247 research outputs found
La stratégie de A à Z, 350 mots pour comprendre
L\u27ouvrage présente et illustre les 350 notions les plus représentatives du champ de la stratégie dans un style à la fois accessible et rigoureux. Il traite des différentes facettes de la stratégie : diagnostic, management stratégique, manoeuvres concurrentielles, innovation, changement, pilotage stratégique.. Chaque entrée propose la traduction anglaise du terme proposé, une présentation simple du concept et une illustration concrète. Une attention particulière est portée aux renvois entre les entrées et à leur complémentarité, afin de veiller à donner de la cohérence à l\u27ouvrage. L\u27équipe de quatre auteurs dispose de compétences et de champ d\u27intérêt très complémentaires
Optical spectroscopy of X-ray sources in the Taurus molecular cloud: discovery of ten new pre-main sequence stars
We have analyzed optical spectra of 25 X-ray sources identified as potential
new members of the Taurus molecular cloud (TMC), in order to confirm their
membership in this SFR. Fifty-seven candidates were previously selected among
the X-ray sources in the XEST survey, having a 2MASS counterpart compatible
with a PMS star based on color-magnitude and color-color diagrams. We obtained
high-resolution optical spectra for 7 of these candidates with the SARG
spectrograph at the TNG telescope, which were used to search for Li absorption
and to measure the Ha line and the radial and rotational velocities; 18
low-resolution optical spectra obtained with DOLORES for other candidate
members were used for spectral classification, for Ha measurements, and to
assess membership together with IR color-color and color-magnitude diagrams and
additional information from the X-ray data. We found that 3 sources show Li
absorption, with equivalent widths of ~500 mA, broad spectral line profiles,
indicating v sin i ~20-40 km/s, radial velocities consistent with those for
known members, and Ha emission. Two of them are classified as new WTTSs, while
the EW (~ -9 Ang) of the Ha line and its broad asymmetric profile clearly
indicate that the third star (XEST-26-062) is a CTTS. Fourteen sources observed
with DOLORES are M-type stars. Fifteen sources show Ha emission; 6 of them have
spectra that indicate surface gravity lower than in MS stars, and their
de-reddened positions in IR color-magnitude diagrams are consistent with their
derived spectral type and with PMS models at the distance of the TMC. The
K-type star XEST-11-078 is confirmed as a new member from the strength of its
Ha emission line. Overall, we confirm membership to the TMC for 10 out of 25
X-ray sources observed in the optical. Three sources remain uncertain.Comment: 15 pages, 7 figures, accepted by Astronomy & Astrophysic
Structural and compositional properties of brown dwarf disks: the case of 2MASS J04442713+2512164
In order to improve our understanding of substellar formation, we have
performed a compositional and structural study of a brown dwarf disk.
We present the result of photometric, spectroscopic and imaging observations
of 2MASS J04442713+2512164, a young brown dwarf (M7.25) member of the Taurus
association. Our dataset, combined with results from the literature, provides a
complete coverage of the spectral energy distribution from the optical to the
millimeter including the first photometric measurement of a brown dwarf disk at
3.7mm, and allows us to perform a detailed analysis of the disk properties.
The target was known to have a disk. High resolution optical spectroscopy
shows that it is intensely accreting, and powers a jet and an outflow. The disk
structure is similar to that observed for more massive TTauri stars. Spectral
decomposition models of Spitzer/IRS spectra suggest that the mid-infrared
emission from the optically thin disk layers is dominated by grains with
intermediate sizes (1.5micron). Crystalline silicates are significantly more
abondant in the outer part and/or deeper layers of the disk, implying very
efficient mixing and/or additional annealing processes. Sub-millimeter and
millimeter data indicate that most of the disk mass is in large grains (>1mm)Comment: 17 pages, 10 figures, 7 tables, accepted for A&
The Spitzer-IRAC Point Source Catalog of the Vela-D Cloud
This paper presents the observations of the Cloud D in the Vela Molecular
Ridge, obtained with the IRAC camera onboard the Spitzer Space Telescope at the
wavelengths \lambda = 3.6, 4.5, 5.8, 8.0 {\mu}m. A photometric catalog of point
sources, covering a field of approximately 1.2 square degrees, has been
extracted and complemented with additional available observational data in the
millimeter region. Previous observations of the same region, obtained with the
Spitzer MIPS camera in the photometric bands at 24 {\mu}m and 70 {\mu}m, have
also been reconsidered to allow an estimate of the spectral slope of the
sources in a wider spectral range. A total of 170,299 point sources, detected
at the 5-sigma sensitivity level in at least one of the IRAC bands, have been
reported in the catalog. There were 8796 sources for which good quality
photometry was obtained in all four IRAC bands. For this sample, a preliminary
characterization of the young stellar population based on the determination of
spectral slope is discussed; combining this with diagnostics in the
color-magnitude and color-color diagrams, the relative population of young
stellar objects in the different evolutionary classes has been estimated and a
total of 637 candidate YSOs have been selected. The main differences in their
relative abundances have been highlighted and a brief account for their spatial
distribution is given. The star formation rate has been also estimated and
compared with the values derived for other star forming regions. Finally, an
analysis of the spatial distribution of the sources by means of the two-point
correlation function shows that the younger population, constituted by the
Class I and flat-spectrum sources, is significantly more clustered than the
Class II and III sources.Comment: Accepted by Ap
Revealing The Millimeter Environment of the New FU Orionis Candidate HBC722 with the Submillimeter Array
We present 230 GHz Submillimeter Array continuum and molecular line
observations of the newly discovered FUor candidate HBC722. We report the
detection of seven 1.3 mm continuum sources in the vicinity of HBC722, none of
which correspond to HBC722 itself. We compile infrared and submillimeter
continuum photometry of each source from previous studies and conclude that
three are Class 0 embedded protostars, one is a Class I embedded protostar, one
is a Class I/II transition object, and two are either starless cores or very
young, very low luminosity protostars or first hydrostatic cores. We detect a
northwest-southeast outflow, consistent with the previous detection of such an
outflow in low-resolution, single-dish observations, and note that its axis may
be precessing. We show that this outflow is centered on and driven by one of
the nearby Class 0 sources rather than HBC722, and find no conclusive evidence
that HBC722 itself is driving an outflow. The non-detection of HBC722 in the
1.3 mm continuum observations suggests an upper limit of 0.02 solar masses for
the mass of the circumstellar disk. This limit is consistent with typical T
Tauri disks and with a disk that provides sufficient mass to power the burst.Comment: 12 pages, 7 figures, accepted by Ap
Right-invariant Sobolev metrics of fractional order on the diffeomorphism group of the circle
In this paper, we study the geodesic flow of a right-invariant metric induced
by a general Fourier multiplier on the diffeomorphism group of the circle and
on some of its homogeneous spaces. This study covers in particular
right-invariant metrics induced by Sobolev norms of fractional order. We show
that, under a certain condition on the symbol of the inertia operator (which is
satisfied for the fractional Sobolev norm for ), the
corresponding initial value problem is well-posed in the smooth category and
that the Riemannian exponential map is a smooth local diffeomorphism.
Paradigmatic examples of our general setting cover, besides all traditional
Euler equations induced by a local inertia operator, the Constantin-Lax-Majda
equation, and the Euler-Weil-Petersson equation.Comment: 40 pages. Corrected typos and improved redactio
On the nature of the EXor accretion events: an unfrequent manifestation of a common phenomenology ?
We present the results of a comparison between classical and newly identified
EXor based on literature data and aimed at recognizing possible differences or
similarities of both categories. Optical and near-IR two-color diagrams,
modalities of fluctuations, and derived values of the mass accretion rates are
indicative of strong similarities between the two samples. We demonstrate how
the difference between the outburst and the quiescence spectral energy
distribution of all the EXor can be well fitted with a single blackbody, as if
an additional thermal component appears during the outbursting phase.
Temperatures of this additional component span between 1000 and 4500 K, while
the radii of the emitting regions (assumed to be a uniform disk) span between
0.01 and 0.1 AU, sizes typical of the inner portions of the circumstellar disk.
Spots persisting up to 50% of the outburst duration, not exceeding the 10% of
the stellar surface, and with temperatures compatible with the EXor mass
accretion rates, are able to account for both the appearance of the additional
thermal component and the dust sublimation in the inner structures of the disk.
We also compare the EXor events with the most significant color and magnitude
fluctuations of active T Tauri stars finding that (i} burst accretion phenomena
should also be important for this latter class; (ii} EXor events could be more
frequent then those accidentally discovered. Remarkable is the case of the
source V2493 Cyg, a T Tauri star recently identified as a strong outbursting
object: new optical and near-IR photometric and spectroscopic data are
presented trying to clarify its EXor or FUor nature.Comment: Accepted for publication in Ap
The Taurus Spitzer Survey: New Candidate Taurus Members Selected Using Sensitive Mid-Infrared Photometry
We report on the properties of pre-main-sequence objects in the Taurus
molecular clouds as observed in 7 mid- and far-infrared bands with the Spitzer
Space Telescope. There are 215 previously-identified members of the Taurus
star-forming region in our ~44 square degree map; these members exhibit a range
of Spitzer colors that we take to define young stars still surrounded by
circumstellar dust (noting that ~20% of the bonafide Taurus members exhibit no
detectable dust excesses). We looked for new objects in the survey field with
similar Spitzer properties, aided by extensive optical, X-ray, and ultraviolet
imaging, and found 148 candidate new members of Taurus. We have obtained
follow-up spectroscopy for about half the candidate sample, thus far confirming
34 new members, 3 probable new members, and 10 possible new members, an
increase of 15-20% in Taurus members. Of the objects for which we have
spectroscopy, 7 are now confirmed extragalactic objects, and one is a
background Be star. The remaining 93 candidate objects await additional
analysis and/or data to be confirmed or rejected as Taurus members. Most of the
new members are Class II M stars and are located along the same cloud filaments
as the previously-identified Taurus members. Among non-members with Spitzer
colors similar to young, dusty stars are evolved Be stars, planetary nebulae,
carbon stars, galaxies, and AGN.Comment: Accepted to ApJS. Two large online-only figures available with the
preprint here: http://web.ipac.caltech.edu/staff/rebull/research.htm
Young Stellar Object Variability (YSOVAR): Long Timescale Variations in the Mid-Infrared
The YSOVAR (Young Stellar Object VARiability) Spitzer Space Telescope
observing program obtained the first extensive mid-infrared (3.6 & 4.5 um)
time-series photometry of the Orion Nebula Cluster plus smaller footprints in
eleven other star-forming cores (AFGL490, NGC1333, MonR2, GGD 12-15, NGC2264,
L1688, Serpens Main, Serpens South, IRAS 20050+2720, IC1396A, and Ceph C).
There are ~29,000 unique objects with light curves in either or both IRAC
channels in the YSOVAR data set. We present the data collection and reduction
for the Spitzer and ancillary data, and define the "standard sample" on which
we calculate statistics, consisting of fast cadence data, with epochs about
twice per day for ~40d. We also define a "standard sample of members",
consisting of all the IR-selected members and X-ray selected members. We
characterize the standard sample in terms of other properties, such as spectral
energy distribution shape. We use three mechanisms to identify variables in the
fast cadence data--the Stetson index, a chi^2 fit to a flat light curve, and
significant periodicity. We also identified variables on the longest timescales
possible of ~6 years, by comparing measurements taken early in the Spitzer
mission with the mean from our YSOVAR campaign. The fraction of members in each
cluster that are variable on these longest timescales is a function of the
ratio of Class I/total members in each cluster, such that clusters with a
higher fraction of Class I objects also have a higher fraction of long-term
variables. For objects with a YSOVAR-determined period and a [3.6]-[8] color,
we find that a star with a longer period is more likely than those with shorter
periods to have an IR excess. We do not find any evidence for variability that
causes [3.6]-[4.5] excesses to appear or vanish within our data; out of members
and field objects combined, at most 0.02% may have transient IR excesses.Comment: Accepted to AJ; 38 figures, 93 page
The geometry of a vorticity model equation
We provide rigorous evidence of the fact that the modified
Constantin-Lax-Majda equation modeling vortex and quasi-geostrophic dynamics
describes the geodesic flow on the subgroup of orientation-preserving
diffeomorphisms fixing one point, with respect to right-invariant metric
induced by the homogeneous Sobolev norm and show the local existence
of the geodesics in the extended group of diffeomorphisms of Sobolev class
with .Comment: 24 page
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