30,944 research outputs found
ROSAT monitoring of persistent giant and rapid variability in the narrow-line Seyfert 1 galaxy IRAS 13224-3809
We report evidence for persistent giant and rapid X-ray variability in the
radio-quiet, ultrasoft, strong Fe II, narrow-line Seyfert 1 galaxy IRAS
13224-3809. Within a 30 day ROSAT High Resolution Imager (HRI) monitoring
observation at least five giant amplitude count rate variations are visible,
with the maximum observed amplitude of variability being about a factor of 60.
We detect a rise by a factor of about 57 in just two days. IRAS 13224-3809
appears to be the most X-ray variable Seyfert known, and its variability is
probably nonlinear. We carefully check the identification of the highly
variable X-ray source with the distant galaxy, and it appears to be secure. We
examine possible explanations for the giant variability. Unusually strong
relativistic effects and partial covering by occulting structures on an
accretion disc can provide plausible explanations of the X-ray data, and we
explore these two scenarios. Relativistic boosting effects may be relevant to
understanding the strong X-ray variability of some steep spectrum Seyferts more
generally.Comment: 14 pages, submitted to MNRA
Phase Diagram of the Hubbard Model: Beyond the Dynamical Mean Field
The Dynamical Cluster Approximation (DCA) is used to study non-local
corrections to the dynamical mean field phase diagram of the two-dimensional
Hubbard model. Regions of antiferromagnetic, d-wave superconducting,
pseudo-gapped non-Fermi liquid, and Fermi liquid behaviors are found, in rough
agreement with the generic phase diagram of the cuprates. The non-local
fluctuations beyond the mean field both suppress the antiferromagnetism and
mediate the superconductivity.Comment: 4 pages, 5 eps figures, submitted to PR
First Time-dependent Study of H2 and H3+ Ortho-Para Chemistry in the Diffuse Interstellar Medium: Observations Meet Theoretical Predictions
The chemistry in the diffuse interstellar medium initiates the gradual
increase of molecular complexity during the life cycle of matter. A key
molecule that enables build-up of new molecular bonds and new molecules via
proton-donation is H3+. Its evolution is tightly related to molecular hydrogen
and thought to be well understood. However, recent observations of ortho and
para lines of H2 and H3+ in the diffuse ISM showed a puzzling discrepancy in
nuclear spin excitation temperatures and populations between these two key
species. H3+, unlike H2, seems to be out of thermal equilibrium, contrary to
the predictions of modern astrochemical models. We conduct the first
time-dependent modeling of the para-fractions of H2 and H3+ in the diffuse ISM
and compare our results to a set of line-of-sight observations, including new
measurements presented in this study. We isolate a set of key reactions for H3+
and find that the destruction of the lowest rotational states of H3+ by
dissociative recombination largely control its ortho/para ratio. A plausible
agreement with observations cannot be achieved unless a ratio larger than 1:5
for the destruction of (1,1)- and (1,0)-states of H3+ is assumed. Additionally,
an increased CR ionization rate to 10(-15) 1/s further improves the fit whereas
variations of other individual physical parameters, such as density and
chemical age, have only a minor effect on the predicted ortho/para ratios. Thus
our study calls for new laboratory measurements of the dissociative
recombination rate and branching ratio of the key ion H3+ under interstellar
conditions.Comment: 27 pages, 6 figures, 3 table
d-wave Superconductivity in the Hubbard Model
The superconducting instabilities of the doped repulsive 2D Hubbard model are
studied in the intermediate to strong coupling regime with help of the
Dynamical Cluster Approximation (DCA). To solve the effective cluster problem
we employ an extended Non Crossing Approximation (NCA), which allows for a
transition to the broken symmetry state. At sufficiently low temperatures we
find stable d-wave solutions with off-diagonal long range order. The maximal
occurs for a doping and the doping
dependence of the transition temperatures agrees well with the generic
high- phase diagram.Comment: 5 pages, 5 figure
Andreev reflection and strongly enhanced magnetoresistance oscillations in GaInAs/InP heterostructures with superconducting contacts
We study the magnetotransport in small hybrid junctions formed by
high-mobility GaInAs/InP heterostructures coupled to superconducting (S) and
normal metal (N) terminals. Highly transmissive superconducting contacts to a
two-dimensional electron gas (2DEG) located in a GaInAs/InP heterostructure are
realized by using a Au/NbN layer system. The magnetoresistance of the S/2DEG/N
structures is studied as a function of dc bias current and temperature. At bias
currents below a critical value, the resistance of the S/2DEG/N structures
develops a strong oscillatory dependence on the magnetic field, with an
amplitude of the oscillations considerably larger than that of the reference
N/2DEG/N structures. The experimental results are qualitatively explained by
taking Andreev reflection in high magnetic fields into account.Comment: 5 pages, 5 figure
Gaps, Rings, and Non-Axisymmetric Structures in Protoplanetary Disks - From Simulations to ALMA Observations
Recent observations by the Atacama Large Millimeter/submillimeter Array
(ALMA) of disks around young stars revealed distinct asymmetries in the dust
continuum emission. In this work we want to study axisymmetric and
non-axisymmetric structures, evocated by the magneto-rotational instability in
the outer regions of protoplanetary disks. We combine the results of
state-of-the-art numerical simulations with post-processing radiative transfer
(RT) to generate synthetic maps and predictions for ALMA. We performed
non-ideal global 3D MHD stratified simulations of the dead-zone outer edge
using the FARGO MHD code PLUTO. The stellar and disk parameters are taken from
a parameterized disk model applied for fitting high-angular resolution
multi-wavelength observations of circumstellar disks. The 2D temperature and
density profiles are calculated consistently from a given surface density
profile and Monte-Carlo radiative transfer. The 2D Ohmic resistivity profile is
calculated using a dust chemistry model. The magnetic field is a vertical net
flux field. The resulting dust reemission provides the basis for the simulation
of observations with ALMA. The fiducial model develops a large gap followed by
a jump in surface density located at the dead-zone outer edge. The jump in
density and pressure is strong enough to stop the radial drift of particles. In
addition, we observe the generation of vortices by the Rossby wave instability
(RWI) at the jumps location close to 60 AU. The vortices are steadily generated
and destroyed at a cycle of 40 local orbits. The RT results and simulated ALMA
observations predict the feasibility to observe such large scale structures
appearing in magnetized disks without having a planet.Comment: Language update, added comments, added citations, in press. (A&A
Cd-vacancy and Cd-interstitial complexes in Si and Ge
The electrical field gradient (EFG), measured e.g. in perturbed angular
correlation (PAC) experiments, gives particularly useful information about the
interaction of probe atoms like 111In / 111Cd with other defects. The
interpretation of the EFG is, however, a difficult task. This paper aims at
understanding the interaction of Cd impurities with vacancies and interstitials
in Si and Ge, which represents a controversial issue. We apply two
complementary ab initio methods in the framework of density functional theory
(DFT), (i) the all electron Korringa-Kohn-Rostoker (KKR) Greenfunction method
and (ii) the Pseudopotential-Plane-Wave (PPW) method, to search for the correct
local geometry. Surprisingly we find that both in Si and Ge the substitutional
Cd-vacancy complex is unstable and relaxes to a split-vacancy complex with the
Cd on the bond-center site. This complex has a very small EFG, allowing a
unique assignment of the small measured EFGs of 54MHz in Ge and 28MHz in Si.
Also, for the Cd-selfinterstitial complex we obtain a highly symmetrical split
configuration with large EFGs, being in reasonable agreement with experiments
Neutron-star radii based on realistic nuclear interactions
The existence of neutron stars with requires the strong stiffness
of the equation of state (EoS) of neutron-star matter. We introduce a
multi-pomeron exchange potential (MPP) working universally among 3- and
4-baryons to stiffen the EoS. Its strength is restricted by analyzing the
nucleus-nucleus scattering with the G-matrix folding model. The EoSs are
derived using the Brueckner-Hartree-Fock (BHF) and the cluster variational
method (CVM) with the nuclear interactions ESC and AV18. The mass-radius
relations are derived by solving the Tolmann-Oppenheimer-Volkoff (TOV)
equation, where the maximum masses over are obtained on the basis of
the terrestrial data. Neutron-star radii at a typical mass are
predicted to be km. The uncertainty of calculated radii is
mainly from the ratio of 3- and 4-pomeron coupling constants, which cannot be
fixed by any terrestrial experiment. Though values of are not
influenced by hyperon-mixing effects, finely-observed values for them indicate
degrees of EoS softening by hyperon mixing in the region of
. If is less than about 12.4 km, the
softening of EoS by hyperon mixing has to be weak. Useful information can be
expected by the space mission NICER offering precise measurements for
neutron-star radii within .Comment: 8 pages, 7 figure
Supernovae, Pulsars and Gamma-Ray Bursts: A Unified Picture
A scenario is proposed that explains both the observed high pulsar velocities
and extragalactic gamma-ray bursts (GRBs). The model involves an ultra-
relativistic jet from a supernova (SN), that produces a GRB and its afterglow,
whose characteristics are similar to an isotropic fireball GRB perhaps with
some differences at late times in the afterglow once some significant
transverse diffusion has occurred. The time scales and many other properties of
GRBs and their afterglows in this model are consistent with observations.
GRBs in this model have special intrinsic properties, that can either falsify
or prove this model unambiguously by observations. The most direct proof is the
detection of a SN about the same time as the luminous GRB event. Most GRBs and
SNe are expected occur at moderate redshift (), if they follow the
observed universal star formation history, as implied in this model. Searching
for GRB/SN associations is a challenge, because majority of the SNe will be
faint. Some additional, dramatic observable consequences are predicted, which
can also be utilized to test the model.Comment: ApJ Letters in press, 4 emulateapj page
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