7,902 research outputs found
DISCUSSION: NEEDED RESEARCH WITH RESPECT TO ENERGY USE IN AGRICULTURAL PRODUCTION
Resource /Energy Economics and Policy,
AN ECONOMIC SIMULATION MODEL FOR ANALYZING NATURAL RESOURCE POLICY
Resource /Energy Economics and Policy,
Can the QCD Effective Charge Be Symmetrical in the Euclidean and the Minkowskian Regions?
We study a possible symmetrical behavior of the effective charges defined in
the Euclidean and Minkowskian regions and prove that such symmetry is
inconsistent with the causality principle.Comment: 5 pages, REVTe
GRMHD simulations of prompt-collapse neutron star mergers: the absence of jets
Inspiraling and merging binary neutron stars are not only important source of
gravitational waves, but also promising candidates for coincident
electromagnetic counterparts. These systems are thought to be progenitors of
short gamma-ray bursts (sGRBs). We have shown previously that binary neutron
star mergers that undergo {\it delayed} collapse to a black hole surrounded by
a {\it weighty} magnetized accretion disk can drive magnetically-powered jets.
We now perform magnetohydrodynamic simulations in full general relativity of
binary neutron stars mergers that undergo {\it prompt} collapse to explore the
possibility of jet formation from black hole-{\it light} accretion disk
remnants. We find that after ms
[ is the ADM mass] following prompt black hole formation, there is
no evidence of mass outflow or magnetic field collimation. The rapid formation
of the black hole following merger prevents magnetic energy from approaching
force-free values above the magnetic poles, which is required for the launching
of a jet by the usual Blandford--Znajek mechanism. Detection of gravitational
waves in coincidence with sGRBs may provide constraints on the nuclear equation
of state (EOS): the fate of an NSNS merger--delayed or prompt collapse, and
hence the appearance or nonappearance of an sGRB--depends on a critical value
of the total mass of the binary, and this value is sensitive to the EOS.Comment: 11 pages, 6 figures, matches published versio
Casimir Energies and Pressures for -function Potentials
The Casimir energies and pressures for a massless scalar field associated
with -function potentials in 1+1 and 3+1 dimensions are calculated. For
parallel plane surfaces, the results are finite, coincide with the pressures
associated with Dirichlet planes in the limit of strong coupling, and for weak
coupling do not possess a power-series expansion in 1+1 dimension. The relation
between Casimir energies and Casimir pressures is clarified,and the former are
shown to involve surface terms. The Casimir energy for a -function
spherical shell in 3+1 dimensions has an expression that reduces to the
familiar result for a Dirichlet shell in the strong-coupling limit. However,
the Casimir energy for finite coupling possesses a logarithmic divergence first
appearing in third order in the weak-coupling expansion, which seems
unremovable. The corresponding energies and pressures for a derivative of a
-function potential for the same spherical geometry generalizes the TM
contributions of electrodynamics. Cancellation of divergences can occur between
the TE (-function) and TM (derivative of -function) Casimir
energies. These results clarify recent discussions in the literature.Comment: 16 pages, 1 eps figure, uses REVTeX
Jet launching from binary black hole-neutron star mergers: Dependence on black hole spin, binary mass ratio and magnetic field orientation
Black hole-neutron star (BHNS) mergers are one of the most promising targets
for multimessenger astronomy. Using general relativistic magnetohydrodynamic
simulations of BHNS undergoing merger we showed that a magnetically--driven jet
can be launched by the remnant if the NS is endowed with a dipole B field
extending from the interior into the exterior as in a radio pulsar. These
self-consistent studies considered a BHNS system with mass ratio , BH
spin aligned with the total orbital angular momentum (OAM), and
a NS that is irrotational, threaded by an aligned B field, and modeled by an
--law equation of state with . Here, as a crucial step in
establishing BHNS systems as viable progenitors of central engines that power
short gamma--ray bursts (sGRBs) and thereby solidify their role as
multimessenger sources, we survey different BHNS configurations that differ in
BH spin (), in the mass ratio ( and
), and in the orientation of the B field (aligned and tilted by
with respect to the OAM). We find that by after the peak
gravitational wave signal a jet is launched in the cases where the initial BH
spin is or . The lifetime of the jets[] and their Poynting
luminosities [] are consistent with sGRBs,
as well as with the Blandford--Znajek mechanism. By the time we terminate our
simulations, we do not observe either an outflow or a large-scale B field
collimation in the other configurations we simulate. These results suggest that
future multimessenger detections from BHNSs are more likely produced by
binaries with highly spinning BH companions and small tilt-angle B fields.Comment: 17 pages, 14 figures. Added references, matches published versio
Magnetic Braking and Damping of Differential Rotation in Massive Stars
Fragmentation of highly differentially rotating massive stars that undergo
collapse has been suggested as a possible channel for binary black hole
formation. Such a scenario could explain the formation of the new population of
massive black holes detected by the LIGO/VIRGO gravitational wave laser
interferometers. We probe that scenario by performing general relativistic
magnetohydrodynamic simulations of differentially rotating massive stars
supported by thermal radiation pressure plus a gas pressure perturbation. The
stars are initially threaded by a dynamically weak, poloidal magnetic field
confined to the stellar interior. We find that magnetic braking and turbulent
viscous damping via magnetic winding and the magnetorotational instability in
the bulk of the star redistribute angular momentum, damp differential rotation
and induce the formation of a massive and nearly uniformly rotating inner core
surrounded by a Keplerian envelope. The core + disk configuration evolves on a
secular timescale and remains in quasi-stationary equilibrium until the
termination of our simulations. Our results suggest that the high degree of
differential rotation required for seed density perturbations to trigger
gas fragmentation and binary black hole formation is likely to be suppressed
during the normal lifetime of the star prior to evolving to the point of
dynamical instability to collapse. Other cataclysmic events, such as stellar
mergers leading to collapse, may therefore be necessary to reestablish
sufficient differential rotation and density perturbations to drive
nonaxisymmetric modes leading to binary black hole formation.Comment: 11 pages, 5 figures. Minor changes, matches published versio
Relativistic Coulomb Resummation in QCD
A relativistic Coulomb-like resummation factor in QCD is suggested, based on
the solution of the quasipotential equation.Comment: 4 pages, 2 eps figures, REVTe
Simulating the Magnetorotational Collapse of Supermassive Stars: Incorporating Gas Pressure Perturbations and Different Rotation Profiles
Collapsing supermassive stars (SMSs) with masses
have long been speculated to be the seeds that can grow and become supermassive
black holes (SMBHs). We previously performed GRMHD simulations of marginally
stable magnetized polytropes uniformly rotating at the
mass-shedding limit to model the direct collapse of SMSs. These configurations
are supported entirely by thermal radiation pressure and model SMSs with . We found that around of the initial stellar mass
forms a spinning black hole (BH) surrounded by a massive, hot, magnetized
torus, which eventually launches an incipient jet. Here we perform GRMHD
simulations of , polytropes to account for the perturbative
role of gas pressure in SMSs with . We also consider
different initial stellar rotation profiles. The stars are initially seeded
with a dynamically weak dipole magnetic field that is either confined to the
stellar interior or extended from its interior into the stellar exterior. We
find that the mass of the BH remnant is of the initial stellar
mass, depending sharply on as well as on the initial stellar
rotation profile. After s
following the BH formation, a jet is launched and it lasts for s, consistent with the duration of long gamma-ray
bursts. Our results suggest that the Blandford-Znajek mechanism powers the jet.
They are also in agreement with our proposed universal model that estimates
accretion rates and luminosities that characterize magnetized BH-disk remnant
systems that launch a jet. This model helps explain why the outgoing
luminosities for vastly different BH-disk formation scenarios all reside within
a narrow range (), roughly independent of .Comment: 16 pages, 7 figures. Added references, matches published versio
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