Detection of buckminsterfullerene emission in the diffuse interstellar medium

Berné, O.; Cox, N. L. J.; Mulas, G.; Joblin, C.

doi:10.1051/0004-6361/201630325

Cited by 55 publications

(67 citation statements)

References 39 publications

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“…We can now confirm that C 60 is indeed widespread and abundant in space. Since the first unambiguous detection of all IR active vibrational modes of C 60 in the Spitzer-IRS spectrum of the planetary nebula (PN) Tc 1 at 7.0, 8.5, 17.4, and 18.9 µm [3], the same spectral features have been found in a variety of evolved star environments (see Section 3), as well as in Reflection Nebulae RNe; see e.g., [4,5], the diffuse ISM [6], and young stellar objects and Herbig Ae/Be stars [7]. Recently, laboratory experiments and astronomical observations have confirmed the identification of two strong (and 3 weaker) diffuse interstellar bands DIBs; see [8] as due to electronic transitions of the C + 60 cation see e.g., [9][10][11][12], and references therein.…”

Section: Introductionmentioning

confidence: 76%

The Formation of Fullerenes in Planetary Nebulae

et al. 2018

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In the last decade, fullerenes have been detected in a variety of astrophysical environments, with the majority being found in planetary nebulae. Laboratory experiments have provided us with insights into the conditions and pathways that can lead to fullerene formation, but it is not clear precisely what led to the formation of astrophysical fullerenes in planetary nebulae. We review some of the available evidence, and propose a mechanism where fullerene formation in planetary nebulae is the result of a two-step process where carbonaceous dust is first formed under unusual conditions; then, the fullerenes form when this dust is being destroyed.

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Section: Introductionmentioning

confidence: 76%

The Formation of Fullerenes in Planetary Nebulae

et al. 2018

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“…By the PN phase, the stars have shed most of their original mass in outflowing winds, leaving behind a fading white dwarf. Subsequent detections of C 60 were made in the ISM (Sellgren et al 2010), other galactic and extra-galactic PNs (García-Hernández et al 2010), H-rich RCB stars (García-Hernández et al 2011), proto-PNs (e.g., Zhang & Kwok 2011), YSOs (Roberts et al 2012), and diffuse clouds (Berné et al 2017). The C 70 fullerene was also identified in a few PNs (Cami et al 2010;, and the C 60 + cation has been suggested to account for a few of the diffuse interstellar bands, also referred to as the "DIBs" (Campbell et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Formation of Interstellar C₆₀ from Silicon Carbide Circumstellar Grains

Bernal

Haenecour

Zega

et al. 2019

ApJL

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We have conducted laboratory experiments with analog crystalline silicon carbide (SiC) grains using transmission electron microscopy (TEM) and electron energy-loss spectroscopy (EELS). The 3C polytype of SiC was used-the type commonly produced in the envelopes of asymptotic giant branch (AGB) stars. We rapidly heated small (∼50 nm) synthetic SiC crystals under vacuum to ∼1300 K and bombarded them with 150 keV Xe ions. TEM imaging and EELS spectroscopic mapping show that such heating and bombardment leaches silicon from the SiC surface, creating layered graphitic sheets. Surface defects in the crystals were found to distort the six-membered rings characteristic of graphite, creating hemispherical structures with diameters matching that of C 60. Such nonplanar features require the formation of five-membered rings. We also identified a circumstellar grain, preserved inside the Murchison meteorite, that contains the remnant of an SiC core almost fully encased by graphite, contradicting long-standing thermodynamic predictions of material condensation. Our combined laboratory data suggest that C 60 can undergo facile formation from shock heating and ion bombardment of circumstellar SiC grains. Such heating/bombardment could occur in the protoplanetary nebula phase, accounting for the observation of C 60 in these objects, in planetary nebulae (PNs) and other interstellar sources receiving PN ejecta. The synthesis of C 60 in astronomical sources poses challenges, as the assembly of 60 pure carbon atoms in an H-rich environment is difficult. The formation of C 60 from the surface decomposition of SiC grains is a viable mechanism that could readily occur in the heterogeneous, hydrogen-dominated gas of evolved circumstellar shells.

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“…The detections of interstellar C 60 and C 70 and their cations have also been reported based on their characteristic infrared (IR) emission features, e.g., the 7. 0, 8.45, 17.3 and 18.9 µm features of C 60 (Cami et al 2010, Sellgren et al 2010, Berné et al 2017, García-Hernández et al 2010) and the 6.4, 7.1, 8.2 and 10.5 µm features of C + 60 (Berné et al 2013, Strelnikov et al 2015. In addition, C + 60 has also been suggested as a promising carrier of the mysterious diffuse interstellar bands at 9348.4, 9365.2, 9427.8, 9577.0, and 9632.1Å (Foing & Ehrenfreund 1994, Campbell et al 2015, 2016, Walker et al 2015.…”

Section: Introductionmentioning

confidence: 99%

On Graphene in the Interstellar Medium

Chen

Zhang

2017

ApJ

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The possible detection of C 24 , a planar graphene, recently reported in several planetary nebulae by García-Hernández et al. (2011 inspires us to explore whether and how much graphene could exist in the interstellar medium (ISM) and how it would reveal its presence through its ultraviolet (UV) extinction and infrared (IR) emission. In principle, interstellar graphene could arise from the photochemical processing of polycyclic aromatic hydrocarbon (PAH) molecules which are abundant in the ISM through a complete loss of their hydrogen atoms, and/or from graphite which is thought to be a major dust species in the ISM through fragmentation caused by grain-grain collisional shattering. Both quantum-chemical computations and laboratory experiments have shown that the exciton-dominated electronic transitions in graphene cause a strong absorption band near 2755Å. We calculate the UV absorption of graphene and place an upper limit of ∼ 5 ppm of C/H (i.e., ∼ 1.9% of the total interstellar C) on the interstellar graphene abundance. We also model the stochastic heating of graphene C 24 in the ISM, excited by single starlight photons of the interstellar radiation field and calculate its IR emission spectra. We also derive the abundance of graphene in the ISM to be < 5 ppm of C/H by comparing the model emission spectra with that observed in the ISM.

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Detection of buckminsterfullerene emission in the diffuse interstellar medium

Cited by 55 publications

References 39 publications

The Formation of Fullerenes in Planetary Nebulae

The Formation of Fullerenes in Planetary Nebulae

Formation of Interstellar C₆₀ from Silicon Carbide Circumstellar Grains

On Graphene in the Interstellar Medium

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Detection of buckminsterfullerene emission in the diffuse interstellar medium

Cited by 55 publications

References 39 publications

The Formation of Fullerenes in Planetary Nebulae

The Formation of Fullerenes in Planetary Nebulae

Formation of Interstellar C60 from Silicon Carbide Circumstellar Grains

On Graphene in the Interstellar Medium

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Formation of Interstellar C₆₀ from Silicon Carbide Circumstellar Grains