The nature of Low-Albedo asteroids from 3-μm multi-color photometry

Lebofsky, L. A.; Jones, Tina; Owensby, P. D.; Feierberg, Michael A.; Consolmagno, G. J.

doi:10.1016/0019-1035(90)90003-r

Cited by 52 publications

(38 citation statements)

References 17 publications

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“…We This analysis indicates that the percentage of hydrated asteroids decreases with the size and that the aqueous alteration process dominates for primitive asteroids with 50 < D < 240 km, as claimed previously in the literature (Howell et al, 2001;Jones et al, 1990;Vilas & Sykes, 1996). In particular, the asteroids larger than 100 km are strongly affected by the aqueous alteration process, as more than half of them present absorption bands associated with hydrated silicates.…”

Section: Aqueous Alteration and Asteroids Diametersupporting

confidence: 83%

“…The most prominent and unambiguous indicator 5 of hydratation is the 3 µm band (Lebofsky, 1980;Jones et al, 1990;Rivkin et al, 2002;Vilas, 1994Vilas, , 2005Howell et al, 2011;Takir & Emery, 2012), associated with free water molecules, and to OH ion bounded in the mineral crystal lattice; while in the visible range there are several bands, centered around 0.43 µm, 0.60-0.65 µm, 0.70 µm and 0.80-0.90 µm, attributed to charge transfer transitions in oxidized iron (Vilas et al, 1993(Vilas et al, , 1994Vilas, 1994;Barucci et al, 1998;Fornasier et al, 1999).…”

Section: Introductionmentioning

confidence: 99%

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Aqueous alteration on main belt primitive asteroids: Results from visible spectroscopy

Fornasier

Lantz

Barucci

et al. 2014

Icarus

114

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This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. The aqueous alteration is particularly important for unraveling the processes occurring during the earliest times of the Solar System history, as it can give information both on the asteroids thermal evolution and on the localization of water sources in the asteroid belt. To investigate this process, we present reflected light spectral observations in the visible region (0.4-0.94 µm) of 80 asteroids belonging to the primitive classes C (prevalently), G, F, B and P, following the Tholen (1984) classification scheme. We find that about 65 % of the C-type and all the G-type asteroids investigated reveal features suggesting the presence of hydrous materials, mainly a band centered around 0.7 µm, while we do not find evidence of hydrated materials in the other low albedo asteroids (B, F, and P) investigated. We combine the present observations with the visible spectra of asteroids available in the literature for a total of 600 primitive main belt asteroids. We analyze all these spectra in a similar way to characterize the absorption band parameters (band center, depth and width) and spectral slope, and to look for possible correlations between the aqueous alteration process and the asteroids taxonomic classes, orbital elements, heliocentric distances, albedo and sizes. Our analysis shows that the aqueous alteration sequence starts from the P-type objects, practically unaltered, and increases through the P → F → B → C → G asteroids, these last being widely aqueous altered, strengthening thus the results previously obtained by Vilas (1994). Around 50% of the observed C-type asteroids show absorption feature in the visible range due to hydrated silicates, implying that more than ∼ 70% of them will have a 3 µm absorption band and thus hydrated minerals on their surfaces, based on correlations between those two absorptions (Howell et al., 2011).1 Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier February 4, 2014We find that the aqueous alteration process dominates in primitive asteroids located between 2.3 and 3.1 AU, that is at smaller heliocentric distances than previously suggested by Vilas et al. (1993). The percentage of hydrated asteroids is strongly correlated with their size. The aqueous alteration process is less effective for bodies smaller than 50 km, while it dominates in the 50-240 km sized primitive asteroids. No correlation is found between the aqu...

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Section: Aqueous Alteration and Asteroids Diametersupporting

confidence: 83%

Section: Introductionmentioning

confidence: 99%

Aqueous alteration on main belt primitive asteroids: Results from visible spectroscopy

Fornasier

Lantz

Barucci

et al. 2014

Icarus

114

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“…The correlation for 70 C-complex objects is shown in the right two columns. In cases where insufficient data exists to determine the Bus-DeMeo taxonomic class, we include Tholen C, B, F, and G taxonomic classes as well as CP and PC, but not those classified as P. The data sources from this table are Zellner et al (1985), Lazzaro et al (2004), Sawyer (1991), Vilas (1994), , Lebofsky et al (1990), Feierberg et al (1985, Rivkin et al (2000Rivkin et al ( , 2002Rivkin et al ( , 2012, Fornasier et al (2011, 2014 Table 3: While a formal taxonomy has not yet been developed for objects in the 3-µm spectral region, the major groupings in such a taxonomy are already apparent. Presented here are the classes as defined by Takir et al (2012) and Rivkin et al (2012), with type examples and possible compositions for each group (also from these cited works).…”

Section: Discussionmentioning

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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“…The martian satellite spectra are the combined data of Murchie and Erard (1996) and this work for Phobos and Murchie et al (1991) and this work for Deimos. The asteroid spectra in this figure are compilations of data from the Eight Color Asteroid Survey (Zellner et al 1985), the 52-Color Survey (Bell et al 1988), and 3-µm data from Jones et al (1990), Lebofsky et al (1990), andHowell (1995) as resampled by Merényi et al (1997).…”

Section: Comparison With Other Bodiesmentioning

confidence: 99%

Near-Infrared Spectrophotometry of Phobos and Deimos

Rivkin

2002

Icarus

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The nature of Low-Albedo asteroids from 3-μm multi-color photometry

Cited by 52 publications

References 17 publications

Aqueous alteration on main belt primitive asteroids: Results from visible spectroscopy

Aqueous alteration on main belt primitive asteroids: Results from visible spectroscopy

Astronomical Observations of Volatiles on Asteroids

Near-Infrared Spectrophotometry of Phobos and Deimos

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