46,692 research outputs found
X-ray inverse Compton emission from the radio halo of M87
M87 has been observed in the 0.2-4 KeV X-ray band using the High Resolution Imager on the Einstein Observatory, and at 1.452 GHz using the Very Large Array. The radio map showed that the halo contained prominent asymmetries to the east and southwest. The X-ray map indicated similar asymmetries, but they were imbedded in the diffuse hot gas that surrounds the core out to a radius of several arcminutes. The hot X-ray emitting gas was assumed to be spherically symmetric and could, therefore, be subtracted from the image. The resultant image was asymmetric with major lobes to the east and southwest that coincide approximately with the asymmetries in the radio halo. The data indicates that inverse Compton emission is a plausible model for the X-rays coming from the asymmetric component
Radial Velocity Curves of Ellipsoidal Red Giant Binaries in the Large Magellanic Cloud
Ellipsoidal red giant binaries are close binary systems where an unseen,
relatively close companion distorts the red giant, leading to light variations
as the red giant moves around its orbit. These binaries are likely to be the
immediate evolutionary precursors of close binary planetary nebula and
post-asymptotic giant branch and post-red giant branch stars. Due to the MACHO
and OGLE photometric monitoring projects, the light variability nature of these
ellipsoidal variables has been well studied. However, due to the lack of radial
velocity curves, the nature of their masses, separations, and other orbital
details has so far remained largely unknown. In order to improve this
situation, we have carried out spectral monitoring observations of a large
sample of 80 ellipsoidal variables in the Large Magellanic Cloud and we have
derived radial velocity curves. At least 12 radial velocity points with good
quality were obtained for most of the ellipsoidal variables. The radial
velocity data are provided with this paper. Combining the photometric and
radial velocity data, we present some statistical results related to the binary
properties of these ellipsoidal variables.Comment: 10 pages, 8 figures, 3 table
A microcontroller system for investigating the catch effect: Functional electrical stimulation of the common peroneal nerve
Correction of drop foot in hemiplegic gait is achieved by electrical stimulation of the common peroneal nerve with a series of pulses at a fixed frequency. However, during normal gait, the electromyographic signals from the tibialis anterior muscle indicate that muscle force is not constant but varies during the swing phase. The application of double pulses for the correction of drop foot may enhance the gait by generating greater torque at the ankle and thereby increase the efficiency of the stimulation with reduced fatigue. A flexible controller has been designed around the Odstock Drop Foot Stimulator to deliver different profiles of pulses implementing doublets and optimum series. A peripheral interface controller (PIC) microcontroller with some external circuits has been designed and tested to accommodate six profiles. Preliminary results of the measurements from a normal subject seated in a multi-moment chair (an isometric torque measurement device) indicate that profiles containing doublets and optimum spaced pulses look favourable for clinical use
Inverting a Supernova: Neutrino Mixing, Temperatures and Binding Energy
We show that the temperatures of the emergent non-electron neutrinos and the
binding energy released by a galactic Type II supernova are determinable,
assuming the Large Mixing Angle (LMA) solution is correct, from observations at
the Sudbury Neutrino Observatory (SNO) and at Super-Kamiokande (SK). If the
neutrino mass hierarchy is inverted, either a lower or upper bound can be
placed on the neutrino mixing angle , and the hierarchy can be
deduced for adiabatic transitions. For the normal hierarchy, neither can
be constrained nor can the hierarchy be determined. Our
conclusions are qualitatively unchanged for the proposed Hyper-Kamiokande
detector.Comment: Following astro-ph/0208035, we adopt electron and non-electron
neutrino spectra with very small differences. Conclusions change
Mobility of Edge Dislocations in the Basal‐Slip System of Zinc
This paper presents the results of measurements of the velocities of 〈1210〉 (0001) edge dislocations in zinc as a function of applied shear stress. All tests were conducted at room temperature on 99.999% pure zinc monocrystals. Dislocations were revealed by means of the Berg‐Barrett x‐ray technique. Stress pulses of microsecond duration were applied to the test specimens by means of a torsion testing machine. Applied resolved shear stresses ranged from 0 to 17.2×10^6 dyn∕cm^2 and measured dislocation velocities ranged from 40–700 cm∕sec. The results of this study indicate that the velocity of edge dislocations in the basal slip system of zinc is linearly proportional to the applied resolved shear stress. These results are analyzed in terms of the phonon drag theory. Agreement between this theory and the results reported here is quite good
Optically visible post-AGB/RGB stars and young stellar objects in the Small Magellanic Cloud: candidate selection, spectral energy distributions and spectroscopic examination
We have carried out a search for optically visible post-AGB candidates in the
Small Magellanic Cloud (SMC). We used mid-IR observations from the Spitzer
Space Telescope to select optically visible candidates with a mid-IR excess. We
obtained low-resolution optical spectra for 801 candidates. After removing
contaminants and poor quality spectra, the final sample comprised of 63
post-AGB/RGB candidates of A - F spectral type. Using the spectra, we estimated
the stellar parameters: effective temperature, surface gravity and [Fe/H]. We
also estimated the reddening and deduced the luminosity using the stellar
parameters combined with photometry. Based on a luminosity criterion, 42 of
these 63 sources were classified as post-RGB candidates and the remaining as
post-AGB candidates. From the spectral energy distributions we found that 6 of
the 63 post-AGB/RGB candidates have a circumstellar shell suggesting that they
are single stars, while 27 of them have a surrounding disc, suggesting that
they are binaries. For the remaining candidates the nature of the circumstellar
environment was unclear. Variability is displayed by 38 post-AGB/RGB candidates
with common variability types being the Population II Cepheids (including
RV-Tauri stars) and semi-regular variables. This study has also revealed a new
s-process enriched RV Tauri star (J005107.19-734133.3). From the numbers of
post-AGB/RGB stars in the SMC, we were able to estimate evolutionary rates that
are in good agreement with the stellar evolution models with mass loss in the
post-AGB phase and re-accretion in the post-RGB phase. This study also resulted
in a new sample of 40 luminous young stellar objects (YSOs) of A - F spectral
type. Additionally, we also identified a group of 63 objects whose spectra are
dominated by emission lines and in some cases, a UV continuum. These objects
are likely to be either hot post-AGB/RGBs or luminous YSOs.Comment: 67 pages, 26 figures, 20 tables, 3 appendices + online supporting
information on CD
Magellanic Cloud stars with TiO bands in emission: binary post-RGB/AGB stars or young stellar objects?
Fourteen stars from a sample of Magellanic Cloud objects selected to have a
mid-infrared flux excess have been found to also show TiO bands in emission.
The mid-infrared dust emission and the TiO band emission indicate that these
stars have large amounts of hot circumstellar dust and gas in close proximity
to the central star. The luminosities of the sources are typically several
thousand L_sun while the effective temperatures are 4000-8000 K. Such stars
could be post-AGB stars of mass 0.4-0.8 M_sun or pre-main-sequence stars (young
stellar objects) with masses of 7-19 M_sun. If the stars are pre-main-sequence
stars, they are substantially cooler and younger than stars at the birth line
where Galactic protostars are first supposed to become optically visible out of
their molecular clouds. They should therefore be hidden in their present
evolutionary state. The second explanation for these stars is that they are
post-AGB or post-RGB stars that have recently undergone a binary interaction
when the red giant of the binary system filled its Roche lobe. Being
oxygen-rich, they have gone through this process before becoming carbon stars.
Most of the stars vary slowly on timescales of 1000 days or more suggesting a
changing circumstellar environment. Apart from the slow variations, most stars
also show variability with periods of tens to hundreds of days. One star shows
a period that is rapidly decreasing and we speculate that this star may have
accreted a large blob of gas and dust onto a disk whose orbital radius is
shrinking rapidly. Another star has Cepheid-like pulsations of rapidly
increasing amplitude suggesting a rapid rate of evolution. Seven stars show
quasi-periodic variability and one star has a light curve similar to that of an
eclipsing binary.Comment: 15 pages, 2 tables, 8 figures, MNRAS, in pres
Phonon entropy of alloying and ordering of Cu-Au
Inelastic neutron scattering spectra were measured with a time-of-flight spectrometer on six disordered Cu-Au alloys at 300 K. The neutron-weighted phonon density of states was obtained from a conventional analysis of these spectra. Several methods were developed to account for this neutron weighting and obtain the phonon entropy of the disordered alloys. The phonon entropies of formation of disordered fcc Cu-Au alloys obtained in this way were generally mutually consistent, and were also consistent with predictions from a cluster approximation obtained from ab-initio calculations by Ozolin[underaccent cedilla [below] s-breve, Wolverton, and Zunger. We estimate a phonon entropy of disordering of 0.15±0.05kB/atom in Cu3Au at 300 K. A resonance mode associated with the motions of the heavy Au atoms in the Cu-rich alloys was observed at 9 meV. An analysis of the resonance mode provided a check on the partial phonon entropy of Au atoms
A newly discovered stellar type: dusty post-red giant branch stars in the Magellanic Clouds
Context: We present a newly discovered class of low-luminosity, dusty,
evolved objects in the Magellanic Clouds. These objects have dust excesses,
stellar parameters, and spectral energy distributions similar to those of dusty
post-asymptotic giant branch (post-AGB) stars. However, they have lower
luminosities and hence lower masses. We suggest that they have evolved off the
red giant branch (RGB) instead of the AGB as a result of binary interaction.
Aims: In this study we aim to place these objects in an evolutionary context
and establish an evolutionary connection between RGB binaries (such as the
sequence E variables) and our new sample of objects. Methods: We compared the
theoretically predicted birthrates of the progeny of RGB binaries to the
observational birthrates of the new sample of objects. Results: We find that
there is order-of-magnitude agreement between the observed and predicted
birthrates of post-RGB stars. The sources of uncertainty in the birthrates are
discussed; the most important sources are probably the observational
incompleteness factor and the post-RGB evolution rates. We also note that
mergers are relatively common low on the RGB and that stars low on the RGB with
mid-IR excesses may recently have undergone a merger. Conclusions: Our sample
of dusty post-RGB stars most likely provides the first observational evidence
for a newly discovered phase in binary evolution: post-RGB binaries with
circumstellar dust.Comment: Accepted for publication in Astronomy and Astrophysics Letter
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