestrial sediments from the Cretaceous-Tertiary-Boundary and Permian-Triassic-Boundary, fulgurite, ink sticks, dinosaur eggs, and a tree char. The occurrences are discussed in the context of known and postulated processes of fullerene formation, including the suggestion that some natural fullerenes might have formed from biological (algal) remains.

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“…Another technique for the preparation of endohedral fullerene compounds is that of ion implantation (the endohedral species is neutralized on implantation). Endohedral species containing lithium and other alkali metals [15][16][17], the noble gases, He and Ne [18], and nitrogen [19] have been produced by that method.Endohedral compounds of all the noble gases can be prepared by heating fullerenes under high noble gas pressure [1][2][3]20]. Initially, yields of incorporation were approximately 0.1% for He, Ne, Ar and Kr and 0.03% for Xe.…”

mentioning

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mentioning

confidence: 99%

Direct detection and quantitation of He@C₆₀ by ultrahigh-resolution Fourier transform ion cyclotron resonance mass spectrometry

Cooper

Hendrickson

Marshall

et al. 2002

J. Am. Soc. Mass Spectrom.

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In this paper, we report negative ion microelectrospray Fourier-transform ion cyclotron resonance (FT-ICR) mass spectrometry of C 60 samples containing ϳ1% 3 He@C 60 or 4 He@C 60 . Resolving 3 He@C 60 Ϫ and 4 He@C 60 Ϫ from C 60 containing 3 or 4 13 C instead of 12 C atoms is technically challenging, because the target species are present in low relative abundance and are very close in mass. Nevertheless, we achieve baseline resolution of 3 He@C 60 Ϫ from 13 C 3 12 C 57 Ϫ and 4 He@C 60 Ϫ from 13 C 4 12 C 56 Ϫ in single-scan mass spectra obtained in broadband mode without preisolation of the ions of interest. The results constitute the first direct mass spectrometric observation of endohedral helium in a fullerene sample at this (low) level of incorporation. The results also demonstrate the feasibility of determining the extent of He incorporation from the FT-ICR mass spectral peak heights. The present measurements are in agreement with those obtained by the pyrolysis method [1][2][3]. Although limited in sensitivity, the mass spectral method is faster and easier than pyrolysis. [4]) were observed [5,6] soon after the discovery of buckminsterfullerene (C 60 ) [7]. Following the development of the Krätschmer-Huffman method for preparation of fullerenes [8] (an electrical discharge between graphite electrodes in the presence of 0.2 atm of He gas), Smalley and co-workers produced macroscopic quantities of endohedral metallofullerenes in laser vaporization experiments on graphite doped with metal salts [4]. Weiske et al. [9] observed helium within the fragments of C 60 ϩ following high-energy collisions between the cations and the noble gas. Shortly after, the full He@C 60 ϩ adduct was observed [10,11]. Endohedral neon and argon compounds have also been produced by that method [12][13][14]. Another technique for the preparation of endohedral fullerene compounds is that of ion implantation (the endohedral species is neutralized on implantation). Endohedral species containing lithium and other alkali metals [15][16][17], the noble gases, He and Ne [18], and nitrogen [19] have been produced by that method.Endohedral compounds of all the noble gases can be prepared by heating fullerenes under high noble gas pressure [1][2][3]20]. Initially, yields of incorporation were approximately 0.1% for He, Ne, Ar and Kr and 0.03% for Xe. Subsequent experiments showed that reiterations of the labeling procedure resulted in higher yields of incorporation (ϳ1%) [21]. 3 He@C 60 , an NMR-active molecule, has also been prepared by that method [21,22]. Recent results have shown that the presence of KCN catalyzes the incorporation of noble gas, giving higher yields of incorporation (ϳ1%) in a single labeling experiment [23]. It is also known that He is trapped inside fullerenes (at about 1 ppm of empty fullerene) prepared by the Krätschmer-Huffman procedure [1,8]. In a recent finding, it was shown that fullerenes extracted from the Allende and Murchison meteorites contained endohedral helium [24]. The 3 He/ 4 He ratio in those fullerenes ...

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Collision ofLi+andNa+with
Zhimin Wan
¹
,
James F. Christian
²
,
Scott L. Anderson
³

Cited by 113 publications

References 25 publications

Interstellar fullerene compounds and diffuse interstellar bands

Interstellar fullerene compounds and diffuse interstellar bands

Terrestrial and Extraterrestrial Fullerenes

Direct detection and quantitation of He@C₆₀ by ultrahigh-resolution Fourier transform ion cyclotron resonance mass spectrometry

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Collision ofLi+andNa+withZhimin Wan1, James F. Christian2, Scott L. Anderson3

Cited by 113 publications

References 25 publications

Interstellar fullerene compounds and diffuse interstellar bands

Interstellar fullerene compounds and diffuse interstellar bands

Terrestrial and Extraterrestrial Fullerenes

Direct detection and quantitation of He@C60 by ultrahigh-resolution Fourier transform ion cyclotron resonance mass spectrometry

Contact Info

Product

Resources

About

Collision ofLi+andNa+with
Zhimin Wan
¹
,
James F. Christian
²
,
Scott L. Anderson
³

Direct detection and quantitation of He@C₆₀ by ultrahigh-resolution Fourier transform ion cyclotron resonance mass spectrometry