15,093 research outputs found
Scientometric and Bibliometric Analysis in Analytical Marketing Research
Theoretical background: Analytical marketing is at the heart of scientific research because it plays an important role in building the competitiveness of enterprises and is an opportunity for them to grow.Purpose of the article: The aim of the article is to present the results of a bibliometric analysis of the developing area of analytical marketing.Research methods: For this purpose, specialist journals published between 1900 and 2021 were searched in the Web of Science database. The scientometric analyses carried out on their basis concern the number of publications, authorship and co-authorship, the number of citations, journals, thematic categories, institutions, countries and keywords. Over 200 publications cited 2,563 times were analyzed.Main findings: The concept of analytical marketing was taken into account by over 400 authors, with Maria Petrescu authoring the highest number of publications, and Michel Wedel being the most significant author due to the number of citations. An important role, due to the number of publications in this area, is played by institutions based in the USA (over 50%), including the University of Nevada, Las Vegas (UNLV) and the Nevada System of Higher Education (NSHE). What is more, the conducted research emphasizes the importance of marketing analytics and presents benefits that stem from using it
Three-Dimensional Simulations of Mixing Instabilities in Supernova Explosions
We present the first three-dimensional (3D) simulations of the large-scale
mixing that takes place in the shock-heated stellar layers ejected in the
explosion of a 15.5 solar-mass blue supergiant star. The outgoing supernova
shock is followed from its launch by neutrino heating until it breaks out from
the stellar surface more than two hours after the core collapse. Violent
convective overturn in the post-shock layer causes the explosion to start with
significant asphericity, which triggers the growth of Rayleigh-Taylor (RT)
instabilities at the composition interfaces of the exploding star. Deep inward
mixing of hydrogen (H) is found as well as fast-moving, metal-rich clumps
penetrating with high velocities far into the H-envelope of the star as
observed, e.g., in the case of SN 1987A. Also individual clumps containing a
sizeable fraction of the ejected iron-group elements (up to several 0.001 solar
masses) are obtained in some models. The metal core of the progenitor is
partially turned over with Ni-dominated fingers overtaking oxygen-rich bullets
and both Ni and O moving well ahead of the material from the carbon layer.
Comparing with corresponding 2D (axially symmetric) calculations, we determine
the growth of the RT fingers to be faster, the deceleration of the dense
metal-carrying clumps in the He and H layers to be reduced, the asymptotic
clump velocities in the H-shell to be higher (up to ~4500 km/s for the
considered progenitor and an explosion energy of 10^{51} ergs, instead of <2000
km/s in 2D), and the outward radial mixing of heavy elements and inward mixing
of hydrogen to be more efficient in 3D than in 2D. We present a simple argument
that explains these results as a consequence of the different action of drag
forces on moving objects in the two geometries. (abridged)Comment: 15 pages, 8 figures, 30 eps files; significantly extended and more
figures added after referee comments; accepted by The Astrophysical Journa
Gravitational waves from three-dimensional core-collapse supernova models: The impact of moderate progenitor rotation
We present predictions for the gravitational-wave (GW) emission of
three-dimensional supernova (SN) simulations performed for a 15 solar-mass
progenitor with the Prometheus-Vertex code using energy-dependent, three-flavor
neutrino transport. The progenitor adopted from stellar evolution calculations
including magnetic fields had a fairly low specific angular momentum (j_Fe <~
10^{15} cm^2/s) in the iron core (central angular velocity ~0.2 rad/s), which
we compared to simulations without rotation and with artificially enhanced
rotation (j_Fe <~ 2*10^{16} cm^2/s; central angular velocity ~0.5 rad/s). Our
results confirm that the time-domain GW signals of SNe are stochastic, but
possess deterministic components with characteristic patterns at low
frequencies (<~200 Hz), caused by mass motions due to the standing accretion
shock instability (SASI), and at high frequencies, associated with gravity-mode
oscillations in the surface layer of the proto-neutron star (PNS). Non-radial
mass motions in the post-shock layer as well as PNS convection are important
triggers of GW emission, whose amplitude scales with the power of the
hydrodynamic flows. There is no monotonic increase of the GW amplitude with
rotation, but a clear correlation with the strength of SASI activity. Our
slowly rotating model is a fainter GW emitter than the non-rotating model
because of weaker SASI activity and damped convection in the post-shock layer
and PNS. In contrast, the faster rotating model exhibits a powerful SASI spiral
mode during its transition to explosion, producing the highest GW amplitudes
with a distinctive drift of the low-frequency emission peak from ~80-100 Hz to
~40-50 Hz. This migration signifies shock expansion, whereas non-exploding
models are discriminated by the opposite trend.Comment: Added new figure, figure 9. Updated figure 9, now figure 10. Modified
the discussion of the proto-neutron star convection. Added a figure showing
the average rotation rate as a function of radius. Added a section discussing
where the low-frequency gravitational waves are generated, this information
is visualized in figure 9. We also made some minor changes to the text and
selected plot
Neutrino Signal of Electron-Capture Supernovae from Core Collapse to Cooling
An 8.8 solar mass electron-capture supernova (SN) was simulated in spherical
symmetry consistently from collapse through explosion to nearly complete
deleptonization of the forming neutron star. The evolution time of about 9 s is
short because of nucleon-nucleon correlations in the neutrino opacities. After
a brief phase of accretion-enhanced luminosities (~200 ms), luminosity
equipartition among all species becomes almost perfect and the spectra of
electron antineutrinos and muon/tau antineutrinos very similar. We discuss
consequences for the neutrino-driven wind as a nucleosynthesis site and for
flavor oscillations of SN neutrinos.Comment: 4 pages, 4 eps figures; published as Physical Review Letters, vol.
104, Issue 25, id. 25110
Global Anisotropy Versus Small-Scale Fluctuations in Neutrino Flux in Core-Collapse Supernova Explosions
Effects of small-scale fluctuations in the neutrino radiation on
core-collapse supernova explosions are examined. Through a parameter study with
a fixed radiation field of neutrinos, we find substantial differences between
the results of globally anisotropic neutrino radiation and those with
fluctuations. As the number of modes of fluctuations increases, the shock
positions, entropy distributions, and explosion energies approach those of
spherical explosion. We conclude that global anisotropy of the neutrino
radiation is the most effective mechanism of increasing the explosion energy
when the total neutrino luminosity is given. This supports the previous
statement on the explosion mechanism by Shimizu and coworkers.Comment: 14 pages, including 12 figures. To be published in the Astrophysical
Journa
Delayed neutrino-driven supernova explosions aided by the standing accretion-shock instability
We present results of 2D hydrodynamic simulations of stellar core collapse,
which confirm that the neutrino-heating mechanism remains viable for the
explosion of a wider mass range of supernova progenitors with iron cores. We
used an energy-dependent treatment of the neutrino transport based on the
"ray-by-ray plus" approximation, in which the number, energy, and momentum
equations are closed with a variable Eddington factor obtained by iteratively
solving a model Boltzmann equation. We focus on the evolution of a 15 Msun
progenitor and show that shock revival and the explosion are initiated at about
600 ms post bounce, powered by neutrino energy deposition. Similar to previous
findings for an 11.2 Msun star, but significantly later, the onset of the
explosion is fostered by the standing accretion shock instability (SASI). This
instability exhibits highest growth rates for the dipole and quadrupole modes,
which lead to large-amplitude bipolar shock oscillations and push the shock to
larger radii, thus increasing the time accreted matter is exposed to neutrino
heating in the gain layer. Therefore also convective overturn behind the shock
is strengthened. A "soft" nuclear equation of state that causes a rapid
contraction and a smaller radius of the forming neutron star and thus a fast
release of gravitational binding energy, seems to be more favorable for an
explosion. Rotation has the opposite effect because it leads to a more extended
and cooler neutron star and thus lower neutrino luminosities and mean energies
and overall less neutrino heating. Neutron star g-mode oscillations and the
acoustic mechanism play no important role in our simulations. (abridged)Comment: 46 pages, 20 figures, 59 eps files; submitted to ApJ; significantly
extended and revised version to account for referee comments; high-resolution
images can be obtained upon reques
Palladium and silver abundances in stars with [Fe/H] > -2.6
Palladium (Pd) and silver (Ag) are the key elements for probing the weak
component in the rapid neutron-capture process (r-process) of stellar
nucleosynthesis. We performed a detailed analysis of the high-resolution and
high signal-to-noise ratio near-UV spectra from the archive of HIRES on the
Keck telescope, UVES on the VLT, and HDS on the Subaru Telescope, to determine
the Pd and Ag abundances of 95 stars. This sample covers a wide metallicity
range with -2.6 [Fe/H] +0.1, and most of them are dwarfs.
The plane-parallel LTE MAFAGS-OS model atmosphere was adopted, and the spectral
synthesis method was used to derive the Pd and Ag abundances from Pd I
{\lambda} 3404 {\AA} and Ag I {\lambda} 3280/3382 {\AA} lines. We found that
both elements are enhanced in metal-poor stars, and their ratios to iron show
flat trends at -0.6 < [Fe/H] < +0.1. The abundance ratios of [Ag/H] and [Pd/H]
are well correlated over the whole abundance range. This implies that Pd and Ag
have similar formation mechanisms during the Galactic evolution.Comment: 15 pages, 12 figures, accepted to A&
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