Studies of proton-irradiated cometary-type ice mixtures

Moore, M. H.; Donn, B.; Khanna, R. K.; A’Hearn, Michael F.

doi:10.1016/0019-1035(83)90236-1

Cited by 239 publications

(118 citation statements)

References 24 publications

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“…In many cases, an absorption band results which is remarkably similar to that seen in the interstellar medium in both proÐle and peak position (Moore et al 1983 ;Lacy et al 1984 ;Grim & Greenberg 1987 ;Tegler et al 1993 ;Schutte & Greenberg 1997 ;Demyk et al 1998 ;Palumbo et al 2000 ;Hudson & Moore 2000). Here we report irradiation experiments using ion bombardment of and ices.…”

Section: Introductionmentioning

confidence: 55%

Hydrogen Isotopic Substitution Studies of the 2165 Wavenumber (4.62 Micron) “XCN” Feature Produced by Ion Bombardment

Palumbo

Pendleton

Strazzulla

2000

ApJ

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The interstellar 4.62 km absorption band, commonly seen toward embedded protostellar objects, has not yet been unambiguously identiÐed ; here we report new results which further elucidate the components of the band carrier, which is often referred to in the literature as the "" XCN ÏÏ band due to previous implications of carbon and nitrogen. If the atmosphere of the early Earth was not overly reducing, as some studies indicate, production of prebiotic molecules containing the cyanogen bond would have been difficult. In that case, CN-bearing molecules, necessary for the origin of life, may have come primarily from extraterrestrial sources, and the interstellar medium may be an important source of those molecules. Laboratory studies show that energetic processing of ice mixtures containing H, C, N, and O atoms readily reproduce a band similar in peak position and proÐle to that seen in the interstellar spectra. Earlier isotopic labeling experiments clearly identiÐed carbon, nitrogen, and oxygen as active participants of the XCN species. In this paper, results of ion bombardment of and CH 3 OH : N 2 ices are presented. A shift in band position resulting from deuterium substitution demon-CD 3 OD : N 2 strates that hydrogen is also a component of the carrier in the laboratory-produced 4.62 km band. Irradiation of ices through ion bombardment allows the testing of mixtures which include a possible N 2 , source of the available nitrogen in dense cloud ices that cannot be probed through UV photolysis experiments.

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Section: Introductionmentioning

confidence: 55%

Hydrogen Isotopic Substitution Studies of the 2165 Wavenumber (4.62 Micron) “XCN” Feature Produced by Ion Bombardment

Palumbo

Pendleton

Strazzulla

2000

ApJ

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“…Laboratory experiments show that long-term irradiation of astrophysical ice mixtures (with the presence of simple hydrocarbons and nitrogen) results in the selective loss of hydrogen and the formation of an irradiation mantle of carbon residues (Moore et al 1983;Johnson et al 1984;Strazzulla et al 1991). They also show that as the radiation dose increases, more complex polymers form, that are poor in hydrogen content, and an initially neutral-colored and high-albedo ice becomes red as the albedo in the visible decreases.…”

Section: Discussionmentioning

confidence: 99%

The spectrum of (136199) Eris between 350 and 2350 nm: results with X-Shooter

Álvarez-Candal

Pinilla-Alonso

Licandro

et al. 2011

A&A

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Context. X-Shooter is the first second-generation instrument for the ESO-Very Large Telescope. It is a spectrograph covering the entire 300−2480 nm spectral range at once with a high resolving power. These properties enticed us to observe the well-known transNeptunian object (136199) Eris during the science verification of the instrument. The target has numerous absorption features in the optical and near-infrared domain that have been observed by different authors, showing differences in these features' positions and strengths. Aims. Besides testing the capabilities of X-Shooter to observe minor bodies, we attempt to constrain the existence of super-volatiles, e.g., CH 4 , CO and N 2 , and in particular we try to understand the physical-chemical state of the ices on Eris' surface. Methods. We observed Eris in the 300−2480 nm range and compared the newly obtained spectra with those available in the literature. We identified several absorption features, measured their positions and depth, and compare them with those of the reflectance of pure methane ice obtained from the optical constants of this ice at 30 K to study shifts in these features' positions and find a possible explanation for their origin. Results. We identify several absorption bands in the spectrum that are all consistent with the presence of CH 4 ice. We do not identify bands related to N 2 or CO. We measured the central wavelengths of the bands and compared to those measured in the spectrum of pure CH 4 at 30 K finding variable spectral shifts. Conclusions. Based on these wavelength shifts, we confirm the presence of a dilution of CH 4 in other ice on the surface of Eris and the presence of pure CH 4 that is spatially segregated. The comparison of the centers and shapes of these bands with previous works suggests that the surface is heterogeneous. The absence of the 2160 nm band of N 2 can be explained if the surface temperature is below 35.6 K, the transition temperature between the alpha and beta phases of this ice. Our results, including the reanalysis of data published elsewhere, point to a heterogeneous surface on Eris.

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“…This results in the selective loss of hydrogen and the formation of an "irradiation mantle" of carbon residues (Moore et al 1983;Johnson et al 1984;Strazzulla & Johnson 1991). This process makes that an initially neutral color and high albedo ice becomes redish.…”

Section: Discussionmentioning

confidence: 99%

Infrared spectroscopy of the largest known trans-Neptunian object 2001 KX$_\mathsf{76}$

Licandro

Ghinassi

Testi

2002

A&A

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Abstract. We report complete near-infrared (0.9-2.4 µm) spectral observations of the largest know trans-Neptunian objects (TNO) 28976 = 2001 KX76 taken in two different nights using the new Near Infrared Camera Spectrometer (NICS) attached to the 3.56 m Telescopio Nazionale Galileo (TNG). The spectra are featureless and correspond to a neutral colored object. Our observations indicate that the surface of 2001 KX76 is probably highly evolved due to long term irradiation, and that collisional resurfacing processes have not played an important role in its evolution.

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Studies of proton-irradiated cometary-type ice mixtures

Cited by 239 publications

References 24 publications

Hydrogen Isotopic Substitution Studies of the 2165 Wavenumber (4.62 Micron) “XCN” Feature Produced by Ion Bombardment

Hydrogen Isotopic Substitution Studies of the 2165 Wavenumber (4.62 Micron) “XCN” Feature Produced by Ion Bombardment

The spectrum of (136199) Eris between 350 and 2350 nm: results with X-Shooter

Infrared spectroscopy of the largest known trans-Neptunian object 2001 KX$_\mathsf{76}$

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