144,944 research outputs found
Rapidly rotating red giants
Stellar oscillations give seismic information on the internal properties of
stars. Red giants are targets of interest since they present mixed modes, which
behave as pressure modes in the convective envelope and as gravity modes in the
radiative core. Mixed modes thus directly probe red giant cores, and allow in
particular the study of their mean core rotation. The high-quality data
obtained by CoRoT and Kepler satellites represent an unprecedented perspective
to obtain thousands of measurements of red giant core rotation, in order to
improve our understanding of stellar physics in deep stellar interiors. We
developed an automated method to obtain such core rotation measurements and
validated it for stars on the red giant branch. In this work, we particularly
focus on the specific application of this method to red giants having a rapid
core rotation. They show complex spectra where it is tricky to disentangle
rotational splittings from mixed-mode period spacings. We demonstrate that the
method based on the identification of mode crossings is precise and efficient.
The determination of the mean core rotation directly derives from the precise
measurement of the asymptotic period spacing {\Delta}{\Pi}1 and of the
frequency at which the crossing of the rotational components is observed.Comment: 4 pages, 2 figures, 2 tables, to be published in the Astro Fluid 2016
Conference Proceedings, editor EAS Publications Serie
A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler
Asteroseismology with the Kepler space telescope is providing not only an
improved characterization of exoplanets and their host stars, but also a new
window on stellar structure and evolution for the large sample of solar-type
stars in the field. We perform a uniform analysis of 22 of the brightest
asteroseismic targets with the highest signal-to-noise ratio observed for 1
month each during the first year of the mission, and we quantify the precision
and relative accuracy of asteroseismic determinations of the stellar radius,
mass, and age that are possible using various methods. We present the
properties of each star in the sample derived from an automated analysis of the
individual oscillation frequencies and other observational constraints using
the Asteroseismic Modeling Portal (AMP), and we compare them to the results of
model-grid-based methods that fit the global oscillation properties. We find
that fitting the individual frequencies typically yields asteroseismic radii
and masses to \sim1% precision, and ages to \sim2.5% precision (respectively 2,
5, and 8 times better than fitting the global oscillation properties). The
absolute level of agreement between the results from different approaches is
also encouraging, with model-grid-based methods yielding slightly smaller
estimates of the radius and mass and slightly older values for the stellar age
relative to AMP, which computes a large number of dedicated models for each
star. The sample of targets for which this type of analysis is possible will
grow as longer data sets are obtained during the remainder of the mission.Comment: 13 pages, 5 figures in the main text, 22 figures in Appendix.
Accepted for publication in Ap
Meeting the Challenge of Interdependent Critical Networks under Threat : The Paris Initiative
NARisques à grande échelle;Gestion des crises internationale;Interdépendances;Infrastructures critiques;Anthrax;Initiative collective;Stratégie;Préparation des Etats-majors
Oscillations in the Sun with SONG: Setting the scale for asteroseismic investigations
Context. We present the first high-cadence multi-wavelength radial-velocity
observations of the Sun-as-a-star, carried out during 57 consecutive days using
the stellar \'echelle spectrograph at the Hertzsprung SONG Telescope operating
at the Teide Observatory. Aims. The aim was to produce a high-quality data set
and reference values for the global helioseismic parameters {\nu_{max}}, and
{\Delta \nu} of the solar p-modes using the SONG instrument. The obtained data
set or the inferred values should then be used when the scaling relations are
applied to other stars showing solar-like oscillations which are observed with
SONG or similar instruments. Methods. We used different approaches to analyse
the power spectrum of the time series to determine {\nu_{max}}; simple Gaussian
fitting and heavy smoothing of the power spectrum. {\Delta\nu} was determined
using the method of autocorrelation of the power spectrum. The amplitude per
radial mode was determined using the method described in Kjeldsen et al.
(2008). Results. We found the following values for the solar oscillations using
the SONG spectrograph: {\nu_{max}} = 3141 {\pm} 12 {\mu}Hz, {\Delta\nu} =
134.98 {\pm} 0.04 {\mu}Hz and an average amplitude of the strongest radial
modes of 16.6 {\pm} 0.4 cm/s. These values are consistent with previous
measurements with other techniques.Comment: 5 pages, 5 figures, letter accepted for A&
Wetting morphologies on randomly oriented fibers
We characterize the different morphologies adopted by a drop of liquid placed
on two randomly oriented fibers, which is a first step toward understanding the
wetting of fibrous networks. The present work reviews previous modeling for
parallel and touching crossed fibers and extends it to an arbitrary orientation
of the fibers characterized by the tilting angle and the minimum spacing
distance. Depending on the volume of liquid, the spacing distance between
fibers and the angle between the fibers, we highlight that the liquid can adopt
three different equilibrium morphologies: (1) a column morphology in which the
liquid spreads between the fibers, (2) a mixed morphology where a drop grows at
one end of the column or (3) a single drop located at the node. We capture the
different morphologies observed using an analytical model that predicts the
equilibrium configuration of the liquid based on the geometry of the fibers and
the volume of liquid
Spectroscopic and photometric analysis of the early-type spectroscopic binary HD 161853 in the centre of an H II region
We study the O-type star HD 161853, which has been noted as a probable
double-lined spectroscopic binary system. We secured high-resolution spectra of
HD 161853 during the past nine years. We separated the two components in the
system and measured their respective radial velocities for the first time. We
confirm that HD 161853 is an 1 Ma old binary system consisting of an O8 V
star ( M) and a B1--3 V star ( M) at about 1.3 kpc. From the radial velocity curve, we measure an
orbital period = 2.667650.00001 d and an eccentricity =
0.1210.007. Its -band light curve is constant within 0.014 mag and does
not display eclipses, from which we impose a maximum orbital inclination
deg. HD 161853 is probably associated with an H II region and a poorly
investigated very young open cluster. In addition, we detect a compact emission
region at 50 arcsec to HD 161853 in 22m-WISE and 24m-Spitzer images,
which may be identified as a dust wave piled up by the radiation pressure of
the massive binary system.Comment: 5 pages, 4 figures, to appear in A&
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