86 research outputs found
Mineralogy and Surface Composition of Asteroids
Methods to constrain the surface mineralogy of asteroids have seen
considerable development during the last decade with advancement in laboratory
spectral calibrations and validation of our interpretive methodologies by
spacecraft rendezvous missions. This has enabled the accurate identification of
several meteorite parent bodies in the main asteroid belt and helped constrain
the mineral chemistries and abundances in ordinary chondrites and basaltic
achondrites. With better quantification of spectral effects due to temperature,
phase angle, and grain size, systematic discrepancies due to non-compositional
factors can now be virtually eliminated for mafic silicate-bearing asteroids.
Interpretation of spectrally featureless asteroids remains a challenge. This
paper presents a review of all mineralogical interpretive tools currently in
use and outlines procedures for their application.Comment: Chapter to appear in the Space Science Series Book: Asteroids IV, 51
pages, 7 figures, 2 table
The Effect of Lunar-like Satellites on the Orbital Infrared Light Curves of Earth-analog Planets
We investigate the influence of lunar-like satellites on the infrared orbital
light curves of Earth-analog extra-solar planets. Such light curves will be
obtained by NASA's Terrestrial Planet Finder (TPF) and ESA's Darwin missions as
a consequence of repeat observations to confirm the companion status of a
putative planet. We use an energy balance model to calculate disk-averaged
infrared (bolometric) fluxes from planet-satellite systems over a full orbital
period (one year). The satellites are assumed to lack an atmosphere, have a low
thermal inertia like that of the Moon and span a range of plausible radii. The
planets are assumed to have thermal and orbital properties that mimic those of
the Earth while their obliquities and orbital longitudes of inferior
conjunction remain free parameters. Even if the gross thermal properties of the
planet can be independently constrained (e.g. via spectroscopy or
visible-wavelength detection of specular glint from a surface ocean) only the
largest (approximately Mars-size) lunar-like satellites can be detected by
light curve data from a TPF-like instrument (i.e. one that achieves a
photometric signal-to-noise of 10-20 at infrared wavelengths). Non-detection of
a lunar-like satellite can obfuscate the interpretation of a given system's
infrared light curve so that it may resemble a single planet with high
obliquity, different orbital longitude of vernal equinox relative to inferior
conjunction and in some cases drastically different thermal characteristics. If
the thermal properties of the planet are not independently established then the
presence of a lunar-like satellite cannot be inferred from infrared data, thus
demonstrating that photometric light curves alone can only be used for
preliminary study of extra-solar Earth-like planets.Comment: 34 pages, 7 figures, accepted to Astrobiolog
Unexpected D-type Interlopers in the Inner Main Belt
Very red featureless asteroids (spectroscopic D-types) are expected to have
formed in the outer solar system far from the sun. They comprise the majority
of asteroids in the Jupiter Trojan population, and are also commonly found in
the outer main belt and among Hildas. The first evidence for D-types in the
inner and middle parts of the main belt was seen in the Sloan Digital Sky
Survey (SDSS). Here we report follow-up observations of SDSS D-type candidates
in the near-infrared. Based on follow up observations of 13 SDSS D-type
candidates, we find a ~20% positive confirmation rate. Known inner belt D-types
range in diameter from roughly 7 to 30 kilometers. Based on these detections we
estimate there are ~100 inner belt D-types with diameters between 2.5 and 20km.
The lower and upper limits for total mass of inner belt D-types is 2x
kg to 2x kg which represents 0.01% to 0.1% of the mass of the inner
belt. The inner belt D-types have albedos at or above the upper end typical for
D-types which raises the question as to whether these inner belt bodies
represent only a subset of D-types, they have been altered by external factors
such as weathering processes, or if they are compositionally distinct from
other D-types. All D-types and candidates have diameters less than 30km, yet
there is no obvious parent body in the inner belt. Dynamical models have yet to
show how D-types originating from the outer solar system could penetrate into
the inner reaches of the Main Belt under current scenarios of planet formation
and subsequent Yarkovsky drift.Comment: 16 pages, 3 figures, 4 tables -- accepted for publication in Icaru
Mid-IR Spectra of HED Meteorites and Synthetic Pyroxenes: Reststrahlen Features (9-12 micron)
In an earlier study. Hamilton (2000) mapped the behavior of the 9-12 micron reststrahlen structures with composition in a suite of primarily natural terrestrial pyroxenes. Here we examine the same set of reststrahlen features in the spectra of diogenites and eucrites and place them in the context of the terrestrial samples and of a suite of well-characterized synthetic pyroxenes. The results will be useful to the interpretation of mid-IR spectra of 4 Vesta and other basaltic asteroids
Diogenite-like Features in the Spitzer IRS (5-35 micrometers) Spectrum of 956 ELISA
We report preliminary results from the Spitzer Infrared Spectrograph (IRS) observations of the V-type asteroid 956 Elisa. Elisa was observed as part of a campaign to measure the 5.2-38 micron spectra of small basaltic asteroids with the Spitzer IRS. Targets include members of the dynamical family of the unique large differentiated asteroid 4 Vesta ("Vesroids"), several outer-main-belt basaltic asteroids whose orbits exclude them from originating on 4 Vesta, and the basaltic near-Earth asteroid 4055 Magellan
Rotational properties of the Haumea family members and candidates: Short-term variability
Haumea is one of the most interesting and intriguing transneptunian objects
(TNOs). It is a large, bright, fast rotator, and its spectrum indicates nearly
pure water ice on the surface. It has at least two satellites and a dynamically
related family of more than ten TNOs with very similar proper orbital
parameters and similar surface properties. The Haumean family is the only one
currently known in the transneptunian belt. Various models have been proposed
but the formation of the family remains poorly understood. In this work, we
have investigated the rotational properties of the family members and
unconfirmed family candidates with short-term variability studies, and report
the most complete review to date. We present results based on five years of
observations and report the short-term variability of five family members, and
seven candidates. The mean rotational periods, from Maxwellian fits to the
frequency distributions, are 6.27+/-1.19 h for the confirmed family members,
6.44+/-1.16 h for the candidates, and 7.65+/-0.54 h for other TNOs (without
relation to the family). According to our study, there is a suggestion that
Haumea family members rotate faster than other TNOs, however, the sample of
family member is still too limited for a secure conclusion. We also highlight
the fast rotation of 2002 GH32. This object has a 0.36+/-0.02 mag amplitude
lightcurve and a rotational period of about 3.98 h. Assuming 2002 GH32 is a
triaxial object in hydrostatic equilibrium, we derive a lower limit to the
density of 2.56 g cm^-3. This density is similar to Haumea's and much more
dense than other small TNO densities.Comment: Accepted for publication, A
The Near-Earth Encounter of 2005 YU55: Thermal Infrared Observations from Gemini North
As part of a multi-observatory campaign to observe 2005 YU55 during its November 2011 encounter with the Earth, thermal infrared photometry and spectroscopy (7.9- 14 and 18-22 micron) were conducted using the Michelle instrument at Gemini North. Reduction of the 8.8 flm photometry and the spectroscopy from UT Nov-IO as well as of all the Gemini data from UT Nov-9 is in progress. Results will be discussed
The 2016 Reactivations of Main-Belt Comets 238P/Read and 288P/(300163) 2006 VW139
We report observations of the reactivations of main-belt comets 238P/Read and
288P/(300163) 2006 VW139, that also track the evolution of each object's
activity over several months in 2016 and 2017. We additionally identify and
analyze archival SDSS data showing 288P to be active in 2000, meaning that both
238P and 288P have now each been confirmed to be active near perihelion on
three separate occasions. From data obtained of 288P from 2012-2015 when it
appeared inactive, we find best-fit R-band H,G phase function parameters of
H_R=16.80+/-0.12 mag and G_R=0.18+/-0.11, corresponding to effective component
radii of r_c=0.80+/-0.04 km, assuming a binary system with equally-sized
components. Fitting linear functions to ejected dust masses inferred for 238P
and 288P soon after their observed reactivations in 2016, we find an initial
average net dust production rate of 0.7+/-0.3 kg/s and a best-fit start date of
2016 March 11 (when the object was at a true anomaly of -63 deg) for 238P, and
an initial average net dust production rate of 5.6+/-0.7 kg/s and a best-fit
start date of 2016 August 5 (when the object was at a true anomaly of -27 deg)
for 288P. Applying similar analyses to archival data, we find similar start
points for previous active episodes for both objects, suggesting that minimal
mantle growth or ice recession occurred between the active episodes in
question. Some changes in dust production rates between active episodes are
detected, however. More detailed dust modeling is suggested to further clarify
the process of activity evolution in main-belt comets.Comment: 21 pages, 9 figures, accepted by A
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