Midinfrared (2.5–13.5 μm) reflectance spectra of powdered stony meteorites

Salisbury, John W.; D'Aria, Dana M.; Jarosewich, E.

doi:10.1016/0019-1035(91)90052-u

Cited by 184 publications

(193 citation statements)

References 29 publications

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“…4.2) pointed at predominantly larger particles as cause for the far-IR emissivity drop. But the Salibury et al (1991a) library provides only spectra of small grain sizes. Le Bras & Erard 2003 found that the grain size effect can shift the CF in wavelengths and change also the contrast.…”

Section: Emissivity Analysismentioning

confidence: 99%

65 Cybele in the thermal infrared: Multiple observations and thermophysical analysis

Müller

Blommaert

2004

A&A

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Abstract. We investigated the physical and thermal properties of 65 Cybele, one of the largest main-belt asteroids. Based on published and recently obtained thermal infrared observations, including ISO measurements, we derived through thermophysical modelling (TPM) a size of 302 × 290 × 232 km (±4%) and an geometric visible albedo of 0.050 ± 0.005. Our model of a regolith covered surface with low thermal inertia and "default" roughness describes the wavelengths and phase angle dependent thermal effects very well. Before/after opposition effect and beaming behaviour can be explained in that way. We found a constant emissivity of 0.9 at wavelengths up to about 100 µm and lower values towards the submillimetre range, indicating a grain size distribution dominated by 200 µm particle sizes. The spectroscopic analysis revealed an emissivity increase between 8.0 and 9.5 µm. We compared this emissivity behaviour with the Christiansen features of carbonaceous chondrite meteorites, but a conclusive identification was not possible. A comparison between the Standard Thermal Model (STM) and the applied TPM clearly demonstrates the limitations and problems of the STM for the analysis of multi-epoch and -wavelengths observations. While the TPM produced a unique diameter/albedo solution, the calculated STM values varied by ±30% and showed clear trends with wavelength and phase angle. 65 Cybele can be considered as a nice textbook case for the thermophysical analysis of combined optical and thermal infrared observations.

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Section: Emissivity Analysismentioning

confidence: 99%

65 Cybele in the thermal infrared: Multiple observations and thermophysical analysis

Müller

Blommaert

2004

A&A

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“…For this study we measured grain size separate < 25 µm, the finer particles being a reasonable analogue of asteroidal regolith in terms of particle size, as suggested from Salisbury et al (1991) and Pieters et al (1993). For emissivity measurements under vacuum and under purging we kept the sample temperature as low as possible (100 °C on the surface) while still having a good signalto-noise ratio.…”

Section: Sample Selectionmentioning

confidence: 99%

“…Among them, Salisbury et al (1991) measured reflectance (mostly bi-conical) spectra in air of many meteorites in the 2.5-to 13-µm spectral range. Emissivity (in air) spectra for large grain size samples (710-1000 µm) in the 5-to 45-µm spectral range were reported by Christensen et al (2000).…”

Section: Introductionmentioning

confidence: 99%

Characterization of asteroid analogues by means of emission and reflectance spectroscopy in the 1- to 100-µm spectral range

et al. 2016

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The last decades have seen a large number of missions targeting small bodies in the solar system. NASA, ESA and JAXA sent missions to different solar system small bodies (SSSB), and the Japan mission Hayabusa returned samples from the surface of the S-type asteroid Itokawa. JAXA launched in 2014 a follow-up mission (Hayabusa2) to collect a sample from carbonaceous (C-type) asteroid 1999 JU3 asteroid and bring it back to Earth. The NASA's OSIRIS-REx mission will launch in September 2016 to explore the carbonaceous asteroid Bennu. Despite an already existing rich collection of reflectance and emissivity spectral libraries for asteroid analogues, those are mostly based on measurements in air for a spectral range covering the visible to the medium infrared (approximately, from 0.4 to 25 µm). To characterize minerals, rocks and meteorites suitable for being surface analogues for asteroids and SSSB in general, spectroscopic measurements are needed for a wider spectral range and in vacuum, conditions that more closely resemble those found on asteroid surfaces. To fill this gap we acquired spectral measurements over a large spectral range (1-100 µm) for several meteorites and other analogues at the Planetary Emissivity Laboratory of the German Aerospace Center in Berlin. Those data provide more direct analogues for asteroid surfaces and expand our existing database of emissivity and reflectance measurements.

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“…Laboratory work on meteorite spectra has included exploring such specific problems as the effects of mixing different mineralogical types (Hiroi et al 1993), and using powdered meteorite samples (Salisbury et al 1991). Geologic processes on asteroids required to produce individual meteorite classes have been modeled in some detail (Kargel 1991, Warren and Kallemeyn 1992, Rubin and Mittlefehldt 1993, Benoit and Sears 1993.…”

Section: Asteroids Vs Meteoritesmentioning

confidence: 99%

Commission 15: Physical Study of Comets. Minor Planets and meteorites (L’etude Physique des Cometes. des Petites Planetes Et des Meteorites)

1994

Trans. Int. Astron. Union

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Midinfrared (2.5–13.5 μm) reflectance spectra of powdered stony meteorites

Cited by 184 publications

References 29 publications

65 Cybele in the thermal infrared: Multiple observations and thermophysical analysis

65 Cybele in the thermal infrared: Multiple observations and thermophysical analysis

Characterization of asteroid analogues by means of emission and reflectance spectroscopy in the 1- to 100-µm spectral range

Commission 15: Physical Study of Comets. Minor Planets and meteorites (L’etude Physique des Cometes. des Petites Planetes Et des Meteorites)

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