436 research outputs found
Properties of the Spatial Sections of the Space-Time of a Rotating System
We study the symmetry group of the geodesic equations of the spatial
solutions of the space-time generated by a noninertial rotating system of
reference. It is a seven dimensional Lie group, which is neither solvable nor
nilpotent. The variational symmetries form a five dimensional solvable
subgroup. Using the symplectic structure on the cotangent bundle we study the
resulting Hamiltonian system, which is closely related to the geodesic flow on
the spatial sections. We have also studied some intrinsic and extrinsic
geometrical properties of the spatial sections.Comment: 12 page
Near-Infrared Imaging Polarimetry of Young Stellar Objects in rho-Ophiuchi
The results of a near-infrared (J H K LP) imaging linear polarimetry survey
of 20 young stellar objects (YSOs) in rho Ophiuchi are presented. The majority
of the sources are unresolved, with K-band polarizations, P_K < 6 per cent.
Several objects are associated with extended reflection nebulae. These objects
have centrosymmetric vector patterns with polarization discs over their cores;
maximum polarizations of P_K > 20 per cent are seen over their envelopes.
Correlations are observed between the degree of core polarization and the
evolutionary status inferred from the spectral energy distribution. K-band core
polarizations >6 per cent are only observed in Class I YSOs. A 3D Monte Carlo
model with oblate grains aligned with a magnetic field is used to investigate
the flux distributions and polarization structures of three of the rho Oph YSOs
with extended nebulae. A rho proportional to r^(-1.5) power law for the density
is applied throughout the envelopes. The large-scale centrosymmetric
polarization structures are due to scattering. However, the polarization
structure in the bright core of the nebula appears to require dichroic
extinction by aligned non-spherical dust grains. The position angle indicates a
toroidal magnetic field in the inner part of the envelope. Since the measured
polarizations attributed to dichroic extinction are usually <10 per cent, the
grains must either be nearly spherical or very weakly aligned. The higher
polarizations observed in the outer parts of the reflection nebulae require
that the dust grains responsible for scattering have maximum grain sizes <=1.05
microns.Comment: 26 pages. Accepted by MNRAS. Available as online early versio
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Seismic retrofitting and health monitoring of school buildings of Cyprus
The vulnerability of existing buildings to seismic forces and their retrofitting is an international problem. The majority of structures in seismic-prone areas worldwide are structures that have been designed either without the consideration of seismic forces, or with previous codes of practice specifying lower levels of seismic forces. In Cyprus, after the three earthquakes that occurred in 1995, 1996, and 1999, the Cyprus State, acting in a pioneering way internationally, has decided the seismic retrofitting of all school buildings, taking into account the sensitivity of the society towards these structures, which house the future generation of the society. In this paper the overall assessment methodology is presented, along with details of the over 10 year ongoing retrofitting program of the school buildings of Cyprus, with emphasis on the description of the program and the development of a wireless monitoring system. In addition, mathematical models of selected school buildings are presented and comparison is made with in-situ measurement
Dust-driven Dynamos in Accretion Disks
Magnetically driven astrophysical jets are related to accretion and involve
toroidal magnetic field pressure inflating poloidal magnetic field flux
surfaces. Examination of particle motion in combined gravitational and magnetic
fields shows that these astrophysical jet toroidal and poloidal magnetic fields
can be powered by the gravitational energy liberated by accreting dust grains
that have become positively charged by emitting photo-electrons. Because a dust
grain experiences magnetic forces after becoming charged, but not before,
charging can cause irreversible trapping of the grain so dust accretion is a
consequence of charging. Furthermore, charging causes canonical angular
momentum to replace mechanical angular momentum as the relevant constant of the
motion. The resulting effective potential has three distinct classes of
accreting particles distinguished by canonical angular momentum, namely (i)
"cyclotron-orbit", (ii) "Speiser-orbit", and (iii) "zero canonical angular
momentum" particles. Electrons and ions are of class (i) but depending on mass
and initial orbit inclination, dust grains can be of any class. Light-weight
dust grains develop class (i) orbits such that the grains are confined to
nested poloidal flux surfaces, whereas grains with a critical weight such that
they experience comparable gravitational and magnetic forces can develop class
(ii) or class (iii) orbits, respectively producing poloidal and toroidal field
dynamos.Comment: 70 pages, 16 figure
UV Circular Polarisation in Star Formation Regions : The Origin of Homochirality?
Ultraviolet circularly polarised light has been suggested as the initial cause of the homochirality of organic molecules in terrestrial organisms, via enantiomeric selection of prebiotic molecules by asymmetric photolysis. We present a theoretical investigation of mechanisms by which ultraviolet circular polarisation may be produced in star formation regions. In the scenarios considered here, light scattering produces only a small percentage of net circular polarisation at any point in space, due to the forward throwing nature of the phase function in the ultraviolet. By contrast, dichroic extinction can produce a fairly high percentage of net circular polarisation (∼10%) and may therefore play a key role in producing an enantiomeric excessPeer reviewe
High Resolution Millimeter-Wave Mapping of Linearly Polarized Dust Emission: Magnetic Field Structure in Orion
We present 1.3 and 3.3 mm polarization maps of Orion-KL obtained with the
BIMA array at approximately 4 arcsec resolution. Thermal emission from
magnetically aligned dust grains produces the polarization. Along the Orion
``ridge'' the polarization position angle varies smoothly from about 10 degrees
to 40 degrees, in agreement with previous lower resolution maps. In a small
region south of the Orion ``hot core,'' however, the position angle changes by
90 degrees. This abrupt change in polarization direction is not necessarily the
signpost of a twisted magnetic field. Rather, in this localized region
processes other than the usual Davis-Greenstein mechanism might align the dust
grains with their long axes parallel with the field, orthogonal to their normal
orientation.Comment: AAS preprint:14 pages, 2 figures (3mm.eps and 1mm.eps); requires
aaspp4.sty To be published in Astrophysical Journal Letter
ISO observations toward the reflection nebula NGC 7023: A nonequilibrium ortho- to para-H2 ratio
We have observed the S(0), S(1), S(2), S(3), S(4) and S(5) rotational lines
of molecular hydrogen (H2) towards the peak of the photodissociation region
(PDR) associated with the reflection nebula NGC 7023. The observed H2 line
ratios show that they arise in warm gas with kinetic temperatures ~300 - 700 K.
However, the data cannot be fitted by an ortho- to para- (OTP) ratio of 3. An
OTP ratio in the range ~1.5 - 2 is necessary to explain our observations. This
is the first detection of a non-equilibrium OTP ratio measured from the H2
pure-rotational lines in a PDR. The existence of a dynamical PDR is discussed
as the most likely explanation for this low OTP ratio.Comment: 4 pages, 3 figure
Investigating the transport of angular momentum from young stellar objects: do H2 jets from Class I YSOs rotate?
In this pilot study, we examine molecular jets from the embedded Class I
sources, HH 26 and HH 72, to search, for the first time, for kinematic
signatures of jet rotation from young embedded sources.High resolution
long-slit spectroscopy of the H2 1-0 S(1) transition was obtained using
VLT/ISAAC, position-velocity (PV) diagrams constructed and intensity-weighted
radial velocities transverse to the jet flow measured. Mean intensity-weighted
velocities vary between vLSR ~ -90 and -65 km/s for HH 26, and -60 and -10 km/s
for HH 72; maxima occur close to the intensity peak and decrease toward the jet
borders. Velocity dispersions are ~ 45 and ~ 80 km/s for HH 26 and HH 72,
respectively, with gas motions as fast as -100 km/s present. Asymmetric PV
diagrams are seen for both objects which a simple empirical model of a
cylindrical jet section shows could in principle be reproduced by jet rotation
alone. Assuming magneto-centrifugal launching, the observed HH 26 flow may
originate at a disk radius of 2-4 AU from the star with the toroidal component
of the magnetic field dominant at the observed location, in agreement with
magnetic collimation models. We estimate that the kinetic angular momentum
transported by the HH 26 jet is ~ 2E5 M_sun/yr AU km/s. This value (a lower
limit to the total angular momentum transported by the flow) already amounts to
70% of the angular momentum that has to be extracted from the disk for the
accretion to proceed at the observed rate.
The results of this pilot study suggest that jet rotation may also be present
at early evolutionary phases and supports the hypothesis that they carry away
excess angular momentum, thus allowing the central protostar to increase its
mass.Comment: 11 pages, 5 figures, accepted for publication in Astronomy &
Astrophysic
HeI 1.083 micron emission and absorption in DG Tau: line excitation in jet, hot wind, and accretion flow
We present long-slit spectroscopy and spectro-astrometry of HeI 1.083 micron
emission in the T Tauri star, DG Tau. We identify three components in the HeI
feature: (1) a blueshifted emission component atv -200 km s^-1, (2) a bright
emission component at zero-velocity with a FWZI of ~500 km s^-1, and (3) a
blueshifted absorption feature at velocities between -250 and -500 km s^-1. The
position and velocity of the blueshifted HeI emission coincide with a
high-velocity component (HVC) of the [FeII] 1.257 micron emission, which arises
from a jet within an arcsecond of the star. The presence of such a high
excitation line (excitation energy ~ 20 eV) within the jet supports the
scenario of shock heating. The bright HeI component does not show any spatial
extension, and it is likely to arise from magnetospheric accretion columns.
The blueshifted absorption shows greater velocities than that in H-alpha,
suggesting that these absorption features arise from the accelerating wind
close to the star.Comment: 10 pages including 2 figures, accepted for publication in the
Astrophysical Journal Letter
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