3,805 research outputs found
The envelope of the power spectra of over a thousand \delta Scuti stars. The - scaling relation
CoRoT and Kepler high-precision photometric data allowed the detection and
characterization of the oscillation parameters in stars other than the Sun.
Moreover, thanks to the scaling relations, it is possible to estimate masses
and radii for thousands of solar-type oscillating stars. Recently, a \Delta\nu
- \rho relation has been found for \delta Scuti stars. Now, analyzing several
hundreds of this kind of stars observed with CoRoT and Kepler, we present an
empiric relation between their frequency at maximum power of their oscillation
spectra and their effective temperature. Such a relation can be explained with
the help of the \kappa-mechanism and the observed dispersion of the residuals
is compatible with they being caused by the gravity-darkening effect
The intricate Galaxy disk: velocity asymmetries in Gaia-TGAS
We use the Gaia-TGAS data to compare the transverse velocities in Galactic
longitude (coming from proper motions and parallaxes) in the Milky Way disk for
negative and positive longitudes as a function of distance. The transverse
velocities are strongly asymmetric and deviate significantly from the
expectations for an axisymmetric Galaxy. The value and sign of the asymmetry
changes at spatial scales of several tens of degrees in Galactic longitude and
about 0.5 kpc in distance. The asymmetry is statistically significant at 95%
confidence level for 57% of the region probed, which extends up to ~1.2 kpc. A
percentage of 24% of the region studied shows absolute differences at this
confidence level larger than 5 km/s and 7% larger than 10 km/s. The asymmetry
pattern shows mild variations in the vertical direction and with stellar type.
A first qualitative comparison with spiral arm models indicates that the arms
are unlikely to be the main source of the asymmetry. We briefly discuss
alternative origins. This is the first time that global all-sky asymmetries are
detected in the Milky Way kinematics, beyond the local neighbourhood, and with
a purely astrometric sample.Comment: Accepted for publication in A&A Letter
Evidence of amplitude modulation due to Resonant Mode Coupling in the delta Scuti star KIC5892969
A study of the star KIC5892969 observed by the Kepler satellite is presented.
Its three highest amplitude modes present a strong amplitude modulation. The
aim of this work is to investigate amplitude variations in this star and their
possible cause. Using the 4 years-long observations available, we obtained the
frequency content of the full light curve. Then, we studied the amplitude and
phase variations with time using shorter time stamps. The results obtained are
compared with the predicted ones for resonant mode coupling of an unstable mode
with lower frequency stable modes. Our conclusion is that resonant mode
coupling is consistent as an amplitude limitation mechanism in several modes of
KIC5892969 and we discuss to which extent it might play an important role for
other delta Scuti stars
Evidence of chaotic modes in the analysis of four delta Scuti stars
Since CoRoT observations unveiled the very low amplitude modes that form a
flat plateau in the power spectrum structure of delta Scuti stars, the nature
of this phenomenon, including the possibility of spurious signals due to the
light curve analysis, has been a matter of long-standing scientific debate. We
contribute to this debate by finding the structural parameters of a sample of
four delta Scuti stars, CID 546, CID 3619, CID 8669, and KIC 5892969, and
looking for a possible relation between these stars' structural parameters and
their power spectrum structure. For the purposes of characterization, we
developed a method of studying and analysing the power spectrum with high
precision and have applied it to both CoRoT and Kepler light curves. We obtain
the best estimates to date of these stars' structural parameters. Moreover, we
observe that the power spectrum structure depends on the inclination,
oblateness, and convective efficiency of each star. Our results suggest that
the power spectrum structure is real and is possibly formed by 2-period island
modes and chaotic modes
Mobility through Heterogeneous Networks in a 4G Environment
Serving and Managing users in a heterogeneous environment. 17th WWRF Meeting in Heidelberg, Germany, 15 - 17 November 2006. [Proceeding presented at WG3 - Co-operative and Ad-hoc Networks]The increase will of ubiquitous access of the users to the requested services points towards the integration of heterogeneous networks. In this sense, a user shall be able to access its services through different access technologies, such as WLAN, Wimax, UMTS and DVB technologies, from the same or different network operators, and to seamless move between different networks with active communications. In this paper we propose a mobility architecture able to support this users’ ubiquitous access and seamless movement, while simultaneously bringing a large flexibility to access network operators
Analysis of transcription factor interactions in osteoblasts using competitive chromatin immunoprecipitation
Chromatin immunoprecipitation (ChIP) is a widely used technique for quantifying protein–DNA interactions in living cells. This method commonly uses fixed (crosslinked) chromatin that is fragmented by sonication (X-ChIP). We developed a simple new ChIP procedure for the immunoprecipitation of sonicated chromatin isolated from osteoblasts in the absence of crosslinking (N-ChIP). The use of noncrosslinked chromatin allowed development of a new modification of the ChIP assay: the combination of N-ChIP and competition with double-stranded oligonucleotides containing specific binding sites for individual transcription factors (Competitive N-ChIP). Using this approach, we were able to discriminate between individual binding sites for the Runx2 transcription factor in the osteocalcin and bone sialoprotein genes that cannot be resolved by traditional X-ChIP. N-ChIP assays were also able to detect several other types of chromatin interactions including those with Dlx homeodomain factors and nuclear proteins such as Sin3a that lack an intrinsic DNA-binding motif and, therefore, bind to chromatin via interactions with other proteins
Electron scattering in isotonic chains as a probe of the proton shell structure of unstable nuclei
Electron scattering on unstable nuclei is planned in future facilities of the
GSI and RIKEN upgrades. Motivated by this fact, we study theoretical
predictions for elastic electron scattering in the N=82, N=50, and N=14
isotonic chains from very proton-deficient to very proton-rich isotones. We
compute the scattering observables by performing Dirac partial-wave
calculations. The charge density of the nucleus is obtained with a covariant
nuclear mean-field model that accounts for the low-energy electromagnetic
structure of the nucleon. For the discussion of the dependence of scattering
observables at low-momentum transfer on the gross properties of the charge
density, we fit Helm model distributions to the self-consistent mean-field
densities. We find that the changes shown by the electric charge form factor
along each isotonic chain are strongly correlated with the underlying proton
shell structure of the isotones. We conclude that elastic electron scattering
experiments in isotones can provide valuable information about the filling
order and occupation of the single-particle levels of protons.Comment: 13 pages; 19 figure
Thermal contact resistance in a non-ideal joint
The contact conductance at an interface can be determined by knowing the material and surface properties and the interfacial pressure distribution. This pressure distribution can be influenced strongly by the roughness of the mating surfaces but until now this effect has been ignored in studies of joint conductance. This thesis considers this effect and shows the circumstances when it is an important factor. Furthermore, it is shown that one can either raise or lower the total resistance of a joint by changing the surface properties in the proper manner for the particular system being considered. Specifically, this thesis deals with three systems: the contact of two rough, wavy surfaces; the contact of two rough but nominally flat plates pressed together over a concentrated area; and the contact of two rough but nominally flat plates bolted together. In each case the pressure distribution is calculated as a function of the surface properties. In the case of wavy surfaces it is found that all necessary information for any combination of parameters can be reduced to one master graph. In the other two cases one such graph is needed for each geometry used. The resulting pressure distributions are used in a specific heat transfer example and the total joint resistance versus roughness is presented. It is shown how one can actually decrease the resistance by increasing the roughness - a seemingly contradictory phenomenon. Heat transfer experiments performed by Joseph Pigott qualitatively confirmed the theoretical findings.Sponsored by George C. Marshall Space Flight Center, NAS
Orbital phase resolved spectroscopy of 4U1538-52 with MAXI
4U 1538-52, an absorbed high mass X-ray binary with an orbital period of 3.73
days, shows moderate orbital intensity modulations with a low level of counts
during the eclipse. Several models have been proposed to explain the accretion
at different orbital phases by a spherically symmetric stellar wind from the
companion. The aim of this work is to study both the light curve and orbital
phase spectroscopy of this source in the long term. Particularly, the folded
light curve and the changes of the spectral parameters with orbital phase to
analyse the stellar wind of QV Nor, the mass donor of this binary system. We
used all the observations made from the Gas Slit Camera on board MAXI of 4U
1538-52 covering many orbits continuously. We obtained the good interval times
for every orbital phase range which were the input to extract our data. We
estimated the orbital period of the system and then folded the light curves and
we fitted the X-ray spectra with the same model for every orbital phase
spectrum. We also extracted the averaged spectrum of all the MAXI data
available. The MAXI spectra in the 2-20 keV energy range were fitted with an
absorbed Comptonization of cool photons on hot electrons. We found a strong
orbital dependence of the absorption column density but neither the
fluorescence iron emission line nor low energy excess were needed to fit the
MAXI spectra. The variation of the spectral parameters over the binary orbit
were used to examine the mode of accretion onto the neutron star in 4U 1538-52.
We deduce a best value of for QV Nor.Comment: 12 pages, 5 figures, accepted to be published by A&A, corrected typos
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