5,336 research outputs found
The Generation of Fullerenes
We describe an efficient new algorithm for the generation of fullerenes. Our
implementation of this algorithm is more than 3.5 times faster than the
previously fastest generator for fullerenes -- fullgen -- and the first program
since fullgen to be useful for more than 100 vertices. We also note a
programming error in fullgen that caused problems for 136 or more vertices. We
tabulate the numbers of fullerenes and IPR fullerenes up to 400 vertices. We
also check up to 316 vertices a conjecture of Barnette that cubic planar graphs
with maximum face size 6 are hamiltonian and verify that the smallest
counterexample to the spiral conjecture has 380 vertices.Comment: 21 pages; added a not
Prospects for CW and LP operation of the European XFEL in hard X-ray regime
The European XFEL will operate nominally at 17.5 GeV in SP (short pulse) mode
with 0.65 ms long bunch train and 10 Hz repetition rate. A possible upgrade of
the linac to CW (continuous wave) or LP (long pulse) modes with a corresponding
reduction of electron beam energy is under discussion since many years. Recent
successes in the dedicated R&D program allow to forecast a technical
feasibility of such an upgrade in the foreseeable future. One of the challenges
is to provide sub-Angstrom FEL operation in CW and LP modes. In this paper we
perform a preliminary analysis of a possible operation of the European XFEL in
the hard X-ray regime in CW and LP modes with the energies of 7 GeV and 10 GeV,
respectively. We consider lasing in the baseline XFEL undulator as well as in a
new undulator with a reduced period. We show that, with reasonable requirements
on electron beam quality, lasing on the fundamental will be possible in
sub-Angstrom regime. As an option for generation of brilliant photon beams at
short wavelengths we also consider harmonic lasing that has recently attracted
a significant attention
A digitalized solar ultraviolet spectrum
Digitalized solar ultraviolet spectrum obtained in rocket experiments for use in analysis of upper atmosphere experiment
Interaction-assisted propagation of Coulomb-correlated electron-hole pairs in disordered semiconductors
A two-band model of a disordered semiconductor is used to analyze dynamical
interaction induced weakening of localization in a system that is accessible to
experimental verification. The results show a dependence on the sign of the
two-particle interaction and on the optical excitation energy of the
Coulomb-correlated electron-hole pair.Comment: 4 pages and 3 ps figure
Synthetic X-ray light curves of BL Lacs from relativistic hydrodynamic simulations
We present the results of relativistic hydrodynamic simulations of the
collision of two dense shells in a uniform external medium, as envisaged in the
internal shock model for BL Lac jets. The non-thermal radiation produced by
highly energetic electrons injected at the relativistic shocks is computed
following their temporal and spatial evolution. The acceleration of electrons
at the relativistic shocks is parametrized using two different models and the
corresponding X-ray light curves are computed. We find that the interaction
time scale of the two shells is influenced by an interaction with the external
medium. For the chosen parameter sets, the efficiency of the collision in
converting dissipated kinetic energy into the observed X-ray radiation is of
the order of one percent.Comment: 22 pages, 6 figures, accepted to A&
Transient Emission From Dissipative Fronts in Magnetized, Relativistic Outflows. II. Synchrotron Flares
The time dependent synchrotron emission from relativistic jets, and the
relation between the synchrotron and ERC emission is considered within the
framework of the radiative front model. The timescale and profile of the
optically thin emission are shown to be determined, in this model, by the shock
formation radius, the thickness of expelled fluid slab and the variation of the
front's parameters due to its transverse expansion. For a range of reasonable
conditions, a variety of flare shapes can be produced, varying from roughly
symmetric with exponential rises and decays, as often seen in blazars, to
highly asymmetric with a fast rise and a much slower, power law decay, as seen
in GRB afterglows. The onset, duration, and fluence of low-frequency (below the
initial turnover frequency) and hard gamma-ray (above the initial gamma-spheric
energy) outbursts are limited by opacity effects; the emission at these
energies is quite generally delayed and, in the case of sufficiently short
length outbursts, severely attenuated. The observational consequences are
discussed. One distinctive prediction of this model is that in a single,
powerful source, the upper cutoff of the gamma-ray spectrum should be
correlated with the timescale of the outburst and with the amplitude of
variations at long wavelengths (typically radio to millimeter).Comment: AAS LaTex, 14 pgs, accepted to A
Thermal X-ray emission from shocked ejecta in Type Ia Supernova Remnants. Prospects for explosion mechanism identification
The explosion mechanism behind Type Ia supernovae is a matter of continuing
debate. The diverse attempts to identify or at least constrain the physical
processes involved in the explosion have been only partially successful so far.
In this paper we propose to use the thermal X-ray emission from young supernova
remnants originated in Type Ia events to extract relevant information
concerning the explosions themselves. We have produced a grid of thermonuclear
supernova models representative of the paradigms currently under debate: pure
deflagrations, delayed detonations, pulsating delayed detonations and
sub-Chandrasekhar explosions, using their density and chemical composition
profiles to simulate the interaction with the surrounding ambient medium and
the ensuing plasma heating, non-equilibrium ionization and thermal X-ray
emission of the ejecta. Key observational parameters such as electron
temperatures, emission measures and ionization time scales are presented and
discussed. We find that not only is it possible to identify the explosion
mechanism from the spectra of young Type Ia Supernova Remnants, it is in fact
necessary to take the detailed ejecta structure into account if such spectra
are to be modeled in a self-consistent way. Neither element line flux ratios
nor element emission measures are good estimates of the true ratios of ejected
masses, with differences of as much as two or three orders of magnitude for a
given model. Comparison with observations of the Tycho SNR suggests a delayed
detonation as the most probable explosion mechanism. Line strengths, line
ratios, and the centroid of the Fe Kalpha line are reasonably well reproduced
by a model of this kind.Comment: 11 pages, 8 figures (5 of them color), accepted for publication by
the Ap
Spectral variability analysis of an XMM-Newton observation of Ark 564
We present a spectral variability analysis of the X-ray emission of the Narrow Line Seyfert 1 galaxy Ark 564 using the data from a ~100 ks XMM-Newton observation. Taking advantage of the high sensitivity of this long observation and the simple spectral shape of Ark 564, we determine accurately the spectral variability patterns in the source. We use standard cross-correlation methods to investigate the correlations between the soft and hard energy band light curves. We also generated 200 energy spectra from data stretches of 500 s duration each and fitted each one of them with a power law plus a bremsstrahlung component (for the soft excess) and we investigated the correlations between the various best fit model parameter values. The ``power law plus bremsstrahlung'' model describes the spectrum well at all times. The iron line and the absorption features, which are found in the time-averaged spectrum of the source are too weak to effect the results of the time resolved spectral fits. We find that the power law and the soft excess flux are variable, on all measured time scales. The power law slope is also variable, and leads the flux variations of both the power law and the bremsstrahlung components. Our results can be explained in the framework of time-dependent Comptonization models. They are consistent with a picture where instabilities propagate through an extended X-ray source, affecting first the soft and then the hard photons producing regions. The soft excess could correspond to ionized disc reflection emission, in which case it responds fast to the primary continuum variations. The time scales are such that light travel times might additionally influence the observed variability structure
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