758 research outputs found
On the Weakening of Chromospheric Magnetic Field in Active Regions
Simultaneous measurement of line-of-sight (LOS) magnetic and velocity fields
at the photosphere and chromosphere are presented. Fe I line at
and at are used respectively for deriving the
physical parameters at photospheric and chromospheric heights. The LOS magnetic
field obtained through the center-of-gravity method show a linear relation
between photospheric and chromospheric field for field strengths less than 700
G. But in strong field regions, the LOS magnetic field values derived from
are much weaker than what one gets from the linear relationship
and also from those expected from the extrapolation of the photospheric
magnetic field. We discuss in detail the properties of magnetic field observed
in from the point of view of observed velocity gradients. The
bisector analysis of Stokes profiles show larger velocity
gradients in those places where strong photospheric magnetic fields are
observed. These observations may support the view that the stronger fields
diverge faster with height compared to weaker fields.Comment: accepted for publication in Ap
Gravitational Baryogenesis: Problems and Possible Resolution
The coupling of baryonic current to the derivative of the curvature scalar,
, inherent to gravitational baryogenesis (GBG), leads to a fourth order
differential equation of motion for instead of the algebraic one of General
Relativity (GR). The fourth-order differential equation is generically
unstable. We consider a possible mechanism of stabilization of GBG by
modification of gravity, introducing an -term into the canonical action of
GR.
It is shown that this mechanism allows for stabilization of GBG with bosonic
and fermionic baryon currents. We have established the region of the model
parameters leading to stabilization of . Still, the standard cosmology would
be noticeably modified.Comment: 11 pages, no figures, presented at International Conference
on Particle Physics and Astrophysics (ICCPA-2022)}. arXiv admin note: text
overlap with arXiv:1808.0857
Generalization of Linearized Gouy-Chapman-Stern Model of Electric Double Layer for Nanostructured and Porous Electrodes: Deterministic and Stochastic Morphology
We generalize linearized Gouy-Chapman-Stern theory of electric double layer
for nanostructured and morphologically disordered electrodes. Equation for
capacitance is obtained using linear Gouy-Chapman (GC) or
Debye-ckel equation for potential near complex
electrode/electrolyte interface. The effect of surface morphology of an
electrode on electric double layer (EDL) is obtained using "multiple scattering
formalism" in surface curvature. The result for capacitance is expressed in
terms of the ratio of Gouy screening length and the local principal radii of
curvature of surface. We also include a contribution of compact layer, which is
significant in overall prediction of capacitance. Our general results are
analyzed in details for two special morphologies of electrodes, i.e.
"nanoporous membrane" and "forest of nanopillars". Variations of local shapes
and global size variations due to residual randomness in morphology are
accounted as curvature fluctuations over a reference shape element.
Particularly, the theory shows that the presence of geometrical fluctuations in
porous systems causes enhanced dependence of capacitance on mean pore sizes and
suppresses the magnitude of capacitance. Theory emphasizes a strong influence
of overall morphology and its disorder on capacitance. Finally, our predictions
are in reasonable agreement with recent experimental measurements on
supercapacitive mesoporous systems
Draft proposal for establishment of CNC centre at NAL
This is a proposal for setting up Computer Numerically Controlled machining facilities at N.A.L. to cater to the increasing requirements for fabrication of complex shaped and intricate/precision components for the aerospace R & D projects of the laboratory for the next 10 - year period. This fairly comprehensive document has been prepared by an
internal technical committee constituted by the Director, after detailed study and discussions and covers the technical and financial aspects for setting up such facilities
Chandra Observations of Gas Stripping in the Elliptical Galaxy NGC 4552 in the Virgo Cluster
We use a 54.4 ks Chandra observation to study ram-pressure stripping in
NGC4552 (M89), an elliptical galaxy in the Virgo Cluster. Chandra images in the
0.5-2 keV band show a sharp leading edge in the surface brightness 3.1 kpc
north of the galaxy center, a cool (kT =0.51^{+0.09}_{-0.06} keV) tail with
mean density n_e ~5.4 +/- 1.7 x 10^{-3} cm^{-3} extending ~10 kpc to the south
of the galaxy, and two 3-4 kpc horns of emission extending southward away from
the leading edge. These are all features characteristic of supersonic
ram-pressure stripping of galaxy gas, due to NGC4552's motion through the
surrounding Virgo ICM. Fitting the surface brightness profile and spectra
across the leading edge, we find the galaxy gas inside the edge is cooler (kT =
0.43^{+0.03}_{-0.02} keV) and denser (n_e ~ 0.010 cm^{-3}) than the surrounding
Virgo ICM (kT = 2.2^{+0.7}_{-0.4} keV and n_e = 3.0 +/- 0.3 x 10^{-4} cm^{-3}).
The resulting pressure ratio between the free-streaming ICM and cluster gas at
the stagnation point is ~7.6^{+3.4}_{-2.0} for galaxy gas metallicities of
0.5^{+0.5}_{-0.3} Zsolar, which suggests that NGC4552 is moving supersonically
through the cluster with a velocity v ~ 1680^{+390}_{-220} km/s (Mach
2.2^{+0.5}_{-0.3}) at an angle xi ~ 35 +/- 7 degrees towards us with respect to
the plane of the sky.Comment: 31 pages, 12 figures, ApJ, in press; paper split into 2 parts, Paper
I(sec 1-3) here, added figs and discussion to conform to published version;
Paper II (sec. 4) in astro-ph/060440
Deep ROSAT-HRI observations of the NGC 1399/NGC 1404 region: morphology and structure of the X-ray halo
We present the analysis of a deep (167 ks) ROSAT HRI observation of the cD
galaxy NGC 1399 in the Fornax cluster. Using both HRI and, at larger radii,
archival PSPC data, we find that the radial behavior of the X-ray surface
brightness profile is not consistent with a simple Beta model and suggests
instead three distinct components. We use a multi-component bidimensional model
to study in detail these three components that we identify respectively with
the cooling flow region, the galactic and the cluster halo. From these data we
derive a binding mass distribution in agreement with that suggested by optical
dynamical indicators, with an inner core dominated by luminous matter and an
extended dark halo differently distributed on galactic and cluster scales. The
HRI data and a preliminary analysis of Chandra public data, allow us to detect
significant density fluctuations in the halo. We discuss possible
non-equilibrium scenarios to explain the hot halo structure, including tidal
interactions with neighboring galaxies, ram stripping from the intra-cluster
medium and merging events. In the innermost region of NGC 1399, the comparison
between the X-ray and radio emission suggests that the radio emitting plasma is
displacing and producing shocks in the hot X-ray emitting gas. We found that
the NGC 1404 halo is well represented by a single symmetric Beta model and
follows the stellar light profile within the inner 8 kpc. The mass distribution
is similar to the `central' component of the NGC 1399 halo. At larger radii ram
pressure stripping from the intra-cluster medium produces strong asymmetries in
the gas distribution. Finally we discuss the properties of the point source
population finding evidence of correlation between the source excess and NGC
1399.Comment: 34 pages in aastex5.0 format, including 28 B&W and 4 color figures.
Uses LaTex packages: subfigure, lscape and psfig. Accepted for publication in
ApJ. High resolution version can be found at:
http://www.na.astro.it/~paolillo/publications.htm
The Ionized Gas Kinematics of the LMC-Type Galaxy NGC 1427A in the Fornax Cluster
NGC 1427A is a LMC-like irregular galaxy in the Fornax cluster with an
extended pattern of strong star formation around one of its edges, which is
probably due to some kind of interaction with the cluster environment. We
present H-alpha velocities within NGC 1427A, obtained through long-slit
spectroscopy at seven different positions, chosen to fall on the brightest HII
regions of the galaxy. Due to its location very near the center of the cluster
this object is an excellent candidate to study the effects that the cluster
environment has on gas-rich galaxies embedded in it. The rotation of NGC 1427A
is modeled in two different ways. The global ionized gas kinematics is
reasonably well described by solid-body rotation, although on small scales it
shows a chaotic behaviour. In this simple model, the collision with a smaller
member of the cluster as being responsible for the peculiar morphology of NGC
1427A is very unlikely, since the only candidate intruder falls smoothly into
the general velocity pattern of the main galaxy. In a more elaborate model, for
which we obtain a better solution, this object does not lie in the same plane
of NGC 1427A, in which case we identify it as a satellite bound to the galaxy.
These results are discussed in the context of a normal irregular versus one
interacting with some external agent. Based on several arguments and
quantitative estimates, we argue that the passage through the hot intracluster
gas of the Fornax cluster is a very likely scenario to explain the
morphological properties of NGC 1427A.Comment: 31 pages, LaTeX2e, uses aas2pp4.sty and psfig.sty, including 7
Postscript figures; accepted for publication in ApJ, Vol. 530, February 200
Inflationary Baryogenesis
In this letter we explore the possibility of creating the baryon asymmetry of
the universe during inflation and reheating due to the decay of a field
associated with the inflaton. CP violation is attained by assuming that this
field is complex with a phase that varies as the inflaton evolves. We consider
chaotic and natural inflation scenarios. In the former case, the complex
decaying field is the inflaton itself and, in the latter case, the phase of the
complex field is the inflaton. We calculate the asymmetry produced using the
Bogolyubov formalism that relates annihilation and creation operators at late
time to the annihilation and creation operators at early time.Comment: 17 pages, Revte
General Stability Analysis of Synchronized Dynamics in Coupled Systems
We consider the stability of synchronized states (including equilibrium
point, periodic orbit or chaotic attractor) in arbitrarily coupled dynamical
systems (maps or ordinary differential equations). We develop a general
approach, based on the master stability function and Gershgorin disc theory, to
yield constraints on the coupling strengths to ensure the stability of
synchronized dynamics. Systems with specific coupling schemes are used as
examples to illustrate our general method.Comment: 8 pages, 1 figur
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