Paucity of Tagish Lake-like parent bodies in the Asteroid Belt and among Jupiter Trojans

Vernazza, Pierre; Fulvio, D.; Brunetto, R.; Emery, Joshua P.; Dukes, C. A.; Cipriani, F.; Witasse, Olivier; Schaible, Micah J.; Zanda, B.; Strazzulla, G.; Baragiola, R. A.

doi:10.1016/j.icarus.2013.04.019

Cited by 86 publications

(74 citation statements)

References 61 publications

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“…The two strongest olivine peaks also undergo this band shift; this effect has already been described on Tagish Lake (Vernazza et al 2013) and Allende (Brunetto et al 2014). The latter discussed the shift amplitude as a function of the peak intensity, which is also observed here: the stronger the band intensity, the bigger the band shift.…”

Section: Phyllosilicatessupporting

confidence: 84%

“…Predictions for these bodies suggested a possible limited effect on the spectral slope (Pieters et al 2000), or even an opposite effect defined as blueing of the slope (Nesvorný et al 2005). Contradictory results have also been obtained in laboratory SpWe ion irradiation experiments performed on primitive materials: spectral reddening on Allende (Lazzarin et al 2006;Brunetto et al 2014) and Frontier Mountain 95002 (Lazzarin et al 2006), and blueing on asphaltite (Moroz et al 2004a) and Tagish Lake meteorite (Vernazza et al 2013) have been observed. Tagish Lake also shows a significant spectral flattening after pulse laser irradiation Article published by EDP Sciences A41, page 1 of 9 (Hiroi et al 2013).…”

Section: Introductionmentioning

confidence: 61%

“…We chose to prepare pellets because in our experimental setup samples are held vertically. Several authors have used pellets to irradiate meteorites (e.g., Hiroi et al 2004;Vernazza et al 2013, and references therein). Irradiation was performed in a vacuum chamber and we placed the samples under dry vacuum between irradiation sessions and reflectance measurements.…”

Section: Experimental Methodsmentioning

confidence: 99%

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Ion irradiation of the Murchison meteorite: Visible to mid-infrared spectroscopic results

Lantz

Brunetto

Barucci

et al. 2015

A&A

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Aims. The goal of this study is to simulate space weathering processes on primitive bodies. We use ion implantation as a simulation of solar wind irradiation, which has been suggested by several authors to be the major component of space weathering on main belt asteroids. The laboratory analogs we irradiate and analyze are carbonaceous chondrites; we started the study with the Allende CV meteorite and in this companion paper we present results on the Murchison CM meteorite. Methods. We performed irradiations on pressed pellets of Murchison with 40 keV He+ and Ar + ions using fluences up to 3 × 10 16 ions/cm 2 . Reflectance spectra were acquired ex situ before and after irradiation in the visible to mid-infrared range (0.4-16 µm). A Raman analysis was also performed to investigate the modifications of the aromatic carbonaceous component. Results. Our results indicate that spectral variations after irradiation within the visible range are smaller than spectral variations due to sample grain size or viewing geometry of the Murchison meteorite. The aqueous alteration band profile near 3 µm changes after irradiation, as adsorbed water is removed, and phyllosilicates are affected. Raman spectroscopy highlights the insoluble organic matter (IOM) modification under irradiation. We observe a shift of the silicates band at 9.9 µm, probably due to a preferential loss of Mg (compared to Fe, the lighter Mg is more easily sputtered backward) and/or amorphization of Mg-rich materials. We compare our results to previous experiments on organic-rich materials (like asphaltite or carbonaceous chondrites), and on ordinary chondrites and olivine grains. We find that the reddening/darkening trend observed on silicate-rich surfaces is not valid for all carbonaceous chondrites, and that the spectral modifications after irradiation are a function of the initial albedo.

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Section: Phyllosilicatessupporting

confidence: 84%

Section: Introductionmentioning

confidence: 61%

Section: Experimental Methodsmentioning

confidence: 99%

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Ion irradiation of the Murchison meteorite: Visible to mid-infrared spectroscopic results

Lantz

Brunetto

Barucci

et al. 2015

A&A

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“…Milliken and Rivkin (2009) show that a 6-14 µm spectrum of Ceres obtained from the Kuiper Airborne Observatory by Cohen et al (1998) is well-matched by linear-mixing models that were developed for the 2-4 µm spectral region and that include brucite (MgOH 2 ) and cronstedtite (Fe-rich serpentine). Vernazza et al (2013) note that 368 Haidea is the only asteroid in the Spitzer Space Telescope (SST) spectral database (of 87 asteroids searched) that shows a single emissivity peak in the Si-O stretch region. The spectrum of Haidea is well-matched in the visible-NIR and the mid-IR by the Tagish Lake meteorite, which is a heavily hydrated meteorite (Zolensky et al, 2002), from which Vernazza et al conclude that Haidea too is hydrated.…”

Section: This Volume)mentioning

confidence: 99%

Astronomical Observations of Volatiles on Asteroids

Rivkin¹,

Campins²,

Emery³

et al. 2015

Asteroids IV

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We have long known that water and hydroxyl are important components in meteorites and asteroids. However, in the time since the publication of Asteroids III, evolution of astronomical instrumentation, laboratory capabilities, and theoretical models have led to great advances in our understanding of H 2 O/OH on small bodies, and spacecraft observations of the Moon and Vesta have important implications for our interpretations of the asteroidal population. We begin this chapter with the importance of water/OH in asteroids, after which we will discuss their spectral features throughout the visible and near-infrared. We continue with an overview of the findings in meteorites and asteroids, closing with a discussion of future opportunities, the results from which we can anticipate finding in Asteroids V. Because this topic is of broad importance to asteroids, we also point to relevant in-depth discussions elsewhere in this volume.1 Water ice sublimation and processes that create, incorporate, or deliver volatiles to the asteroid belt Accretion/Solar system formation 1.1The concept of the "snow line" (also known as "water-frost line") is often used in discussing the water inventory of small bodies in our solar system. The snow line is the heliocentric distance at which water ice is stable enough to be accreted into planetesimals. The placement of the snow line has varied in different models. A location just inside Jupiter helps explain the greater mass of the giant planets as they accrete a larger fraction of the mass in the solar nebula. Although the location of the snow line before and during planet formation is uncertain, some studies show it may have fallen within the asteroid belt (Lunine, 2006). The location of the snow line in our solar system coinciding with the asteroid belt is consistent with observations of disks around other stars (e.g., Su et al., 2013), where planetesimal rings tend to coincide with the snow line around those stars. However, it seems the relatively simple concept of a static snow line requires revisions in light of new results on several fronts. For instance, the snow line likely moved with time as the Sun's luminosity changed early in solar system history (e.g., Martin and Livio, 2012). Even though there is no agreement on the details of planetesimal formation and growth, some models favor the growth of ~100 km-scale planetesimals directly from cm-scale pieces Cuzzi et al., 2010; for a dissenting view see Weidenschilling, 2011). Hence, the timing of those assemblies as conditions change could have a strong influence on the amount of radioactive elements present in a planetesimal's interior and on its rock-to-ice ratio, further complicating the concept of a snow line. Recent observations also point to a more complex picture. For example, the concept of an asteroid-comet continuum, where there is no clear boundary between primitive asteroids and cometary nuclei (e.g., Gounelle, 2011) is gaining support and is consistent with the intermittent cometary behavior of some main belt and near-E...

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“…Albedos have been used to identify candidate V-type asteroids throughout the Main Belt that have been subsequently observed spectroscopically to confirm their taxonomic type (Hardersen et al 2014). Moreover, objects with extremely low albedos (p V ∼0.02) in the Main Belt have been identified as the possible progenitors of the Tagish Lake meteorite, one of the darkest and most primitive carbonaceous chondrites ever found (Vernazza et al 2013).…”

Section: Taxonomy Albedo and Beamingmentioning

confidence: 99%

Space-Based Thermal Infrared Studies of Asteroids

Mainzer¹,

Usui²,

Trilling³

2015

Asteroids IV

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Large-area surveys operating at mid-infrared wavelengths have proven to be a valuable means of discovering and characterizing minor planets. Through the use of radiometric models, it is possible to derive physical properties such as diameters, albedos, and thermal inertia for large numbers of objects. Modern detector array technology has resulted in a significant improvement in spatial resolution and sensitivity compared with previous generations of spacebased infrared telescopes, giving rise to a commensurate increase in the number of objects that have been observed at these wavelengths. Space-based infrared surveys of asteroids therefore offer an effective method of rapidly gathering information about small body populations orbital and physical properties. The AKARI, WISE/NEOWISE, Spitzer, and Herschel missions have significantly increased the number of minor planets with well-determined diameters and albedos.

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Paucity of Tagish Lake-like parent bodies in the Asteroid Belt and among Jupiter Trojans

Cited by 86 publications

References 61 publications

Ion irradiation of the Murchison meteorite: Visible to mid-infrared spectroscopic results

Ion irradiation of the Murchison meteorite: Visible to mid-infrared spectroscopic results

Astronomical Observations of Volatiles on Asteroids

Space-Based Thermal Infrared Studies of Asteroids

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