pinecone/core-2020-05-10-deduplication huggingface dataset:
The Deep Underground Neutrino Experiment -- DUNE: the precision era of
  neutrino physics

The last decade was remarkable for neutrino physics. In particular, the
phenomenon of neutrino flavor oscillations has been firmly established by a
series of independent measurements. All parameters of the neutrino mixing are
now known and we have elements to plan a judicious exploration of new scenarios
that are opened by these recent advances. With precise measurements, we can
test the 3-neutrino paradigm, neutrino mass hierarchy and CP asymmetry in the
lepton sector. The future long-baseline experiments are considered to be a
fundamental tool to deepen our knowledge of electroweak interactions. The Deep
Underground Neutrino Experiment -- DUNE will detect a broad-band neutrino beam
from Fermilab in an underground massive Liquid Argon Time-Projection Chamber at
an L/E of about $10^3$ km / GeV to reach good sensitivity for CP-phase
measurements and the determination of the mass hierarchy. The dimensions and
the depth of the Far Detector also create an excellent opportunity to look for
rare signals like proton decay to study violation of baryonic number, as well
as supernova neutrino bursts, broadening the scope of the experiment to
astrophysics and associated impacts in cosmology. In this presentation, we will
discuss the physics motivations and the main experimental features of the DUNE
project required to reach its scientific goals.Comment: To appear in the proceedings of STARS 2017 symposium
  (https://indico.cern.ch/event/542644/
Cross-tests of CMB features in the primordial spectra

The recent Planck data on the power spectrum of temperature anisotropies of
the cosmic microwave background marginally support deviations from the
$\Lambda$CDM model at several multipoles. With a view towards current and
forthcoming observational surveys, we trace these features to other observables
like the scalar bispectrum and the tensor power spectrum. A possible detection
of such bumps in these channels would increase their statistical significance
shedding light on the ultra violet mechanisms responsible for their appearance
in the data.Comment: 7 pp., 1 figure. Contribution to the proceedings of "STARS2017 - 4th
  Caribbean Symposium on Cosmology, Gravitation, Nuclear and Astroparticle
  Physics / SMFNS2017 - 5th International Symposium on Strong Electromagnetic
  Fields and Neutron Stars", 7 to 13 of May, 2017, Havana and Varadero, Cuba.
  Talk also given in PASCOS-17 and COSMO-1
Mixed Phase within the Multi-polytrope Approach to High Mass Twins

We present a multi-polytrope approach to describe high-mass twins fulfilling
chiral effective field theory estimations of the neutron star equation state
and test it against the appearance of mixed phases at the hadron-quark
interface. In addition, we discuss astrophysical applications of this method
and expected future measurements that shall further constrain neutron star
matter and the understanding of the QCD phase diagram.Comment: 6 pages, 2 figures, Proceedings of the Conference "STARS2017 - 4th
  Caribbean Symposium on Cosmology, Gravitation, Nuclear and Astroparticle
  Physics / SMFNS2017 - 5th International Symposium on Strong Electromagnetic
  Fields and Neutron Stars", 7 to 13 of May, 2017, Havana and Varadero, Cub
The Magnetic Field Distribution in Strongly Magnetized Neutron Stars

In this work, we expand on a previously reported realistic calculation of the
magnetic field profile for the equation of state inside strongly magnetized
neutron stars. In addition to showing that magnetic fields increase
quadratically with increasing baryon chemical potential of magnetized matter
(instead of exponentially, as previously assumed), we show here that the
magnetic field increase with baryon number density is more complex and harder
to model. We do so by the analysis of several different realistic models for
the microscopic description of matter in the star (including hadronic, hybrid
and quark models) combined with general relativistic solutions by solving
Einstein-Maxwell's field equations in a self-consistent way for stars endowed
with a poloidal magnetic field.Comment: Proceedings of the 4th Caribbean Symposium on Cosmology, Gravitation,
  Nuclear and Astroparticle Physics (STARS2017) and 5th International Symposium
  on Strong Electromagnetic Fields and Neutron Stars (SMFNS2017
Could the low braking index pulsar PSR J1734-3333 evolve into a
  magnetar?

The low braking-index pulsar PSR J1734$-$3333 could be born with superhigh
internal magnetic fields $B_{\rm in}\sim10^{15}-10^{16}$ G, and undergo a
supercritical accretion soon after its formation in a supernova explosion. The
buried multipole magnetic fields will merger into a dipole magnetic field.
Since the magnetic flow transfers from the core to the crust of the pulsar, its
surface dipole field grows quickly at a power-law form assumed until it
saturates at the level of internal dipole field. The increase in surface dipole
magnetic field results in the observed low braking index of $n=0.9(2)$. Keeping
an average field growth index $\varepsilon=1.34(6)$, this pulsar will become a
magnetar with surface dipole magnetic field at the equator $B_{\rm d}\sim
2.6(1)\times 10^{14}$\,G and $\sim 5.3(2)\times 10^{14}$\,G after next 50\,kyrs
and 100\,kys, respectively.Comment: 2017 Astron. Nachr. DOI:10.1002/asna.20171343
Reinvestigation of the electron fraction and electron Fermi energy of
  neutron star

In this work, we reinvestigate the electron fraction $Y_{e}$ and electron
Fermi energy $E_{F}(e)$ of neutron stars, based on our previous work of Li et
al.(2016), in which we firstly deduced a special solution to $E_{F}(e)$, and
then obtained several useful analytical formulae for $Y_{\rm e}$ and matter
density $\rho$ within classical models and the relativistic mean field(RMF)
theory using numerically fitting. The advantages of this work include the
following aspects:(1) The linear functions are substituted for the nonlinear
exponential functions used in the previous work. This method may be more
simple, and closer to realistic equation of state\,(EoS) of a neutron star(NS),
because there are linear or quasi-linear relationships between number fractions
of leptons and matter density, which can be seen by solving NS EoS; (2)we
introduce a dimensionless variable $\varrho$\,($\varrho=\rho/\rho_0$,
$\rho_{0}$ is the standard saturated nuclear density), which greatly reduces
the scope of the fitting coefficients;(3)we present numerical errors including
absolute and relative deviations between the data and fit. By numerically
simulating, we have obtained several analytical formulae for $Y_{e}$ and $\rho$
for both APR98 and RMF models. Combining these analytical formulae with the
special solution, we can calculate the value of $E_{\rm F}(e)$ for any given
matter density. Since $Y_e$ and $E_{ F}(e)$ are important in assessing cooling
rate of a NS and the possibility of kaon/pion condensation in the NS interior,
this study could be useful in the future study on the thermal evolution of a
NS.Comment: 3 figures, 3 tables , and We welcome any comment you might have about
  the content, To be published in Astron. Nach
Fluxtube Dynamics in Neutron Star Cores

Although the detailed structure of neutron stars remains unknown, their
equilibrium temperatures lie well below the Fermi temperature of dense nuclear
matter, suggesting that the nucleons in the stars' core form Cooper pairs and
exhibit macroscopic quantum behavior. The presence of such condensates impacts
on the neutron stars' large scale properties. Specifically, superconducting
protons in the outer core (expected to show type-II properties) alter the
stars' magnetism as the magnetic field is no longer locked to the charged
plasma but instead confined to fluxtubes. The motion of these structures
governs the dynamics of the core magnetic field. To examine if field evolution
could be driven on observable timescales, several mechanisms affecting the
fluxtube distribution are addressed and characteristic timescales for realistic
equations of state estimated. The results suggest that the corresponding
timescales are not constant but vary for different densities inside the star,
generally being shortest close to the crust-core interface.Comment: Proceedings of the 4th Caribbean Symposium on Cosmology, Gravitation,
  Nuclear and Astroparticle Physics (STARS2017) and 5th International Symposium
  on Strong Electromagnetic Fields and Neutron Stars (SMFNS2017
Magneto-elastic oscillations modulating the emission of magnetars

Magneto-elastic oscillations of neutron stars are believed to explain
observed quasi-periodic oscillations (QPOs) in the decaying tail of the giant
flares of highly magnetized neutron stars (magnetars). Strong efforts of the
theoretical modelling from different groups have increased our understanding of
this phenomenon significantly. Here, we discuss some constraints on the matter
in neutron stars that arise if the interpretation of the observations in terms
of superfluid, magneto-elastic oscillations is correct. To explain the observed
modulation of the light curve of the giant flare, we describe a model that
allows the QPOs to couple to the stellar exterior through the magnetic field.
In this magnetosphere, the shaking magnetic field induces currents that provide
scattering targets for resonant cyclotron scattering of photons, which is
calculated with a Monte-Carlo approach and coupled to a code that calculates
the momentum distribution of the charge carriers as a one-dimensional
accelerator problem. We show first results of a simplified, but self-consistent
momentum distribution, i.e. a waterbag distribution, and of the corresponding
spectra.Comment: 7 pages, 4 figures, proceedings of stars2017 and 2017smfn
Detection of a centrifugal magnetosphere in one of the most massive
  stars in the $\rho$ Oph star-forming cloud

Recent XMM-Newton observations of the B2 type star rho Oph A indicated a
periodicity of 1.205d, which was ascribed to rotational modulation. Since
variability of X-ray emission in massive stars is frequently the signature of a
magnetic field, we investigated whether the presence of a magnetic field can
indeed be invoked to explain the observed X-ray peculiarity. Two FORS2
spectropolarimetric observations in different rotation phases revealed the
presence of a negative (<B_z>_all=-419+-101G) and positive (<B_z>_all=538+-69G)
longitudinal magnetic field, respectively. We estimate a lower limit for the
dipole strength as B_d = 1.9+-0.2kG. Our calculations of the Kepler and Alfven
radii imply the presence of a centrifugally supported, magnetically confined
plasma around rho Oph A. The study of the spectral variability indicates a
behaviour similar to that observed in typical magnetic early-type Bp stars.Comment: 7 pages, 1 table, 5 figures, accepted for publication in A
Testing pseudo-complex general relativity with gravitational waves

We show how the model of pseudo-complex general relativity can be tested
using gravitational wave signals from coalescing compact objects. The model,
which agrees with Einstein gravity in the weak-field limit, diverges
dramatically in the near-horizon regime, with certain parameter ranges
excluding the existence of black holes. We show that simple limits can be
placed on the model in both the inspiral and ringdown phase of coalescing
compact objects. We discuss further how these bounds relate to current
observational limits. In particular, for minimal scenarios previously
considered in the literature, gravitational wave observations are able to
constrain pseudo-complex general relativity parameters to values that require
the existence of black hole horizons
Inhomogeneous Cosmological Models Containing Homogeneous Inner
  Hypersurface Geometry. Changes of the Bianchi Type

There are investigated such cosmological models which instead of the usual
spatial homogeneity property only fulfil the condition that in a certain
synchronized system of reference all spacelike sections t = const. are
homogeneous manifolds. This allows time-dependent changes of the BIANCHI type.
Discussing differential geometrical theorems it is shown which of them are
permitted. Besides the trivial case of changing into type I there exist some
possible changes between other types. However, physical reasons like energy
inequalities partially exclude them.Comment: 10 pages, LaTeX, 1 figur
Comparing selfinteracting scalar fields and R + R^3 cosmological models

We generalize the well-known analogies between m^2 \phi^2 and R + R^2
theories to include the selfinteraction \lambda \phi^4-term for the scalar
field. It turns out to be the R + R^3 Lagrangian which gives an appropriate
model for it. Considering a spatially flat Friedman cosmological model, common
and different properties of these models are discussed, e.g., by linearizing
around a ground state the masses of the resp. spin 0-parts coincide. Finally,
we prove a general conformal equivalence theorem between a Lagrangian L = L(R),
L'L" \ne 0, and a minimally coupled scalar field in a general potential.Comment: 16 pages, LaTe
Phase-resolved spectroscopy and photometry of the eclipsing polar EP Draconis (=H1907+690)

We present phase-resolved optical spectroscopy and CCD photometry of the faint eclipsing polar EP Dra (H1907+690). A revised ephemeris is derived which connects all 32000 binary cycles since its discovery by Remillard et al. (1991). We found no difference between spin and and orbital periods of the white dwarf. Changes in the light curve morphology are attributed to a different beaming behaviour which might change on timescales as short as one or several orbital periods. Optical light curve modelling was used to estimate the co-latitude of the accretion spot, which must be larger than 40 degrees. We have detected Zeeman absorption lines of Halpha originating in an accretion halo in a field of 16MG. The low-resolution spectra reveal no indication of resolved cyclotron harmonics, which is also suggestive of a relatively low field strength in the accretion region. The Balmer emission lines contain significant contributions from the UV-illuminated hemisphere of the companion star, whereas the HeII4686 emission originates predominantly from the accretion stream. The emission lines have a multi-component structure and we could single out a narrow emission line in the Hbeta and Hgamma lines. Its radial velocity amplitude suggests a low mass for the white dwarf, if the lines are interpreted as being of reprocessed origin from the whole illuminated hemisphere of the companion star
Cyclotron spectroscopy of VV Puppis

We present phase-resolved spectrophotometric observations of VV Puppis obtained during two different states of accretion. We confirm the detection of cyclotron lines from emission regions at both poles (Wickramasinghe et al. 1989) having significantly different field strength of B_1 ~ 31MG and B_2 ~ 54MG. Our phase-resolved data allowed the detection of phase-dependent wavelength shifts of the cyclotron lines from the main accretion pole which is due to the varying aspect of the observer. A corresponding motion of the cyclotron lines from the secondary pole appears likely. Compared to 1984, the cyclotron lines from the main pole appeared redshifted in 1989, during an episode of higher system brightness. This shift can be explained assuming either different locations of the accretion spot and, hence, variations of the magnetic field, or variations of the plasma temperature both triggered by variations of the mass accretion rate. The cyclotron lines from the second pole do not show such changes suggesting that the coupling region for the weakly accreting pole is more or less stationary whereas the coupling region of the main pole varies in space, most likely depending on the mass accretion rate
ROSAT Public PSPC Observations in the Las Campanas Redshift Survey

The Las Campanas Redshift Survey, an optically selected survey which contains 26,418 galaxy redshifts, has been correlated with ``The First ROSAT Source Catalogue of Pointed Observations with the PSPC,'' which contains 50,408 sources from 2876 ROSAT pointed observations. Ten matches were found. The optical spectra of most of the ten matches show weak narrow emission lines. Due to their high x-ray luminosities, their high x-ray--to--optical flux ratios, and the evidence of rapid x-ray variability in the two brightest matches, we interpret the majority of these objects to be narrow-line Seyfert galaxies or ``hidden'' active galactic nuclei. Of the ten matches, only one galaxy shows the characteristics of a bona fide starburst
Faint galaxies and the X-ray background

We summarise our recent work on the faint galaxy contribution to the cosmic X-ray background (XRB). At bright X-ray fluxes (in the ROSAT pass band), broad line QSOs dominate the X-ray source population, but at fainter fluxes there is evidence for a significant contribution from emission-line galaxies. Here we present statistical evidence that these galaxies can account for a large fraction of the XRB. We also demonstrate that these galaxies have significantly harder X-ray spectra than QSOs. Finally we present preliminary findings from infra-red spectroscopy on the nature of this X-ray emitting galaxy population. We conclude that a hybrid explanation consisting of obscured/Type 2 AGN surrounded by starburst activity can explain the properties of these galaxies and perhaps the origin of the entire XRB
Present Epoch Plus: An X-ray Survey for Cosmology

This paper summarizes some cosmologically interesting measurements which are uniquely possible in the hard X-ray band and presents a mission concept capable of achieving them. The Present Epoch Plus mission will achieve a surface brightness sensitivity of better than 1% per square degree in the 2-10 keV band, and create a catalog of about 10^6 sources. About 160,000 extragalactic sources are expected to be detected in the 2-10 keV band, providing an all sky survey with nearly uniform selection effects 10 times deeper than exisiting or planned surveys. The PEP concept can be achieved within the size and budgetary constraints of a NASA Medium Explorer (MIDEX) mission
A new X-ray mission to measure the power spectrum of fluctuations in the Universe

We propose a new, simple, dedicated X-ray mission to measure the power spectrum of density fluctuations in the Universe, by accurately mapping the X-ray background on the whole sky on scales of arounf one sq deg. Since the method relies on the detection of excess fluctuations produced by the clustering of X-ray sources at intermediate redshifts above the confusion noise produced by bright foreground sources, counting noise and systematic noise need to be kept to a minimum. We propose a proportional counter with collimated fields of view of various sizes as the optimal instrument for this mission
Early versus late type galaxies in compact groups

We find a strong correlation between the effective radius of the largest early-type galaxies in compact groups of galaxies and the velocity dispersion of the groups. The lack of a similar correlation for late type galaxies is supportive of the so called second generation merging scenario which predicts that ellipticals should dominate the internal dynamics of the groups, while late-type galaxies are mainly recent interlopers which are still in an early stage of interaction with the group potential
Novel methods and the maximum likelihood estimation technique for estimating traffic critical gap

Most unsignalised intersection capacity calculation procedures are based on gap acceptance models. Accuracy of critical gap estimation affects accuracy of capacity and delay estimation. Several methods have been published to estimate drivers’ sample mean critical gap, the Maximum Likelihood Estimation (MLE) technique regarded as the most accurate.  This study assesses three novel methods; Average Central Gap (ACG) method, Strength Weighted Central Gap method (SWCG), and Mode Central Gap method (MCG), against MLE for their fidelity in rendering true sample mean critical gaps. A Monte Carlo event based simulation model was used to draw the maximum rejected gap and accepted gap for each of a sample of 300 drivers across 32 simulation runs. Simulation mean critical gap is varied between 3s and 8s, while offered gap rate is varied between 0.05veh/s and 0.55veh/s. This study affirms that MLE provides a close to perfect fit to simulation mean critical gaps across a broad range of conditions. The MCG method also provides an almost perfect fit and has superior computational simplicity and efficiency to the MLE. The SWCG method performs robustly under high flows; however, poorly under low to moderate flows. Further research is recommended using field traffic data, under a variety of minor stream and major stream flow conditions for a variety of minor stream movement types, to compare critical gap estimates using MLE against MCG. Should the MCG method prove as robust as MLE, serious consideration should be given to its adoption to estimate critical gap parameters in guidelines
Behavior of taxi customers in hailing vacant taxis: a nested logit model for policy analysis

This study models and examines the taxi customers' preferences for hailing vacant taxis on streets. A stated preference survey was conducted to randomly select and interview 1242 taxi customers at taxi stands and pedestrians on streets, who had experiences of taking taxis recently, about their choices under different given hypothetical scenarios. In total, 4968 observations were collected and used for developing the discrete choice models for the analysis. To account for the potential correlations among alternatives, two nested logit models are developed, calibrated, and compared with a standard multinomial logit model in the investigation. The results of likelihood ratio test demonstrate that one of the developed nested logit models is better than the standard multinomial logit model to describe the search behavior of taxi customers. The model results also show that the walking time to and the waiting time at the location for hailing taxis, the extra travel time to the destination because of local circulation for finding a way from the pickup location heading to a passenger's destination, as well as the taxi customers' perceptions for walking to and waiting at taxi stands were found as significant factors to influence their decisions. In addition, the results of market segmentation analysis illustrate the variations in taxi-search strategies of taxi customers in different districts and regions. Some policy implications on introducing more taxi stands and improving the utilization rates of taxi stands are also discussed. We believe that the proposed models, findings, and discussion are useful for developing micro-simulation models to evaluate the performance of road traffic networks with taxi services and developing simulation-based optimization models to answer policy questions related to taxi services. Copyright © 2015 John Wiley & Sons, Ltd.postprin
Designing Rapid Transit Network Design with Alternative routes

The aim of this paper is to propose a model for the design of a robust rapid transit network. In this paper, a\ud
network is said to be robust when the effect of disruption on total trip coverage is minimized. The proposed\ud
model is constrained by three different kinds of flow conditions. These constraints will yield a network that\ud
provides several alternative routes for given origin–destination pairs, therefore increasing robustness. The\ud
paper includes computational experiments which show how the introduction of robustness influences\ud
network desig