2,119 research outputs found
Scattering by Conducting Cylinders Below a Dielectric Layer With a Fast Noniterative Approach
A spectral-domain technique to solve the scattering
by perfectly conducting cylinders placed below a dielectric layer is
presented. Propagation fields are expressed in an analytic form, in
the frame of the cylindrical wave approach. The fields scattered by
the buried objects are decomposed into cylindrical waves, which
are, in turn, represented by plane-wave spectra. Due to the interaction
with a layered layout, the scattered fields experience multiple
infinite reflections at the boundaries of the layer. Using suitable
reflection and transmission coefficients inside the plane-wave
spectra, the interaction with such a layered geometry can be solved
with a single-reflection approach. Multiple reflections are collected
by a set of two scattered fields, i.e., an upward-propagating field,
excited by the scatterers and transmitted up to the top medium,
and a down-propagating one, which from the top medium reaches
the scatterers after transmission through the layer. Therefore, the
analytical theory is developed in a very compact way and can be
solved through a fast and efficient numerical implementation. Numerical
results are evaluated in an accurate way and validated by
comparisons with results obtained with a multiple-reflection approach.
The scattered field can be evaluated in any point of the domain,
in the far-field as well as the near-field region. Two-dimensional
maps displaying the magnitude of the total scattered field
are reported, showing examples of applications of the technique
The truncated and evolving inner accretion disc of the black hole GX 339-4
The nature of accretion onto stellar mass black holes in the low/hard state
remains unresolved, with some evidence suggesting that the inner accretion disc
is truncated and replaced by a hot flow. However, the detection of relativistic
broadened Fe emission lines, even at relatively low luminosities, seems to
require an accretion disc extending fully to its innermost stable circular
orbit. Modelling such features is however highly susceptible to degeneracies,
which could easily bias any interpretation. We present the first systematic
study of the Fe line region to track how the inner accretion disc evolves in
the low/hard state of the black hole GX 3394. Our four observations display
increased broadening of the Fe line over two magnitudes in luminosity, which we
use to track any variation of the disc inner radius. We find that the disc
extends closer to the black hole at higher luminosities, but is consistent with
being truncated throughout the entire low/hard state, a result which renders
black hole spin estimates inaccurate at these stages of the outburst.
Furthermore, we show that the evolution of our spectral inner disc radius
estimates corresponds very closely to the trend of the break frequency in
Fourier power spectra, supporting the interpretation of a truncated and
evolving disc in the hard state.Comment: Accepted for publication in A&A. Some typos corrected from version
Revealing accretion onto black holes: X-ray reflection throughout three outbursts of GX 339-4
Understanding the dynamics behind black hole state transitions and the
changes they reflect in outbursts has become long-standing problem. The X-ray
reflection spectrum describes the interaction between the hard X-ray source
(the power-law continuum) and the cool accretion disc it illuminates, and thus
permits an indirect view of how the two evolve. We present a systematic
analysis of the reflection spectrum throughout three outbursts (500+
observations) of the black hole binary GX 339-4, representing the largest study
applying a self-consistent treatment of reflection to date. Particular
attention is payed to the coincident evolution of the power-law and reflection,
which can be used to determine the accretion geometry. The hard state is found
to be distinctly reflection weak, however the ratio of reflection to power-law
gradually increases as the source luminosity rises. In contrast the reflection
is found dominate the power-law throughout most of the soft state, with
increasing supremacy as the source decays. We discuss potential dynamics
driving this, favouring inner disc truncation and decreasing coronal height for
the hard and soft states respectively. Evolution of the ionisation parameter,
power-law slope and high-energy cut-off also agree with this interpretation.Comment: Accepted for publication in MNRA
Probing 3D Density and Velocity Fields of ISM in Centers of Galaxies with Future X-Ray Observations
Observations of bright and variable "reflected" X-ray emission from molecular
clouds located within inner hundred parsec of our Galaxy have demonstrated that
the central supermassive black hole, Sgr A*, experienced short and powerful
flares in the past few hundred years. These flares offer a truly unique
opportunity to determine 3D location of the illuminated clouds (with ~10 pc
accuracy) and to reveal their internal structure (down to 0.1 pc scales). Short
duration of the flare(s), combined with X-rays high penetration power and
insensitivity of the reflection signal to thermo- and chemo-dynamical state of
the gas, ensures that the provided diagnostics of the density and velocity
fields is unbiased and almost free of the projection and opacity effects. Sharp
and sensitive snapshots of molecular gas accessible with aid of future X-ray
observatories featuring large collecting area and high angular (arcsec-level)
and spectral (eV-level) resolution cryogenic bolometers will present invaluable
information on properties of the supersonic turbulence inside the illuminated
clouds, map their shear velocity field and allow cross-matching between X-ray
data and velocity-resolved emission of various molecular species provided by
ALMA and other ground-based facilities. This will highlight large and
small-scale dynamics of the dense gas and help uncovering specifics of the ISM
lifecycle and high-mass star formation under very extreme conditions of
galactic centers. While the former is of particular importance for the SMBH
feeding and triggering AGN feedback, the latter might be an excellent test case
for star formation taking place in high-redshift galaxies.Comment: White paper submitted to the Astro2020 Decadal Surve
3C 33: another case of photoionized soft X-ray emission in radio galaxies
All the observations available in the Chandra and XMM-Newton archives have
been used to investigate the X-ray spectral properties of 3C 33. In this paper
is presented a complete X-ray analysis of the nuclear emission of this narrow
line radio galaxy. The broad band spectrum of 3C 33 is complex. The hard part
resembles that of Seyfert 2 galaxies, with a heavily obscured nuclear continuum
(N_H~10^23 cm^-2) and a prominent Fe Kalpha line. This represents the nuclear
radiation directly observed in transmission through a cold circumnuclear gas.
On the other hand an unabsorbed continuum plus emission lines seem to fit well
the soft part of the spectrum (0.5-2 keV) suggesting that the jet does not
significantly contribute to the X-ray emission. We discuss the possible
collisional or photoionized origin of the gas that emits the soft X-ray lines.
Our results, strengthened by optical spectroscopy favor the photoionization
scenario.Comment: 7 pages, 5 figures, accepted for publication in A&
Evolution of the disc atmosphere in the X-ray binary MXB 1659-298, during its 2015-2017 outburst
We report on the evolution of the X-ray emission of the accreting neutron
star (NS) low mass X-ray binary (LMXB), MXB 1659-298, during its most recent
outburst in 2015-2017. We detected 60 absorption lines during the soft state
(of which 21 at more than 3 ), that disappeared in the hard state
(e.g., the Fe xxv and Fe xxvi lines). The absorbing plasma is at rest, likely
part of the accretion disc atmosphere. The bulk of the absorption features can
be reproduced by a high column density () of highly
ionised () plasma. Its disappearance during the
hard state is likely the consequence of a thermal photo-ionisation instability.
MXB 1659-298's continuum emission can be described by the sum of an absorbed
disk black body and its Comptonised emission, plus a black body component. The
observed spectral evolution with state is in line with that typically observed
in atoll and stellar mass black hole LMXB. The presence of a relativistic Fe
K disk-line is required during the soft state. We also tentatively
detect the Fe xxii doublet, whose ratio suggests an electron density of the
absorber of , hence, the absorber is likely located at
from the illuminating source, well inside the Compton and
outer disc radii. MXB 1659-298 is the third well monitored atoll LMXB
showcasing intense Fe xxv and Fe xxvi absorption during the soft state that
disappears during the hard state.Comment: MNRAS in pres
Echoes of multiple outbursts of Sagittarius A* revealed by Chandra
The relatively rapid spatial and temporal variability of the X-ray radiation
from some molecular clouds near the Galactic center shows that this emission
component is due to the reflection of X-rays generated by a source that was
luminous in the past, most likely the central supermassive black hole,
Sagittarius A*. Studying the evolution of the molecular cloud reflection
features is therefore a key element to reconstruct Sgr A*'s past activity. The
aim of the present work is to study this emission on small angular scales in
order to characterize the source outburst on short time scales. We use Chandra
high-resolution data collected from 1999 to 2011 to study the most rapid
variations detected so far, those of clouds between 5' and 20' from Sgr A*
towards positive longitudes. Our systematic spectral-imaging analysis of the
reflection emission, notably of the Fe Kalpha line at 6.4 keV and its
associated 4-8 keV continuum, allows us to characterize the variations down to
15" angular scale and 1-year time scale. We reveal for the first time abrupt
variations of few years only and in particular a short peaked emission, with a
factor of 10 increase followed by a comparable decrease, that propagates along
the dense filaments of the Bridge cloud. This 2-year peaked feature contrasts
with the slower 10-year linear variations we reveal in all the other molecular
structures of the region. Based on column density constraints, we argue that
these two different behaviors are unlikely to be due to the same illuminating
event. The variations are likely due to a highly variable active phase of Sgr
A* sometime within the past few hundred years, characterized by at least two
luminous outbursts of a few-year time scale and during which the Sgr A*
luminosity went up to at least 10^39 erg/s.Comment: 17 pages, 16 figures, Accepted for publication in Astronomy &
Astrophysic
A pilot project to limit the human impacts on the fragile antarctic biota: Mitigation of a runway through vegetation transplantation
Background: Antarctica is among the world\u2019s last great wildernesses, but the anthropogenic activities and associated infrastructures threaten its fragile biota. We quantify the impact of the construction of a 2200 m long gravel runway airstrip for airfreight operations of the Italian research station on vegetation ecosystems at Boulder Clay (continental Antarctica). We propose a pilot project to mitigate this impact through the transplantation of vegetation from the runway to safe sites. Methods: A vegetation field survey was performed through phytosociological relev\ue9s and vegetation mapping and data were analyzed through multivariate analysis. Results: We quantify the destructive impact of the runway construction on the flora and vegetation of Boulder Clay. Based on vegetation characteristics, 28 priority areas were transplanted from the runway to safe sites, with 89% of survival. Conclusions: To our knowledge, this is the first time that vegetation transplantation was performed in Antarctica to mitigate the consequences of human actions, as formerly it was used only for scientific experiments. This pilot project provides a tool to support management decisions, involving the quantitative evaluation of the infrastructure impacts and showing the suitability of practical mitigation actions. This pilot project proposes a practical tool exportable to all Antarctica and beyond and suggests to link the permissions\u2019 release for the new infrastructures in Antarctica to the realization of specific conservation and mitigation actions
Sensation Seeking and Gambling Behavior in Adolescence: Can Externalizing Problems Moderate This Relationship?
Gambling is a widespread phenomenon during adolescence. Among different risk factors involved in the onset of adolescent gambling behaviors, one factor that is studied is the sensation seeking personality trait. However, the literature is heterogeneous and a direct relationship between sensation seeking and gaming behaviors has not always been highlighted. This suggests that the relationship can be influenced by other factors. In particular, we explored the moderating role of externalizing problems in this relationship. A total of 363 adolescents (232 males and 131 females) aged 14 to 20 (M = 16.35, SD = 1.36) completed a battery of questionnaires aimed to assess their gambling behaviors, as well as the levels of externalizing problems and sensation seeking. The results showed that sensation seeking was associated with gambling severity, but this relationship was significant when externalizing problems were high and medium. On the contrary, when externalizing problems were low, the relationship between sensation seeking and gambling severity was not significant. Overall, sensation seeking in adolescence can favor the implementation of risk behaviors, such as gambling, but only in association with the presence of externalizing problems. Limitations, strengths, and social and clinical implications of the present study are discussed
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