8,810 research outputs found
Continuous-flow IRMS technique for determining the 17O excess of CO2 using complete oxygen isotope exchange with cerium oxide
This paper presents an analytical system for analysis of all single
substituted isotopologues (<sup>12</sup>C<sup>16</sup>O<sup>17</sup>O,
<sup>12</sup>C<sup>16</sup>O<sup>18</sup>O, <sup>13</sup>C<sup>16</sup>O<sup>16</sup>O) in nanomolar quantities
of CO<sub>2</sub> extracted from stratospheric air samples. CO<sub>2</sub> is
separated from bulk air by gas chromatography and CO<sub>2</sub> isotope ratio
measurements (ion masses 45 / 44 and 46 / 44) are performed using isotope ratio
mass spectrometry (IRMS). The <sup>17</sup>O excess (Î<sup>17</sup>O) is
derived from isotope measurements on two different CO<sub>2</sub> aliquots:
unmodified CO<sub>2</sub> and CO<sub>2</sub> after complete oxygen isotope exchange with
cerium oxide (CeO<sub>2</sub>) at 700 °C. Thus, a single measurement of
Î<sup>17</sup>O requires two injections of 1 mL of air with a CO<sub>2</sub>
mole fraction of 390 ÎŒmol mol<sup>â1</sup> at 293 K and 1 bar pressure
(corresponding to 16 nmol CO<sub>2</sub> each). The required sample size
(including flushing) is 2.7 mL of air. A single analysis (one pair of
injections) takes 15 minutes. The analytical system is fully automated for
unattended measurements over several days. The standard deviation of the
<sup>17</sup>O excess analysis is 1.7‰. Multiple
measurements on an air sample reduce the measurement uncertainty, as
expected for the statistical standard error. Thus, the uncertainty for a
group of 10 measurements is 0.58‰ for Δ
<sup>17</sup>O in 2.5 h of analysis. 100 repeat analyses of one air sample
decrease the standard error to 0.20‰. The instrument
performance was demonstrated by measuring CO<sub>2</sub> on stratospheric air
samples obtained during the EU project RECONCILE with the high-altitude
aircraft Geophysica. The precision for RECONCILE data is 0.03‰ (1σ) for ÎŽ<sup>13</sup>C, 0.07‰ (1σ) for ÎŽ<sup>18</sup>O and 0.55‰ (1σ) for δ<sup>17</sup>O for a sample of 10
measurements. This is sufficient to examine stratospheric enrichments, which
at altitude 33 km go up to 12‰ for δ<sup>17</sup>O
and up to 8‰ for ÎŽ<sup>18</sup>O with respect to
tropospheric CO<sub>2</sub> : δ<sup>17</sup>O ~
21‰ Vienna Standard Mean Ocean Water (VSMOW), ÎŽ<sup>18</sup>O ~
41‰ VSMOW (LĂ€mmerzahl et al., 2002). The samples
measured with our analytical technique agree with available data for
stratospheric CO<sub>2</sub>
OH-selected AGB and post-AGB objects I.Infrared and maser properties
Using 766 compact objects from a survey of the galactic Plane in the 1612-MHz
OH line, new light is cast on the infrared properties of evolved stars on the
TP-AGB and beyond. The usual mid-infrared selection criteria, based on IRAS
colours, largely fail to distinguish early post-AGB stages. A two-colour
diagram from narrower-band MSX flux densities, with bimodal distributions,
provides a better tool to do the latter. Four mutually consistent selection
criteria for OH-masing red PPNe are given, as well as two for early post-AGB
masers and one for all post--AGB masers, including the earliest ones. All these
criteria miss a group of blue, high-outflow post-AGB sources with 60-mum
excess; these will be discussed in detail in Paper II. The majority of post-AGB
sources show regular double-peaked spectra in the OH 1612-MHz line, with fairly
low outflow velocities, although the fractions of single peaks and irregular
spectra may vary with age and mass. The OH flux density shows a fairly regular
relation with the stellar flux and the envelope optical depth, with the maser
efficiency increasing with IRAS colour R21. The OH flux density is linearly
correlated with the 60-mum flux density.Comment: 16 pages, LaTex, 22 figures, AJ (accepted
Surface defreezing of glasses
A glass surface may still flow below the bulk glass transition temperature,
where the underlying bulk is frozen. Assuming the existence at T=T* of a bulk
thermodynamical glass transition, we show that the glass-vapor interface is
generally wetted by a liquid layer of thickness ~ -ln(T*-T) when T--> T*.
Contrary to standard surface melting of crystals however, the integrated value
of the diffusivity across the interface remains finite for T-->T*. Difference
in shape induced by bulk and by surface flow is discussed as a possible means
of experimental detection of surface defreezing.Comment: five pages, three figure
Mass-luminosity relation and pulsational properties of Wolf-Rayet stars
Evolution of Population I stars with initial masses from 70M_\odot to
130M_\odot is considered under various assumptions on the mass loss rate \dot
M. The mass-luminosity relation of W-R stars is shown to be most sensitive to
the mass loss rate during the helium burning phase \dot M_{3\alpha}. Together
with the mass-luminosity relation obtained for all evolutionary sequences
several more exact relations are determined for the constant ratio
f_{3\alpha}=\dot M/\dot M_{3\alpha} with 0.5 \le f_{3\alpha} \le 3.
Evolutionary models of W-R stars were used as initial conditions in
hydrodynamic computations of radial nonlinear stellar oscillations. The
oscillation amplitude is larger in W-R stars with smaller initial mass or with
lower mass loss rate due to higher surface abundances of carbon and oxygen. In
the evolving W-R star the oscillation amplitude decreases with decreasing
stellar mass M and for M < 10M_\odot the sufficiently small nonlinear effects
allow us to calculate the integral of the mechanical work W done over the
pulsation cycle in each mass zone of the hydrodynamical model. The only
positive maximum on the radial dependence of W is in the layers with
temperature of T\sim 2e5K where oscillations are excited by the iron Z--bump
kappa-mechanism. Radial oscillations of W-R stars with mass of M > 10M_\odot
are shown to be also excited by the kappa-mechanism but the instability driving
zone is at the bottom of the envelope and pulsation motions exist in the form
of nonlinear running waves propagating outward from the inner layers of the
envelope.Comment: 15 pages, 10 figures, submitted to Astronomy Letter
Spectral Characteristics of Greenland Lichens
Spectral reflectance measurements conducted during two field campaigns in west Greenland, and in the laboratory using samples collected during those campaigns, are discussed to evaluate the spectral signature of lichens. Given the diversity in lichen species, colors, and appearance â ranging from crust-like (crustose) to almost like mini shrubs (fructicose) â it is not surprising that no single signature was found. Some of the brighter fructicose lichens have reflectance characteristics very similar to those of green vegetation, with a pronounced rise in reflectivity around 750 nm. However, the most abundant lichen species covering rocks in the ice-marginal zone of west Greenland are dark grey to black crustose and foliose ephilithic (rock-growing) lichens and the shape of the reflectance spectrum for these lichens is generally very different from that of other surface types and landcovers, with near-zero reflectance at visible wavelengths, and a maximum around 1 600 nm. This characteristic allows rock-covered lichen to be identified on multispectral satellite imagery.LâĂ©valuation de la signature spectrale des lichens est effectuĂ©e Ă partir de mesures prises en laboratoire et sur le terrain, au Groenland occidental. Aucune signature spĂ©cifique ne peut ĂȘtre identifiĂ©e, en raison de la diversitĂ© des espĂšces quant Ă leur couleur et Ă leur port, allant de la croĂ»te Ă lâarbuste nain. Les lichens arbustifs les plus brillants montrent une signature spectrale semblable Ă celle des plantes vertes, avec un pic trĂšs prononcĂ© autour de 750 nm. Toutefois, les lichens les plus abondants sur les roches Ă proximitĂ© des glaces sont gris foncĂ©s Ă noirs et du type crustacĂ© ou foliacĂ©; leur spectre de rĂ©flectance montre une allure trĂšs diffĂ©rente de celle des autres types de surface et de couverture, et se rapproche de zĂ©ro dans le spectre visible avec un pic autour de 1 600 nm. Cette caractĂ©ristique permet lâidentification des roches recouvertes de lichens par lâimagerie satellitaire multispectrale
The COBE DIRBE Point Source Catalog
We present the COBE DIRBE Point Source Catalog, an all-sky catalog containing
infrared photometry in 10 bands from 1.25 microns to 240 microns for 11,788 of
the brightest near and mid-infrared point sources in the sky. Since DIRBE had
excellent temporal coverage (100 - 1900 independent measurements per object
during the 10 month cryogenic mission), the Catalog also contains information
about variability at each wavelength, including amplitudes of variation
observed during the mission. Since the DIRBE spatial resolution is relatively
poor (0.7 degrees), we have carefully investigated the question of confusion,
and have flagged sources with infrared-bright companions within the DIRBE beam.
In addition, we filtered the DIRBE light curves for data points affected by
companions outside of the main DIRBE beam but within the `sky' portion of the
scan. At high Galactic latitudes (|b| > 5 degrees), the Catalog contains
essentially all of the unconfused sources with flux densities greater than 90,
60, 60, 50, 90, and 165 Jy at 1.25, 2.2, 3.5, 4.9, 12, and 25 microns,
respectively, corresponding to magnitude limits of approximately 3.1, 2.6, 1.7,
1.3, -1.3, and -3.5. At longer wavelengths and in the Galactic Plane, the
completeness is less certain because of the large DIRBE beam and possible
contributions from extended emission. The Catalog also contains the names of
the sources in other catalogs, their spectral types, variability types, and
whether or not the sources are known OH/IR stars. We discuss a few remarkable
objects in the Catalog. [abridged]Comment: Accepted for publication in the Astrophysical Journal Supplement. The
full tables are available at http://www.etsu.edu/physics/bsmith/dirbe
Patterns of calculated basal drag on ice streams B and C, Antarctica
This is the published version.Patterns of strain rate and slope on the ice streams are unusual.
They cannot be accounted for in the usual way as due to standing waves in ice flow
over a basal obstruction to flow (such as a sticky spot) . The features are studied using
the force-budget technique. The conventional flow law is used, together with
measurements of surface strain rate and shape of the glacier, to compute basal drag.
The results for Ice Stream C are as expected, in that the drag varies from site to site
but is directed inland, restraining the flow. The calculated drag at the base of Ice
Stream B, on the other hand, is in places such that it acts to propel the glacier
forward. This result is untenable. Either the conventional flow law is not applicable
to Ice Stream B or there are large spatial variations in ice stiffness, perhaps associated
with foliation, or both
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