3,789 research outputs found
Body Size and Substrate Type Modulate Movement by the Western Pacific Crown-Of-Thorns Starfish, Acanthaster solaris
The movement capacity of the crown-of-thorns starfishes (Acanthaster spp.) is a primary determinant of both their distribution and impact on coral assemblages. We quantified individual movement rates for the Pacific crown-of-thorns starfish (Acanthaster solaris) ranging in size from 75–480 mm total diameter, across three different substrates (sand, flat consolidated pavement, and coral rubble) on the northern Great Barrier Reef. The mean (±SE) rate of movement for smaller (diameter) A. solaris was 23.99 ± 1.02 cm/ min and 33.41 ± 1.49 cm/ min for individuals \u3e350 mm total diameter. Mean (±SE) rates of movement varied with substrate type, being much higher on sand (36.53 ± 1.31 cm/ min) compared to consolidated pavement (28.04 ± 1.15 cm/ min) and slowest across coral rubble (17.25 ± 0.63 cm/ min). If average rates of movement measured here can be sustained, in combination with strong directionality, displacement distances of adult A. solaris could range from 250–520 m/ day, depending on the prevailing substrate. Sustained movement of A. solaris is, however, likely to be highly constrained by habitat heterogeneity, energetic constraints, resource availability, and diurnal patterns of activity, thereby limiting their capacity to move between reefs or habitats
WASP-44b, WASP-45b and WASP-46b: three short-period, transiting extrasolar planets
We report the discovery of three extrasolar planets that transit their
moderately bright (Vmag = 12-13) host stars. WASP-44b is a 0.89-MJup planet in
a 2.42-day orbit around a G8V star. WASP-45b is a 1.03-MJup planet which passes
in front of the limb of its K2V host star every 3.13 days. Weak Ca II H+K
emission seen in the spectra of WASP-45 suggests the star is chromospherically
active. WASP-46b is a 2.10-MJup planet in a 1.43-day orbit around a G6V star.
Rotational modulation of the light curves of WASP-46 and weak Ca II H+K
emission in its spectra show the star to be photospherically and
chromospherically active.
We imposed circular orbits in our analyses as the radial velocity data are
consistent with (near-)circular orbits, as could be expected from both
empirical and tidal-theory perspectives for such short-period, Jupiter-mass
planets. We discuss the impact of fitting for eccentric orbits for such planets
when not supported by the data. The derived planetary and stellar radii depend
on the fitted eccentricity and these parameters inform intense theoretical
efforts concerning tidal circularisation and heating, bulk planetary
composition and the observed systematic errors in planetary and stellar radii.
As such, we recommend exercising caution in fitting the orbits of short period,
Jupiter-mass planets with an eccentric model when there is no evidence of
non-circularity.Comment: 12 pages, 8 figures, 6 tables. As accepted for publication in MNRA
Characterisation of the microbiome along the gastrointestinal tract of growing turkeys
The turkey microbiome is largely understudied, despite its relationship with bird health and growth, and the prevalence of human pathogens such as Campylobacter spp. In this study we investigated the microbiome within the small intestine (SI), caeca (C), large intestine (LI) and cloaca (CL) of turkeys at 6, 10 and 16 weeks of age. Eight turkeys were dissected within each age category and the contents of the SI, C, LI and CL were harvested. 16S rDNA based QPCR was performed on all samples and samples for the 4 locations within 3 birds/age group were sequenced using ion torrent-based sequencing of the 16S rDNA. Sequencing data showed on a genus level, an abundance of Lactobacillus, Streptococcus and Clostridium XI (38.2, 28.1 and 13.0% respectively) irrespective of location and age. The caeca exhibited the greatest microbiome diversity throughout the development of the turkey. PICRUSt data predicted an array of bacterial function, with most differences being apparent in the caeca of the turkeys as they matured. QPCR revealed that the caeca within 10 week old birds, contained the most Campylobacter spp. Understanding the microbial ecology of the turkey gastrointestinal tract is essential in terms of understanding production efficiency and in order to develop novel strategies for targeting Campylobacter spppublishersversionPeer reviewe
Thermonuclear Kinetics in Astrophysics
Over the billions of years since the Big Bang, the lives, deaths and
afterlives of stars have enriched the Universe in the heavy elements that make
up so much of ourselves and our world. This review summarizes the methods used
to evolve these nuclear abundances within astrophysical simulations. These
methods fall into 2 categories; evolution via rate equations and via
equilibria. Because the rate equations in nucleosynthetic applications involve
a wide range of timescales, implicit methods have proven mandatory, leading to
the need to solve matrix equations. Efforts to improve the performance of such
rate equation methods are focused on efficient solution of these matrix
equations, in particular by making best use of the sparseness of these
matrices, and finding methods that require less frequent matrix solutions.
Recent work to produce hybrid schemes which use local equilibria to reduce the
computational cost of the rate equations is also discussed. Such schemes offer
significant improvements in the speed of reaction networks and are accurate
under circumstances where calculations which assume complete equilibrium fail.Comment: 27 pages, 2 figures, a review for a special issue of Nuclear Physics
Thermal emission from WASP-24b at 3.6 and 4.5 {\mu}m
Aims. We observe occultations of WASP-24b to measure brightness temperatures
and to determine whether or not its atmosphere exhibits a thermal inversion
(stratosphere). Methods. We observed occultations of WASP-24b at 3.6 and 4.5
{\mu}m using the Spitzer Space Telescope. It has been suggested that there is a
correlation between stellar activity and the presence of inversions, so we
analysed existing HARPS spectra in order to calculate log R'HK for WASP-24 and
thus determine whether or not the star is chromospherically active. We also
observed a transit of WASP-24b in the Str\"{o}mgren u and y bands, with the
CAHA 2.2-m telescope. Results. We measure occultation depths of 0.159 \pm 0.013
per cent at 3.6 {\mu}m and 0.202 \pm 0.018 per cent at 4.5 {\mu}m. The
corresponding planetary brightness temperatures are 1974 \pm 71 K and 1944 \pm
85 K respectively. Atmosphere models with and without a thermal inversion fit
the data equally well; we are unable to constrain the presence of an inversion
without additional occultation measurements in the near-IR. We find log R'HK =
-4.98 \pm 0.12, indicating that WASP-24 is not a chromospherically active star.
Our global analysis of new and previously-published data has refined the system
parameters, and we find no evidence that the orbit of WASP-24b is non-circular.
Conclusions. These results emphasise the importance of complementing Spitzer
measurements with observations at shorter wavelengths to gain a full
understanding of hot Jupiter atmospheres.Comment: 7 pages, 4 figures, 3 tables. Accepted for publication in A&
Explosive Nucleosynthesis: What we learned and what we still do not understand
This review touches on historical aspects, going back to the early days of
nuclear astrophysics, initiated by BFH and Cameron, discusses (i) the
required nuclear input from reaction rates and decay properties up to the
nuclear equation of state, continues (ii) with the tools to perform
nucleosynthesis calculations and (iii) early parametrized nucleosynthesis
studies, before (iv) reliable stellar models became available for the late
stages of stellar evolution. It passes then through (v) explosive environments
from core-collapse supernovae to explosive events in binary systems (including
type Ia supernovae and compact binary mergers), and finally (vi) discusses the
role of all these nucleosynthesis production sites in the evolution of
galaxies. The focus is put on the comparison of early ideas and present, very
recent, understanding.Comment: 11 pages, to appear in Springer Proceedings in Physics (Proc. of
Intl. Conf. "Nuclei in the Cosmos XV", LNGS Assergi, Italy, June 2018
Constraints on dark matter models from a Fermi LAT search for high-energy cosmic-ray electrons from the Sun
During its first year of data taking, the Large Area Telescope (LAT) onboard
the Fermi Gamma-Ray Space Telescope has collected a large sample of high-energy
cosmic-ray electrons and positrons (CREs). We present the results of a
directional analysis of the CRE events, in which we searched for a flux excess
correlated with the direction of the Sun. Two different and complementary
analysis approaches were implemented, and neither yielded evidence of a
significant CRE flux excess from the Sun. We derive upper limits on the CRE
flux from the Sun's direction, and use these bounds to constrain two classes of
dark matter models which predict a solar CRE flux: (1) models in which dark
matter annihilates to CREs via a light intermediate state, and (2) inelastic
dark matter models in which dark matter annihilates to CREs.Comment: 18 pages, 8 figures, accepted for publication in Physical Review D -
contact authors: Francesco Loparco ([email protected]), M. Nicola Mazziotta
([email protected]) and Jennifer Siegal-Gaskins ([email protected]
Measurement of the rate of nu_e + d --> p + p + e^- interactions produced by 8B solar neutrinos at the Sudbury Neutrino Observatory
Solar neutrinos from the decay of B have been detected at the Sudbury
Neutrino Observatory (SNO) via the charged current (CC) reaction on deuterium
and by the elastic scattering (ES) of electrons. The CC reaction is sensitive
exclusively to nu_e's, while the ES reaction also has a small sensitivity to
nu_mu's and nu_tau's. The flux of nu_e's from ^8B decay measured by the CC
reaction rate is
\phi^CC(nu_e) = 1.75 +/- 0.07 (stat)+0.12/-0.11 (sys.) +/- 0.05(theor) x 10^6
/cm^2 s.
Assuming no flavor transformation, the flux inferred from the ES reaction
rate is
\phi^ES(nu_x) = 2.39+/-0.34 (stat.)+0.16}/-0.14 (sys) x 10^6 /cm^2 s.
Comparison of \phi^CC(nu_e) to the Super-Kamiokande Collaboration's precision
value of \phi^ES(\nu_x) yields a 3.3 sigma difference, providing evidence that
there is a non-electron flavor active neutrino component in the solar flux. The
total flux of active ^8B neutrinos is thus determined to be 5.44 +/-0.99 x
10^6/cm^2 s, in close agreement with the predictions of solar models.Comment: 6 pages (LaTex), 3 figures, submitted to Phys. Rev. Letter
Detection and Characterization of Extrasolar Planets through Doppler Spectroscopy
Over 300 extrasolar planets have been found since 1992, showing that
planetary systems are common and exhibit an outstanding variety of
characteristics. As the number of detections grows and as models of planet
formation progress to account for the existence of these new worlds,
statistical studies and confrontations of observation with theory allow to
progressively unravel the key processes underlying planet formation. In this
chapter we review the dominant contribution of Doppler spectroscopy to the
present discoveries and to our general understanding of planetary systems. We
also emphasize the synergy of Doppler spectroscopy and transit photometry in
characterizing the physical properties of transiting extrasolar planets. As we
will see, Doppler spectroscopy has not reached its limits yet and it will
undoubtly play a leading role in the detection and characterization of the
first Earth-mass planets.Comment: 50 pages, 16 figures, to appear in the proceedings of the Les Houches
Winter School "Physics and Astrophysics of Planetary Systems" (EDP Sciences:
EAS Publications Series
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