640 research outputs found
Optimal control of hybrid systems and renewable energies
International policies for sustainable development have led to an increase in distributed power production based on renewable resources [...
A broad iron line in the Chandra/HETG spectrum of 4U 1705-44
We present the results of a Chandra 30 ks observation of the low mass X-ray
binary and atoll source 4U 1705-44. Here we concentrate on the study of
discrete features in the energy spectrum at energies below 3 keV, as well as on
the iron Kalpha line, using the HETG spectrometer on board of the Chandra
satellite. Below 3 keV, three narrow emission lines are found at 1.47, 2.0, and
2.6 keV. The 1.47 and 2.6 keV are probably identified with Ly-alpha emission
from Mg XII and S XVI, respectively. The identification of the feature at 2.0
keV is uncertain due to the presence of an instrumental feature at the same
energy. The iron Kalpha line at ~6.5 keV is found to be intrinsically broad
(FWHM ~ 1.2 keV); its width can be explained by reflection from a cold
accretion disk extending down to 15 km from the neutron star center or by
Compton broadening in the external parts of a hot (~2 keV) Comptonizing corona.
We finally report here precise X-ray coordinates of the source.Comment: 8 pages including 2 figures. ApJ Letters, in pres
Optimal charging of electric vehicles in microgrids through discrete event optimization
In this paper, a discrete event approach is proposed for the optimal charging of electrical vehicles in microgrids. In particular, the considered system is characterized by renewable energy sources (RES), non-renewable energy sources, electrical storage, a connection to the external grid and a charging station for electric vehicles (EVs). The decision variables are relevant to the schedule of production plants, storage systems and EVs' charging. The objective function to be minimized is related to the cost of purchasing energy from the external grid, the use of nonrenewable energy sources and tardiness of customer's service. The proposed approach is applied to a real case study and it is shown that it allows to considerably reduce the dimension of the problem (and thus the computational time required) as compared to a discrete-time approach
Coupling Between Periodic and Aperiodic Variability in SAX J1808.4-3658
We detect a significant broadening in the wings of the 401 Hz peak in the
power spectrum of the accreting millisecond binary pulsar SAX J1808.4-3658.
This feature is consistent with the convolution of the red noise present in the
power spectrum with the harmonic line. We conclude that the flux modulated by
the spin period shows aperiodic variability similar to the red noise in the
overall flux, suggesting such variability also originates at the magnetic caps
close to the neutron star surface. This is analogous to the results found in
some longer period, higher magnetic field pulsators in high mass X-ray
binaries.Comment: 16 pages, 3 figures, to be published in The Astrophysical Journa
Testing Rate Dependent corrections on timing mode EPIC-pn spectra of the accreting Neutron Star GX 13+1
When the EPIC-pn instrument on board XMM-Newton is operated in Timing mode,
high count rates (>100 cts/s) of bright sources may affect the calibration of
the energy scale, resulting in a modification of the real spectral shape. The
corrections related to this effect are then strongly important in the study of
the spectral properties. Tests of these calibrations are more suitable in
sources which spectra are characterised by a large number of discrete features.
Therefore, in this work, we carried out a spectral analysis of the accreting
Neutron Star GX 13+1, which is a dipping source with several narrow absorption
lines and a broad emission line in its spectrum. We tested two different
correction approaches on an XMM-Newton EPIC-pn observation taken in Timing
mode: the standard Rate Dependent CTI (RDCTI or epfast) and the new, Rate
Dependent Pulse Height Amplitude (RDPHA) corrections. We found that, in
general, the two corrections marginally affect the properties of the overall
broadband continuum, while hints of differences in the broad emission line
spectral shape are seen. On the other hand, they are dramatically important for
the centroid energy of the absorption lines. In particular, the RDPHA
corrections provide a better estimate of the spectral properties of these
features than the RDCTI corrections. Indeed the discrete features observed in
the data, applying the former method, are physically more consistent with those
already found in other Chandra and XMM-Newton observations of GX 13+1.Comment: Accepted for publication in MNRAS; 10 pages, 8 figure
An XMM-Newton study of the 401 Hz accreting pulsar SAX J1808.4-3658 in quiescence
SAX J1808.4-3658 is a unique source being the first Low Mass X-ray Binary
showing coherent pulsations at a spin period comparable to that of millisecond
radio pulsars. Here we present an XMM-Newton observation of SAX J1808.4-3658 in
quiescence, the first which assessed its quiescent luminosity and spectrum with
good signal to noise. XMM-Newton did not reveal other sources in the vicinity
of SAX J1808.4-3658 likely indicating that the source was also detected by
previous BeppoSAX and ASCA observations, even if with large positional and flux
uncertainties. We derive a 0.5-10 keV unabsorbed luminosity of L_X=5x10^{31}
erg/s, a relatively low value compared with other neutron star soft X-ray
transient sources. At variance with other soft X-ray transients, the quiescent
spectrum of SAX J1808.4-3658 was dominated by a hard (Gamma~1.5) power law with
only a minor contribution (<10%) from a soft black body component. If the power
law originates in the shock between the wind of a turned-on radio pulsar and
matter outflowing from the companion, then a spin-down to X-ray luminosity
conversion efficiency of eta~10^{-3} is derived; this is in line with the value
estimated from the eclipsing radio pulsar PSR J1740-5340. Within the deep
crustal heating model, the faintness of the blackbody-like component indicates
that SAX J1808.4-3658 likely hosts a massive neutronstar (M>1.7 solar masses).Comment: Paper accepted for publication in ApJ
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