5,185 research outputs found
METODO INNOVATIVO PER CREARE UN LAYER NANOSTRUTTURATO HONEYCOMB DI TITANIA, AUTOGENERATO SULLE SUPERFICI DI MATERIALI A BASE TITANIO, DESTINATI AL DOMINIO MEDICALE E CHIRURGICO DEGLI IMPIANTI DENTALI, DELLE PROTESI ORTOPEDICHE E DELLE OSTEOSINTESI.
NANOTECNOLOGIA, TITANIO, PROTESI ORTOPEDICHE, OSTEOSINTESI, NANOSTRUTTUR
Mapping Moho depth variations in central Italy from PsMoho-P delay times: Evidence of an E-W transition in the Adriatic Moho at 42°N latitude
Along the Italian peninsula adjoin two crustal domains, peri-Tyrrhenian and Adriatic, whose
boundary is not univocal in central Italy. In this area, we attempt to map the extent of the Moho in the
two terrains from variations of the travel time difference between the direct P wave and the P-to-S wave
converted at the crust-mantle boundary, called PsMoho. We use teleseismic receiver functions computed
at 38 broad-band stations in this and previous studies, and assigned each of the recording sites to the
Adriatic or peri-Tyrrhenian terrains based on station location, geologic and geophysical data and
interpretation, and consistency of delays with the regional Moho trend. The results of the present study
show that the PsMoho arrival time varies from 2.3 to 4.1 s in the peri-Tyrrhenian domain and from 3.7 to
5.5 s in the Adriatic domain. As expected, the lowest time difference is observed along the Tyrrhenian
coastline and the largest values are observed in the axial zone of the Apennine chain. A key new result of
this study is a sharp E-W boundary in the Adriatic domain that separates a deeper Moho north of about
42 N latitude from a shallower Moho to the south. This feature is constrained for a length of about 40 km
by the observations available in this study. The E-W boundary requires a revision of prior mapping of the
Moho in central Italy and supports previous hypotheses of lithosphere segmentation
A multidisciplinary approach using LCCA and micro-simulation 10 model for the management of the urban pavements
The maintenance and the rehabilitation of the urban road pavements are not often based on
systematic program and scheduling but rather on emergency or on other not identified reasons.
Moreover the Life Cycle Cost Analysis (LCCA), the only peculiar procedure for the
management pavement, finds its own application for highway and motorway, even if it is
possible to search the best investment for the urban interstate and arterials.
By the light of the quantity of the involved resources, it seems necessary to define an operative
methodology for programming the maintenance and rehabilitation activities for the urban
pavement. The paper is oriented towards the development of a multidisciplinary approach to
make decision on management of urban pavement using the basic concepts of the LCCA and
micro-simulation model to define a scheme of work zone that minimizes the delay on the traffic
flow.
The best rehabilitation strategy should be characterized by the lowest users\u2019 cost that depends on
the time period of the work zone, which is conditioned by both own scheme and the provided
treatment, and on \u201csocial cost\u201d as increased travel time for queue generation .
Different scenarios for different work zone plans were developed and a micro-simulation model
was used to assess increased total travel time of a traffic flow within the maintenance area.
In this work an analysis by means of the above mentioned approach was carried out on real scenario in the city of Palermo in order to point out the several frames of the adopted
methodology
Chandra Observation of the Persistent Emission from the Dipping Source XB 1916-053
We present the results of a 50 ks long Chandra observation of the dipping
source XB 1916-053. During the observation two X-ray bursts occurred and the
dips were not present at each orbital period. From the zero-order image we
estimate the precise X-ray coordinates of the source with a 90% uncertainty of
0.6''. In this work we focus on the spectral study of discrete absorption
features, during the persistent emission, using the High Energy Transmission
Grating Spectrometer on board the Chandra satellite. We detect, for the first
time in the 1st-order spectra of XB 1916-053, absorption lines associated to Ne
X, Mg XII, Si XIV, and S XVI, and confirm the presence of the Fe XXV and Fe
XXVI absorption lines with a larger accuracy with respect to the previous XMM
EPIC pn observation. Assuming that the line widths are due to a bulk motion or
a turbulence associated to the coronal activity, we estimate that the lines are
produced in a photoionized absorber distant from the neutron star 4 x 10^{10}
cm, near the disk edge.Comment: 20 pages, 10 figures, submitted to ApJ on 2005-09-22, accepted by ApJ
on 2006-05-0
Bipolar disorder and peripartum mood episodes: Epidemiology and clinical correlates
INTRODUCTION: It is known that the peripartum period is a high-risk period of recurrence in bipolar disorder (BD). However, data on correlations between reproductive life events, such as age at menarche and peripartum period, are mixed in BD. OBJECTIVES: The aims of this retrospective study are to investigate the lifetime rate of peripartum mood episodes, the clinical correlates and the relationship between age at menarche and peripartum episode in a sample of women with BD. METHODS: The study focused on comparisons between women with vs. without peripartum mood episodes (n = 292). Socio-demographic and clinical characteristics between women with vs without BD peripartum episode were examined through descriptive statistics.Adjusted logistic regression analysis was run to examine the association between variables. RESULTS: In our sample, 30% had at least one BD peripartum episode. Women with peripartum episode had significantly earlier age at menarche, earlier onset of BD and longer duration of untreated disorder compared to women without peripartum episode. After adjustment, the late menarche (>15 years) was associated with lower probability of BD episodes during the peripartum period compared to normal menarche (12-14 years). CONCLUSIONS: Peripartum mood episodes are common in BD and are correlated with early onset of BD and long duration of untreated disorder. Moreover, age at menarche may be related to the risk of peripartum mood episodes. The results deserve to be deepened in further studies
Broad-band Spectral Evolution of Scorpius X-1 along its Color-Color Diagram
We analyze a large collection of RXTE archive data from April 1997 to August
2003 of the bright X-ray source Scorpius X-1 in order to study the broadband
spectral evolution of the source for different values of the inferred mass
accretion rate by studying energy spectra from selected regions in the Z-track
of its Color-Color Diagram. A two-component model, consisting of a soft thermal
component interpreted as thermal emission from an accretion disk and a thermal
Comptonization component, is unable to fit the whole 3--200 keV energy spectrum
at low accretion rates. Strong residuals in the highest energy band of the
spectrum require the addition of a third component that can be fitted with a
power-law component, that could represent a second thermal Comptonization from
a much hotter plasma, or a hybrid thermal/non-thermal Comptonization. We
discuss the physical implications derived from the results of our analysis,
with a particular emphasis on the hardest part of the X-ray emission and its
possible origins.Comment: 18 pages. Accepted for publication in Ap
Timing of the Accreting Millisecond Pulsar XTE J1814-338
We present a precise timing analysis of the accreting millisecond pulsar XTE
J1814-338 during its 2003 outburst, observed by RXTE. A full orbital solution
is given for the first time; Doppler effects induced by the motion of the
source in the binary system were corrected, leading to a refined estimate of
the orbital period, P_orb=15388.7229(2)s, and of the projected semimajor axis,
a sini/c= 390.633(9) lt-ms. We could then investigate the spin behaviour of the
accreting compact object during the outburst. We report here a refined value of
the spin frequency (nu=314.35610879(1) Hz) and the first estimate of the spin
frequency derivative of this source while accreting (nu^dot=(-6.7 +/- 0.7)
10^(-14) Hz/s). This spin down behaviour arises when both the fundamental
frequency and the second harmonic are taken into consideration. We discuss this
in the context of the interaction between the disc and the quickly rotating
magnetosphere, at accretion rates sufficiently low to allow a threading of the
accretion disc in regions where the Keplerian velocity is slower than the
magnetosphere velocity. We also present indications of a jitter of the pulse
phases around the mean trend, which we argue results from movements of the
accreting hotspots in response to variations of the accretion rate.Comment: 7 pages, 4 figures, Accepted for publication by MNRA
Spectral analysis of LMC X-2 with XMM/Newton: unveiling the emission process in the extragalactic Z-source
We present the results of the analysis of an archival observation of LMC X-2
performed with XMM/Newton. The spectra taken by high-precision instruments have
never been analyzed before. We find an X-ray position for the source that is
inconsistent with the one obtained by ROSAT, but in agreement with the Einstein
position and that of the optical counterpart. The correlated spectral and
timing behaviour of the source suggests that the source is probably in the
normal branch of its X-ray color-color diagram. The spectrum of the source can
be fitted with a blackbody with a temperature 1.5 keV plus a disk blackbody at
0.8 keV. Photoelectric absorption from neutral matter has an equivalent
hydrogen column of 4 x 10^{20} cm^{-2}. An emission line, which we identify as
the O VIII Lyman alpha line, is detected, while no feature due to iron is
detected in the spectrum. We argue that the emission of this source can be
straightforwardly interpreted as a sum of the emission from a boundary layer
between the NS and the disc and a blackbody component coming from the disc
itself. Other canonical models that are used to fit Z-sources do not give a
satisfactory fit to the data. The detection of the O VIII emission line (and
the lack of detection of lines in the iron region) can be due to the fact that
the source lies in the Large Magellanic Cloud.Comment: Accepted for publication by Astronomy & Astrophysic
Evidence for a resonant cyclotron line in IGR J16493-4348 from the Swift-BAT hard X-ray survey
Resonant absorption cyclotron features are a key diagnostic tool to directly
measure the strength of the magnetic field of accreting neutron stars. However,
typical values for cyclotron features lie in the high-energy part of the
spectrum between 20 keV and 50 keV, where detection is often damped by the low
statistics from single pointed observations. We show that long-term monitoring
campaign performed with Swift-BAT of persistently, but faint, accreting
high-mass X-ray binaries is able to reveal in their spectra the presence of
cyclotron features. We extracted the average Swift-BAT 15-150 keV spectrum from
the 54 months long Swift-BAT survey of the high-mass X-ray source IGR
J16493-4348. To constrain the broadband spectrum we used soft X-ray spectra
from Swift-XRT and Suzaku pointed observations. We model the spectra using a
set of phenomenological models usually adopted to describe the energy spectrum
of accreting high-mass X-ray binaries; irrespective of the models we used, we
found significant improvements in the spectral fits adding to the models a
broad (10 keV width) absorption feature, with best-fitting energy estimate
between 30 and 33 keV, that we interpret as evidence for a resonant cyclotron
absorption feature. We also discuss instrumental issues related to the use of
Swift-BAT for this kind of studies and the statistical method to weight the
confidence level of this detection. Correcting for the gravitational redshift
of a 1.4 M_{\sun} neutron star, the inferred surface magnetic field is Bsurf
3.7 x 10^{12} Gauss. The spectral parameters of IGR J16493-4348 fit well with
empirical correlations observed when the whole sample of high-mass binaries
with detected cyclotron features is considered.Comment: Published in Astronomy & Astrophysics, 2011, 532, A7
Resolving the Fe xxv Triplet with Chandra in Cen X-3
We present the results of a 45 ks Chandra observation of the high-mass X-ray
binary Cen X--3 at orbital phases between 0.13 and 0.40 (in the eclipse
post-egress phases). Here we concentrate on the study of discrete features in
the energy spectrum at energies between 6 and 7 keV, i.e. on the iron
K line region, using the High Energy Transmission Grating Spectrometer
on board the Chandra satellite. We clearly see a K neutral iron line
at keV and were able to distinguish the three lines of the
\ion{Fe}{25} triplet at 6.61 keV, 6.67 keV, and 6.72 keV, with an equivalent
width of 6 eV, 9 eV, and 5 eV, respectively. The equivalent width of the
K neutral iron line is 13 eV, an order of magnitude lower than
previous measures. We discuss the possibility that the small equivalent width
is due to a decrease of the solid angle subtended by the reflector.Comment: 11 pages, 2 figures, To appear in the Astrophysical Journal Letter
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