5,361 research outputs found
Modeling the RV jitter of early M dwarfs using tomographic imaging
In this paper we show how tomographic imaging (Zeeman Doppler Imaging, ZDI)
can be used to characterize stellar activity and magnetic field topologies,
ultimately allowing to filter out the radial velocity (RV) activity jitter of
M-dwarf moderate rotators. This work is based on spectropolarimetric
observations of a sample of five weakly-active early M-dwarfs (GJ 205, GJ 358,
GJ 410, GJ479, GJ 846) with HARPS-Pol and NARVAL. These stars have v sin i and
RV jitters in the range 1-2 km/s and 2.7-10.0 m/s rms respectively. Using a
modified version of ZDI applied to sets of phase-resolved Least-Squares- Decon-
volved (LSD) profiles of unpolarized spectral lines, we are able to
characterize the distribution of active regions at the stellar surfaces. We
find that darks spots cover less than 2% of the total surface of the stars of
our sample. Our technique is e cient at modeling the rotationally mod- ulated
component of the activity jitter, and succeeds at decreasing the amplitude of
this com- ponent by typical factors of 2-3 and up to 6 in optimal cases. From
the rotationally modulated time-series of circularly polarized spectra and with
ZDI, we also reconstruct the large-scale magnetic field topology. These fields
suggest that bi-stability of dynamo processes observed in active M dwarfs may
also be at work for moderately active M dwarfs. Comparing spot distributions
with field topologies suggest that dark spots causing activity jitter
concentrate at the magnetic pole and/or equator, to be confirmed with future
data on a larger sample.Comment: 34 pages, accepted for publication in MNRA
M-dwarf stellar winds: the effects of realistic magnetic geometry on rotational evolution and planets
We perform three-dimensional numerical simulations of stellar winds of
early-M dwarf stars. Our simulations incorporate observationally reconstructed
large-scale surface magnetic maps, suggesting that the complexity of the
magnetic field can play an important role in the angular momentum evolution of
the star, possibly explaining the large distribution of periods in field dM
stars, as reported in recent works. In spite of the diversity of the magnetic
field topologies among the stars in our sample, we find that stellar wind
flowing near the (rotational) equatorial plane carries most of the stellar
angular momentum, but there is no preferred colatitude contributing to mass
loss, as the mass flux is maximum at different colatitudes for different stars.
We find that more non-axisymmetric magnetic fields result in more asymmetric
mass fluxes and wind total pressures (defined as the sum of
thermal, magnetic and ram pressures). Because planetary magnetospheric sizes
are set by pressure equilibrium between the planet's magnetic field and , variations of up to a factor of in (as found in the
case of a planet orbiting at several stellar radii away from the star) lead to
variations in magnetospheric radii of about 20 percent along the planetary
orbital path. In analogy to the flux of cosmic rays that impact the Earth,
which is inversely modulated with the non-axisymmetric component of the total
open solar magnetic flux, we conclude that planets orbiting M dwarf stars like
DT~Vir, DS~Leo and GJ~182, which have significant non-axisymmetric field
components, should be the more efficiently shielded from galactic cosmic rays,
even if the planets lack a protective thick atmosphere/large magnetosphere of
their own.Comment: 16 pages, 9 figures, to appear in MNRA
Effects of light and intraspecific competition on growth and crown morphology of two size classes of understory balsam fir saplings
This paper characterizes the growth and crown morphology of young balsam fir saplings naturally regenerated under a gradient of understory light environments and intraspecific competition densities for two size classes (50-100 cm and 100-200 cm). Most growth and crown morphological parameters investigated were strongly related to the natural light gradient investigated (3-83% full sunlight), but the relationship tended to plateau at around 25% full sunlight. The relationships were generally better for the larger size class. Intraspecific competition did not significantly affect growth and crown morphology of saplings receiving less than 25% full sunlight, but it affected relative height growth, relative radial growth and the apical dominance ratio for those receiving more than 25% full sunlight (R2=0.506; p<0.001; R2=0.403; p<0.002; R2=0.348; p<0.001, respectively). These results suggest that live crown ratio, apical dominance ratio and the number of internodal branches can provide, alone or in combination, useful indicators of vigour for understory fir. Such a study provides the basic data inputs required for the development of empirically-derived mechanistic models that can predict understory tree growth and survival
Diatomées périphytiques comme indicateurs de stress combinés liés à l'historique minier et à la pression urbaine dans le bassin versant de Junction Creek (Ontario, Canada)
International audienceSudbury (Ontario, Canada) has a long mining history that has left the region with a distinctive legacy of environmental impacts. Several actions have been undertaken since the 1970s to rehabilitate this deteriorated environment, in both terrestrial and aquatic ecosystems. Despite a marked increase in environmental health, we show that the Junction Creek system remains under multiple stressors from present and past mining operations, and from urban-related pressures such as municipal wastewater treatment plants, golf courses and stormwater runoff. Water samples have elevated metal concentrations, with values reaching up to 1 mg·
Color terms: Native language semantic structure and artificial language structure formation in a large-scale online smartphone application
Artificial language games give researchers the opportunity to investigate the emergence and evolution of semantic structure, i.e. the organization of meaning spaces into discrete categories. A possible issue for this approach is that categories might simply carry over from participantsâ native languages, a potential bias that has mostly been ignored. We investigate this in a referential communication game by comparing color terms from three different languages to those of an artificial language. Here, we assess the similarity of the semantic structures, and test the influence of the semantic structure on artificial language communication. We compare the in-game communication to a separate online naming task providing us with the native language structure. Our results show that native and artificial language structure overlap at least moderately. Furthermore, communicative behavior and performance were influenced by the shared semantic structure, but only for English-speaking pairs. These results imply a cognitive link between participantsâ semantic structures and artificial language structure formation.1. Introduction - Artificial language games, semantic structure, and possible biases - Color terms and categorical facilitation 2. Method - The Color Game -- Participants -- Materials -- Procedure - Online survey -- Participants -- Materials -- Procedure - Predictions 3. Results - Prediction 1 - Prediction 2.1 - Prediction 2.2 - Prediction 2.3 - Prediction 3 4. Discussion 5. Conclusio
DeepWalk: Online Learning of Social Representations
We present DeepWalk, a novel approach for learning latent representations of
vertices in a network. These latent representations encode social relations in
a continuous vector space, which is easily exploited by statistical models.
DeepWalk generalizes recent advancements in language modeling and unsupervised
feature learning (or deep learning) from sequences of words to graphs. DeepWalk
uses local information obtained from truncated random walks to learn latent
representations by treating walks as the equivalent of sentences. We
demonstrate DeepWalk's latent representations on several multi-label network
classification tasks for social networks such as BlogCatalog, Flickr, and
YouTube. Our results show that DeepWalk outperforms challenging baselines which
are allowed a global view of the network, especially in the presence of missing
information. DeepWalk's representations can provide scores up to 10%
higher than competing methods when labeled data is sparse. In some experiments,
DeepWalk's representations are able to outperform all baseline methods while
using 60% less training data. DeepWalk is also scalable. It is an online
learning algorithm which builds useful incremental results, and is trivially
parallelizable. These qualities make it suitable for a broad class of real
world applications such as network classification, and anomaly detection.Comment: 10 pages, 5 figures, 4 table
Powerful Winds from Low-Mass Stars: V374 Peg
The rapid rotation (P=0.44 d) of the M dwarf V374Peg (M4) along with its
intense magnetic field point toward magneto-centrifugal acceleration of a
coronal wind. In this work, we investigate the structure of the wind of V374Peg
by means of 3D magnetohydrodynamical (MHD) numerical simulations. For the first
time, an observationally derived surface magnetic field map is implemented in
MHD models of stellar winds for a low mass star. We show that the wind of
V374Peg deviates greatly from a low-velocity, low-mass-loss rate solar-type
wind. We find general scaling relations for the terminal velocities, mass-loss
rates, and spin-down times of highly magnetized M dwarfs. In particular, for
V374Peg, our models show that terminal velocities across a range of stellar
latitudes reach ~(1500-2300) n_{12}^{-1/2} km/s, where n_{12} is the coronal
wind base density in units of 10^{12} cm^{-3}, while the mass-loss rates are
about 4 x 10^{-10} n_{12}^{1/2} Msun/yr. We also evaluate the angular-momentum
loss of V374Peg, which presents a rotational braking timescale ~28
n_{12}^{-1/2} Myr. Compared to observationally derived values from period
distributions of stars in open clusters, this suggests that V374Peg may have
low coronal base densities (< 10^{11} cm^{-3}). We show that the wind ram
pressure of V374Peg is about 5 orders of magnitude larger than for the solar
wind. Nevertheless, a small planetary magnetic field intensity (~ 0.1G) is able
to shield a planet orbiting at 1 AU against the erosive effects of the stellar
wind. However, planets orbiting inside the habitable zone of V374Peg, where the
wind ram pressure is higher, might be facing a more significant atmospheric
erosion. In that case, higher planetary magnetic fields of, at least, about
half the magnetic field intensity of Jupiter, are required to protect the
planet's atmosphere.Comment: 13 pages, 5 figures, 1 table. MNRAS in pres
Magnetic field and wind of Kappa Ceti: towards the planetary habitability of the young Sun when life arose on Earth
We report magnetic field measurements for Kappa1~Cet, a proxy of the young
Sun when life arose on Earth. We carry out an analysis of the magnetic
properties determined from spectropolarimetric observations and reconstruct its
large-scale surface magnetic field to derive the magnetic environment, stellar
winds and particle flux permeating the interplanetary medium around Kappa1~Cet.
Our results show a closer magnetosphere and mass-loss rate of Mdot = 9.7 x
10^{-13} Msol/yr, i.e., a factor 50 times larger than the current solar wind
mass-loss rate, resulting in a larger interaction via space weather
disturbances between the stellar wind and a hypothetical young-Earth analogue,
potentially affecting the planet's habitability. Interaction of the wind from
the young Sun with the planetary ancient magnetic field may have affected the
young Earth and its life conditionsComment: 6 pages, 5 figures, Published at the Astrophysical Journal Letters
(ApJL): Manuscript #LET3358
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