615 research outputs found
Evidence for an external origin of heavy elements in hot DA white dwarfs
We present a series of systematic abundance measurements for 89 hydrogen
atmosphere (DA-type) white dwarfs with temperatures spanning 16000-77000K drawn
from the FUSE spectral archive. This is the largest study to date of white
dwarfs where radiative forces are significant, exceeding our earlier work,
based mainly on IUE and HST data, by a factor three. Using heavy element
blanketed non-LTE stellar atmosphere calculations, we have addressed the heavy
element abundance patterns making completely objective measurements of
abundance values and their error ranges using a \c{hi}2 fitting technique. We
are able to establish the broad range of abundances seen in a given temperature
range and establish the incidence of stars which appear, in the optical, to be
atmospherically devoid of any material other than H. We compare the observed
abundances to predictions of radiative levitation calculations, revealing
little agreement. We propose that the supply of heavy elements is accreted from
external sources rather than being intrinsic to the star. These elements are
then retained in the white dwarf atmospheres by radiative levitation, a model
that can explain both the diversity of measured abundances for stars of similar
temperature and gravity, including cases with apparently pure H envelopes, and
the presence of photospheric metals at temperatures where radiative levitation
is no longer effective.Comment: 23 pages. 13 Figures, 4 Tables. Accepted for publication in the
Monthly Notices of the Royal Astronomical Societ
The status and future of EUV astronomy
The Extreme Ultraviolet wavelength range was one of the final windows to be
opened up to astronomy. Nevertheless, it provides very important diagnostic
tools for a range of astronomical objects, although the opacity of the
interstellar medium restricts the majority of observations to sources in our
own galaxy. This review gives a historical overview of EUV astronomy, describes
current instrumental capabilities and examines the prospects for future
facilities on small and medium-class satellite platforms.Comment: Published in Advances in Space Researc
Effective area calibration of the reflection grating spectrometers of XMM-Newton. II. X-ray spectroscopy of DA white dwarfs
White dwarf spectra have been widely used as a calibration source for X-ray
and EUV instruments. The in-flight effective area calibration of the reflection
grating spectrometers (RGS) of XMM-Newton depend upon the availability of
reliable calibration sources. We investigate how well these white dwarf spectra
can be used as standard candles at the lowest X-ray energies in order to gauge
the absolute effective area scale of X-ray instruments. We calculate a grid of
model atmospheres for Sirius B and HZ 43A, and adjust the parameters using
several constraints until the ratio of the spectra of both stars agrees with
the ratio as observed by the low energy transmission grating spectrometer
(LETGS) of Chandra. This ratio is independent of any errors in the effective
area of the LETGS. We find that we can constrain the absolute X-ray spectrum of
both stars with better than 5 % accuracy. The best-fit model for both stars is
close to a pure hydrogen atmosphere, and we put tight limits to the amount of
helium or the thickness of a hydrogen layer in both stars. Our upper limit to
the helium abundance in Sirius B is 4 times below the previous detection based
on EUVE data. We also find that our results are sensitive to the adopted
cut-off in the Lyman pseudo-continuum opacity in Sirius B. We get best
agreement with a long wavelength cut-off. White dwarf model atmospheres can be
used to derive the effective area of X-ray spectrometers in the lowest energy
band. An accuracy of 3-4 % in the absolute effective area can be achieved.Comment: 15 pages, 7 figures, accepted for publication in Astronomy &
Astrophysics, main journa
High ions towards white dwarfs: circumstellar line shifts and stellar temperature
Based on a compilation of OVI, CIV, SiIV and NV data from IUE, FUSE, GHRS,
STIS, and COS, we derive an anti- correlation between the stellar temperature
and the high ion velocity shift w.r.t. to the photosphere, with positive (resp.
negative) velocity shifts for the cooler (resp. hotter) white dwarfs. This
trend probably reflects more than a single process, however such a dependence
on the WD's temperature again favors a CS origin for a very large fraction of
those ion absorptions, previously observed with IUE, HST-STIS, HST-GHRS, FUSE,
and now COS, selecting objects for which absorption line radial velocities,
stellar effective temperature and photospheric velocity can be found in the
literature. Interestingly, and gas in near-equilibrium in the star vicinity. It
is also probably significant that the temperature that corresponds to a null
radial velocity, i.e. \simeq 50,000K, also corresponds to the threshold below
which there is a dichotomy between pure or heavy elements atmospheres as well
as some temperature estimates for and a form of balance between radiation
pressure and gravitation. This is consistent with ubiquitous evaporation of
orbiting dusty material. Together with the fact that the fraction of stars with
(red-or blue-) shifted lines and the fraction of stars known to possess heavy
species in their atmosphere are of the same order, such a velocity-temperature
relationship is consistent with quasi-continuous evaporation of orbiting CS
dusty material, followed by accretion and settling down in the photosphere. In
view of these results, ion measurements close to the photospheric or the IS
velocity should be interpreted with caution, especially for stars at
intermediate temperatures. While tracing CS gas, they may be erroneously
attributed to photospheric material or to the ISM, explaining the difficulty of
finding a coherent pattern of the high ions in the local IS 3D distribution.Comment: Accepted by A&A. Body of paper identical to v1. This submission has a
more appropriate truncation of the original abstrac
Do the constants of nature couple to strong gravitational fields?
Recently, white dwarf stars have found a new use in the fundamental physics
community. Many prospective theories of the fundamental interactions of Nature
allow traditional constants, like the fine structure constant , to vary
in some way. A study by Berengut et al. (2013) used the Fe/Ni V line
measurements made by Preval et al. (2013) from the hot DA white dwarf G191-B2B,
in an attempt to detect any variation in . It was found that the Fe V
lines indicated an increasing alpha, whereas the Ni V lines indicated a
decreasing alpha. Possible explanations for this could be misidentification of
the lines, inaccurate atomic data, or wavelength dependent distortion in the
spectrum. We examine the first two cases by using a high S/N reference spectrum
from the hot sdO BD+284211 to calibrate the Fe/Ni V atomic data. With
this new data, we re-evaluate the work of Berengut et al. (2013) to derive a
new constraint on the variation of alpha in a gravitational field.Comment: 4 pages, 2 figures: To appear in the proceedings of the "19th
European White Dwarf Workshop" in Montreal, Canada, 201
Comparison of stimulation patterns for FES-cycling using measures of oxygen cost and stimulation cost
<b>Aim</b><p></p>
The energy efficiency of FES-cycling in spinal cord injured subjects is very much lower than that of normal cycling, and efficiency is dependent upon the parameters of muscle stimulation. We investigated measures which can be used to evaluate the effect on cycling performance of changes in stimulation parameters, and which might therefore be used to optimise them. We aimed to determine whether oxygen cost and stimulation cost measurements are sensitive enough to allow discrimination between the efficacy of different activation ranges for stimulation of each muscle group during constant-power cycling. <p></p>
<b>Methods</b><p></p>
We employed a custom FES-cycling ergometer system, with accurate control of cadence and stimulated exercise workrate. Two sets of muscle activation angles (âstimulation patternsâ), denoted âP1â and âP2â, were applied repeatedly (eight times each) during constant-power cycling, in a repeated measures design with a single paraplegic subject. Pulmonary oxygen uptake was measured in real time and used to determine the oxygen cost of the exercise. A new measure of stimulation cost of the exercise is proposed, which represents the total rate of stimulation charge applied to the stimulated muscle groups during cycling. A number of energy-efficiency measures were also estimated. <p></p>
<b>Results</b><p></p>
Average oxygen cost and stimulation cost of P1 were found to be significantly lower than those for P2 (paired <i>t</i>-test, <i>p</i> < 0.05): oxygen costs were 0.56 ± 0.03 l min<sup>â1</sup> and 0.61 ± 0.04 l min<sup>â1</sup>(mean ± S.D.), respectively; stimulation costs were 74.91 ± 12.15 mC min<sup>â1</sup> and 100.30 ± 14.78 mC min<sup>â1</sup> (mean ± S.D.), respectively. Correspondingly, all efficiency estimates for P1 were greater than those for P2. <p></p>
<b>Conclusion</b><p></p>
Oxygen cost and stimulation cost measures both allow discrimination between the efficacy of different muscle activation patterns during constant-power FES-cycling. However, stimulation cost is more easily determined in real time, and responds more rapidly and with greatly improved signal-to-noise properties than the ventilatory oxygen uptake measurements required for estimation of oxygen cost. These measures may find utility in the adjustment of stimulation patterns for achievement of optimal cycling performance. <p></p>
A far-UV survey of three hot, metal-polluted white dwarf stars: WD0455-282, WD0621-376, and WD2211-495
Using newly obtained high-resolution data () from the
\textit{Hubble Space Telescope}, and archival UV data from the \textit{Far
Ultraviolet Spectroscopic Explorer} we have conducted a detailed UV survey of
the three hot, metal-polluted white dwarfs WD0455-282, WD0621-376, and
WD2211-495. Using bespoke model atmospheres we measured , log
, and photospheric abundances for these stars. In conjunction with data from
Gaia we measured masses, radii, and gravitational redshift velocities for our
sample of objects. We compared the measured photospheric abundances with those
predicted by radiative levitation theory, and found that the observed Si
abundances in all three white dwarfs, and the observed Fe abundances in
WD0621-376 and WD2211-495, were larger than those predicted by an order of
magnitude. These findings imply not only an external origin for the metals, but
also ongoing accretion, as the metals not supported by radiative levitation
would sink on extremely short timescales. We measured the radial velocities of
several absorption features along the line of sight to the three objects in our
sample, allowing us to determine the velocities of the photospheric and
interstellar components along the line of sight for each star. Interestingly,
we made detections of circumstellar absorption along the line of sight to
WD0455-282 with three velocity components. To our knowledge, this is the first
such detection of multi-component circumstellar absorption along the line of
sight to a white dwarf.Comment: 19 pages, 23 figures, 8 tables. Accepted for publication in the
Monthly Notices of the Royal Astronomical Societ
A comparison of DA white dwarf temperatures and gravities from FUSE Lyman line and ground-based Balmer line observations
Observation of the strengths and profiles of the hydrogen Balmer absorption
series is an established technique for determining the effective temperature
and surface gravity of hot H-rich white dwarf stars. In principle, the Lyman
series lines should be equally useful but, lying in the far-UV, are only
accessible from space. Nevertheless, there are situations (for example, where
the optical white dwarf spectrum is highly contaminated by the presence of a
companion) in which use of the Lyman series may be essential. Therefore, it is
important to establish whether or not the Lyman lines provide an equally valid
means of measurement. We have already made a first attempt to study this
problem, comparing Lyman line measurements from a variety of far-UV instruments
with ground-based Balmer line studies. Within the measurement uncertainties we
found the results from each line series to be broadly in agreement. However, we
noted a number of potential systematic effects that could bias either
measurement. With the availability of the FUSE data archive and observations
from our own Guest Observer programmes, we now have an opportunity of examining
the use of the Lyman series in more detail from observations of 16 DA white
dwarfs. The new results partially reproduce the earlier study, showing that
Balmer and Lyman line determined temperatures are in good agreement up to
\~50000K. However, above this value there is an increasing systematic
difference between the Lyman and Balmer line results, the former yielding the
higher temperature.Comment: Accepted for publication in the Monthly Notices of the Royal
Astronomical Society: 15 pages (inc 10 figures
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