3,174 research outputs found
Rotationally resolved spectroscopy of dwarf planet (136472) Makemake
Context. Icy dwarf planets are key for studying the chemical and physical
states of ices in the outer solar system. The study of secular and rotational
variations gives us hints of the processes that contribute to the evolution of
their surface. Aims. The aim of this work is to search for rotational
variability on the surface composition of the dwarf planet (136472) Makemake
Methods. We observed Makemake in April 2008 with the medium-resolution
spectrograph ISIS, at the William Herschel Telescope (La Palma, Spain) and
obtained a set of spectra in the 0.28 - 0.52 {\mu}m and 0.70 - 0.95 {\mu}m
ranges, covering 82% of its rotational period. For the rotational analysis, we
organized the spectra in four different sets corresponding to different
rotational phases, and after discarding one with low signal to noise, we
analyzed three of them that cover 71% of the surface. For these spectra we
computed the spectral slope and compared the observed spectral bands of methane
ice with reflectances of pure methane ice to search for shifts of the center of
the bands, related to the presence of CH 4 /N 2 solid solution. Results. All
the spectra have a red color with spectral slopes between 20%/1000 {\AA} and
32%/1000 {\AA} in accordance with previously reported values. Some variation in
the spectral slope is detected, pointing to the possibility of a variation in
the surface content or the particle size of the solid organic compound. The
absorption bands of methane ice present a shift toward shorter wavelengths,
indicating that methane (at least partially) is in solid solution with
nitrogen. There is no variation within the errors of the shifts with the
wavelength or with the depth of the bands, so there is no evidence of variation
in the CH 4 /N 2 mixing ratio with rotation. By comparing with all the
available data in the literature, no secular compositional variations between
2005 and 2008 is found
Near-infrared spectroscopy of 1999 JU3, the target of the Hayabusa 2 mission
Context. Primitive asteroids contain complex organic material and ices
relevant to the origin of life on Earth. These types of asteroids are the
target of several-sample return missions to be launched in the next years. 1999
JU3 is the target of the Japanese Aerospace Exploration Agency's Hayabusa 2
mission. Aims. 1999 JU3 has been previously identified as a C-class asteroid.
Spectroscopic observations at longer wavelengths will help to constrain its
composition. Methods. We obtained spectroscopy of 1999 JU3 from 0.85 to 2.2
microns, with the 3.6 m Telescopio Nazionale Galileo using the low resolution
mode of the Near Infrared Camera Spectrograph. Results. We present a
near-infrared spectrum of 1999 JU3 from 0.85 to 2.2microns that is consistent
with previously published spectra and with its C-type classification.
Conclusions. Our spectrum confirms the primitive nature of 1999 JU3 and its
interest as target of the sample-return mission Hayabusa 2.Comment: Research Note: 3 pages 1 Figure Received December 2012; accepted 4
March 201
Rotationally resolved spectroscopy of (20000) Varuna in the near-infrared
Models of the escape and retention of volatiles by minor icy objects exclude
any presence of volatile ices on the surface of TNOs smaller than ~1000km in
diameter at the typical temperature in this region of the solar system, whereas
the same models show that water ice is stable on the surface of objects over a
wide range of diameters. Collisions and cometary activity have been used to
explain the process of surface refreshing of TNOs and Centaurs. These processes
can produce surface heterogeneity that can be studied by collecting information
at different rotational phases. The aims of this work are to study the surface
composition of (20000)Varuna, a TNO with a diameter ~650km and to search for
indications of rotational variability. We observed Varuna during two
consecutive nights in January 2011 with NICS@TNG obtaining a set of spectra
covering the whole rotation period of Varuna. After studying the spectra
corresponding to different rotational phases, we did not find any indication of
surface variability. In all the spectra, we detect an absorption at 2{\mu}m,
suggesting the presence of water ice on the surface. We do not detect any other
volatiles on the surface, although the S/N is not high enough to discard their
presence. Based on scattering models, we present two possible compositions
compatible with our set of data and discuss their implications in the frame of
the collisional history of the Kuiper Belt. We find that the most probable
composition for the surface of Varuna is a mixture of amorphous silicates,
complex organics, and water ice. This composition is compatible with all the
materials being primordial. However, our data can also be fitted by models
containing up to a 10% of methane ice. For an object with the characteristics
of Varuna, this volatile could not be primordial, so an event, such as an
energetic impact, would be needed to explain its presence on the surface.Comment: 6 pages, 5 figures, to be published in A&
Additional spectra of asteroid 1996 FG3, backup target of the ESA MarcoPolo-R mission
Near-Earth binary asteroid (175706) 1996 FG3 is the current backup target of
the ESA MarcoPolo-R mission, selected for the study phase of ESA M3 missions.
It is a primitive (C-type) asteroid that shows significant variation in its
visible and near-infrared spectra. Here we present new spectra of 1996 FG3 and
we compare our new data with other published spectra, analysing the variation
in the spectral slope. The asteroid will not be observable again over the next
three years at least. We obtained the spectra using DOLORES and NICS
instruments at the Telescopio Nazionale Galileo (TNG), a 3.6m telescope located
at El Roque de los Muchachos Observatory in La Palma, Spain. To compare with
other published spectra of the asteroid, we computed the spectral slope S', and
studied any plausible correlation of this quantity with the phase angle
(alpha). In the case of visible spectra, we find a variation in spectral slope
of Delta S' = 0.15 +- 0.10 %/10^3 A/degree for 3 < alpha < 18 degrees, in good
agreement with the values found in the literature for the phase reddening
effect. In the case of the near-infrared, we find a variation in the slope of
Delta S' = 0.04 +- 0.08 %/10^3 A/degree for 6 < alpha < 51 degrees. Our
computed variation in S' agrees with the only two values found in the
literature for the phase reddening in the near-infrared. The variation in the
spectral slope of asteroid 1996 FG3 shows a trend with the phase angle at the
time of the observations, both in the visible and the near-infrared. It is
worth noting that, to fully explain this spectral variability we should take
into account other factors, like the position of the secondary component of the
binary asteroid 1999 FG3 with respect to the primary, or the spin axis
orientation at the time of the observations. More data are necessary for an
analysis of this kind.Comment: 4 pages, 3 figures, Accepted in A&A 25 June 201
The Spectrum of Pluto, 0.40 - 0.93 m I. Secular and longitudinal distribution of ices and complex organics
Context. During the last 30 years the surface of Pluto has been
characterized, and its variability has been monitored, through continuous
near-infrared spectroscopic observations. But in the visible range only few
data are available. Aims. The aim of this work is to define the Pluto's
relative reflectance in the visible range to characterize the different
components of its surface, and to provide ground based observations in support
of the New Horizons mission. Methods. We observed Pluto on six nights between
May and July 2014, with the imager/spectrograph ACAM at the William Herschel
Telescope (La Palma, Spain). The six spectra obtained cover a whole rotation of
Pluto (Prot = 6.4 days). For all the spectra we computed the spectral slope and
the depth of the absorption bands of methane ice between 0.62 and 0.90 m.
To search for shifts of the center of the methane bands, associated with
dilution of CH4 in N2, we compared the bands with reflectances of pure methane
ice. Results. All the new spectra show the methane ice absorption bands between
0.62 and 0.90 m. The computation of the depth of the band at 0.62 m
in the new spectra of Pluto, and in the spectra of Makemake and Eris from the
literature, allowed us to estimate the Lambert coefficient at this wavelength,
at a temperature of 30 K and 40 K, never measured before. All the detected
bands are blue shifted, with minimum shifts in correspondence with the regions
where the abundance of methane is higher. This could be indicative of a
dilution of CH4:N2 more saturated in CH4. The longitudinal and secular
variations of the parameters measured in the spectra are in accordance with
results previously reported in the literature and with the distribution of the
dark and bright material that show the Pluto's albedo maps from New Horizons.Comment: This manuscript may change and improve during the reviewing process.
The data reduction and calibration is reliable and has been checked
independently using different reduction approaches. The data will be made
publicily available when the paper is accepted. If you need them before,
please, contact the autho
Multiple jumps and vacancy diffusion in a face-centered cubic metal
The diffusion of monovacancies in gold has been studied by computer
simulation. Multiple jumps have been found to play a central role in the atomic
dynamics at high temperature, and have been shown to be responsible for an
upward curvature in the Arrhenius plot of the diffusion coefficient.
Appropriate saddle points on the potential energy surface have been found,
supporting the interpretation of vacancy multiple jumps as distinct migration
mechanisms.Comment: 16 page
Recovery of residual copper from low-content tailings derived from waste electrical cable treatment
The current work aims at the recovery of residual copper from electrical cables with low content of copper (less than 5%). The sample originated from the tailings of electrical cables that had been previously subjected to copper recycling treatment. The tailings were successively treated with physical methods (sieving, heavy medium sep- aration in ZnCl2 bath, and counter-current separation) and electrochemical methods (cementation, electrowin- ning). Sieving seems to be more efficient than gravity separation methods, since, for 1.00 mm aperture and sieving time as short as 2 min, the undersize copper grade of the product was 57% in copper (from 4% in the feed), with corresponding copper recovery of 53%. Longer sieving times or larger apertures led to products with higher copper recovery but of lower grade. As regards cementation, preliminary tests were carried out to investigate the effect of pH using high purity CuSO4 \ub7 5H2O instead of dissolving metallic copper. Subsequent tests using the sieving undersize product of the scrap copper wire confirmed the results of the preliminary tests; in addition to pH, this product was also used to investigate the effects of the attacking chemical (H2SO4, HCl, H2O2), sacrificial metal (aluminium, iron scrap), temperature, and surface area on cementation. The results show that cementation of the dissolved copper from scrap wire is efficient at pH = 2.5\u20133.2, with sufficient copper recovery within a few hours. Also, electrowinning tests on the undersize sieving product proved the feasibility to obtain pure copper by electrodeposition onto stainless steel cathode with lead anode, without contamination of the electrolytic solution. In both methods, copper purity degrades when HCl acid is used instead of H2SO4. Espe- cially with the use of H2SO4 in electrowinning, it was observed that lead anode is passivated when the solution is entirely depleted from copper ions. The results of the current work clearly demonstrate the feasibility to obtain pure copper from low-grade electric wire scraps by successively submitting the tailings to sieving and cementation
On the need for multi-dimensional models for the safety analysis of (fast-spectrum) Molten Salt Reactors
This paper aims at characterizing the impact of adopting numerical models with different dimensionalities on the predicted behavior of fast-spectrum Molten Salt Reactors (MSRs). The study encompasses 1-D, 2-D, and 3-D representations of thermal-hydraulics and precursor transport/diffusion, along with spatial and point kinetics models for neutronics. We evaluate the accuracy of each model based on steady-state results and on the reactor response to 2 different transient initiators. The findings emphasize the significance of utilizing a 3-D representation with accurate thermal-hydraulics modeling, and with either spatial kinetics or carefully calibrated point kinetics incorporating a spatial description of precursors transport. 2-D and 1-D models can reproduce main trends and remain valuable tools for e.g. reactor design, control-oriented studies or uncertainty quantification. However, proper calibration of these models is needed and the user should be aware that alterations in flow patterns could jeopardize model calibration and hide first-order local effects
An \emph{ab initio} method for locating characteristic potential energy minima of liquids
It is possible in principle to probe the many--atom potential surface using
density functional theory (DFT). This will allow us to apply DFT to the
Hamiltonian formulation of atomic motion in monatomic liquids [\textit{Phys.
Rev. E} {\bf 56}, 4179 (1997)]. For a monatomic system, analysis of the
potential surface is facilitated by the random and symmetric classification of
potential energy valleys. Since the random valleys are numerically dominant and
uniform in their macroscopic potential properties, only a few quenches are
necessary to establish these properties. Here we describe an efficient
technique for doing this. Quenches are done from easily generated "stochastic"
configurations, in which the nuclei are distributed uniformly within a
constraint limiting the closeness of approach. For metallic Na with atomic pair
potential interactions, it is shown that quenches from stochastic
configurations and quenches from equilibrium liquid Molecular Dynamics (MD)
configurations produce statistically identical distributions of the structural
potential energy. Again for metallic Na, it is shown that DFT quenches from
stochastic configurations provide the parameters which calibrate the
Hamiltonian. A statistical mechanical analysis shows how the underlying
potential properties can be extracted from the distributions found in quenches
from stochastic configurations
Testing the nature of S0 galaxies using planetary nebula kinematics in NGC 1023
We investigate the manner in which lenticular galaxies are formed by studying
their stellar kinematics: an S0 formed from a fading spiral galaxy should
display similar cold outer disc kinematics to its progenitor, while an S0
formed in a minor merger should be more dominated by random motions. In a pilot
study to attempt to distinguish between these scenarios, we have measured the
planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the
Planetary Nebula Spectrograph, we have detected and measured the line-of-sight
velocities of 204 candidate PNe in the field of this galaxy. Out to
intermediate radii, the system displays the kinematics of a normal
rotationally-supported disc system. After correction of its rotational
velocities for asymmetric drift, the galaxy lies just below the spiral galaxy
Tully-Fisher relation, as one would expect for a fading system. However, at
larger radii the kinematics undergo a gradual but major transition to random
motion with little rotation. This transition does not seem to reflect a change
in the viewing geometry or the presence of a distinct halo component, since the
number counts of PNe follow the same simple exponential decline as the stellar
continuum with the same projected disc ellipticity out to large radii. The
galaxy's small companion, NGC 1023A, does not seem to be large enough to have
caused the observed modification either. This combination of properties would
seem to indicate a complex evolutionary history in either the transition to
form an S0 or in the past life of the spiral galaxy from which the S0 formed.
More data sets of this type from both spirals and S0s are needed in order to
definitively determine the relationship between these types of system.Comment: Accepted for publication in MNRAS. Version with full resolution
figure 1 can be found at
http://www.nottingham.ac.uk/~ppzmrm/N1023_PNS.accepted.pd
- …