4,543 research outputs found
CHEOPS performance for exomoons: The detectability of exomoons by using optimal decision algorithm
Many attempts have already been made for detecting exomoons around transiting
exoplanets but the first confirmed discovery is still pending. The experience
that have been gathered so far allow us to better optimize future space
telescopes for this challenge, already during the development phase. In this
paper we focus on the forthcoming CHaraterising ExOPlanet Satellite
(CHEOPS),describing an optimized decision algorithm with step-by-step
evaluation, and calculating the number of required transits for an exomoon
detection for various planet-moon configurations that can be observable by
CHEOPS. We explore the most efficient way for such an observation which
minimizes the cost in observing time. Our study is based on PTV observations
(photocentric transit timing variation, Szab\'o et al. 2006) in simulated
CHEOPS data, but the recipe does not depend on the actual detection method, and
it can be substituted with e.g. the photodynamical method for later
applications. Using the current state-of-the-art level simulation of CHEOPS
data we analyzed transit observation sets for different star-planet-moon
configurations and performed a bootstrap analysis to determine their detection
statistics. We have found that the detection limit is around an Earth-sized
moon. In the case of favorable spatial configurations, systems with at least
such a large moon and with at least Neptune-sized planet, 80\% detection chance
requires at least 5-6 transit observations on average. There is also non-zero
chance in the case of smaller moons, but the detection statistics deteriorates
rapidly, while the necessary transit measurements increase fast. (abridged)Comment: 32 pages, 14 figures, accepted for publication in PAS
Characterizations of quasitrivial symmetric nondecreasing associative operations
We provide a description of the class of n-ary operations on an arbitrary
chain that are quasitrivial, symmetric, nondecreasing, and associative. We also
prove that associativity can be replaced with bisymmetry in the definition of
this class. Finally we investigate the special situation where the chain is
finite
Measurement induced chaos with entangled states
The dynamics of an ensemble of identically prepared two-qubit systems is
investigated which is subjected to the iteratively applied measurements and
conditional selection of a typical entanglement purification protocol. It is
shown that the resulting measurement-induced non-linear dynamics of the
two-qubit state exhibits strong sensitivity to initial conditions and also true
chaos. For a special class of initially prepared two-qubit states two types of
islands characterize the asymptotic limit. They correspond to a separable and a
maximally entangled two-qubit state, respectively, and their boundaries form
fractal-like structures. In the presence of incoherent noise an additional
stable asymptotic cycle appears.Comment: 5 pages, 3 figure
Investigation of alpha-nuclear potential families from elastic scattering experiments
In this work we present the continuation of the reported analysis [1] of the experimentally measured angular distributions of the reaction Cd-106(alpha, alpha)Cd-106 at several different energies around the Coulomb barrier. The difficulties that arise in the study of Cd-106-alpha-nuclear potential and the so called Family Problem are addressed
Conditions for one-dimensional supersonic flow of quantum gases
One can use transsonic Bose-Einstein condensates of alkali atoms to establish
the laboratory analog of the event horizon and to measure the acoustic version
of Hawking radiation. We determine the conditions for supersonic flow and the
Hawking temperature for realistic condensates on waveguides where an external
potential plays the role of a supersonic nozzle. The transition to supersonic
speed occurs at the potential maximum and the Hawking temperature is entirely
determined by the curvature of the potential
Alpha-induced cross sections of 106Cd for the astrophysical p-process
The 106Cd(alpha,gamma)110Sn reaction cross section has been measured in the
energy range of the Gamow window for the astrophysical p-process scenario. The
cross sections for 106Cd(alpha,n)109Sn and for 106Cd(alpha,p)109In below the
(alpha,n) threshold have also been determined. The results are compared with
predictions of the statistical model code NON-SMOKER using different input
parameters. The comparison shows that a discrepancy for 106Cd(alpha,gamma)110Sn
when using the standard optical potentials can be removed with a different
alpha+106Cd potential. Some astrophysical implications are discussed.Comment: 10 pages, 9 figures, accepted for publication in Phys. Rev
Alpha-induced reactions for the astrophysical p-process: the case of 151Eu
The cross sections of 151Eu(alpha,gamma)155Tb and 151Eu(alpha,n)154Tb
reactions have been measured with the activation method. Some aspects of the
measurement are presented here to illustrate the requirements of experimental
techniques needed to obtain nuclear data for the astrophysical p-process
nucleosynthesis. Preliminary cross section results are also presented and
compared with the predictions of statistical model calculations.Comment: Accepted for publication in Journal of Physics Conference Series,
proceeding of the Nuclear Physics in Astrophysics IV. conferenc
The period-luminosity relation of red supergiants with Gaia DR2
We revisit the K -band period-luminosity (P-L) relations of Galactic red
supergiants using Gaia Data Release 2 parallaxes and up to 70 yr of photometry
from AAVSO and ASAS campaigns. In addition, we examine 206 LMC red supergiants
using 50 yr of photometric data from the Digitised Harvard Astronomical Plate
Collection. We identified periods by computing power spectra and calculated the
period-luminosity relations of our samples and compared them with the
literature. Newly available data tighten the P-L relations substantially.
Identified periods form two groups: one with periods of 300-1000 days,
corresponding to pulsations, and another with Long Secondary Periods between
1000 and 8000 days. Among the 48 Galactic objects we find shorter periods in 25
stars and long secondary periods in 23 stars. In the LMC sample we identify 85
and 94 red supergiants with shorter and long secondary periods, respectively.
The P-L relation of the Galactic red supergiants is in agreement with the red
supergiants in both, the Large Magellanic Cloud and the Andromeda Galaxy. We
and no clear continuity between the known red giant period-luminosity
sequences, and the red supergiant sequences investigated here.Comment: Resubmitted with the supplementary material. Acknowledgements section
and affiliations have been update
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