2,179 research outputs found
Statistical Uncertainties in Temperature Diagnostics for Hot Coronal Plasma Using the ASCA SIS
Statistical uncertainties in determining the temperatures of hot (0.5 keV to
10 keV) coronal plasmas are investigated. The statistical precision of various
spectral temperature diagnostics is established by analyzing synthetic ASCA
Solid-state Imaging Spectrometer (SIS) CCD spectra. The diagnostics considered
are the ratio of hydrogen-like to helium-like line complexes of
elements, line-free portions of the continuum, and the entire spectrum. While
fits to the entire spectrum yield the highest statistical precision, it is
argued that fits to the line-free continuum are less susceptible to atomic data
uncertainties but lead to a modest increase in statistical uncertainty over
full spectral fits. Temperatures deduced from line ratios can have similar
accuracy but only over a narrow range of temperatures. Convenient estimates of
statistical accuracies for the various temperature diagnostics are provided
which may be used in planning ASCA SIS observations.Comment: postscript file of 8 pages+3 figures; 4 files tarred, compressed and
uuencoded. To appear in the Astrophysical Journal Letters; contents copyright
1994 American Astronomical Societ
Driver vs. manager perceptions of commonly used safety practices in commercial motor vehicle operations
This research investigated the perceptions of Commercial Motor Vehicle Operators and Safety Professionals regarding 35 commonly implemented practices used to improve operating safety. Several differences were found in how drivers of different backgrounds rated various practices, and between the drivers and safety managers. These differences were found to be persistent even when combined with measures of safety performance and experience. Managers tended to overvalue (relative to drivers) practices related to hiring, while drivers tended to overvalue (relative to managers) practices related to company support and reward systems. Motor Carriers, insurers, and regulators could consider areas of agreement with respect to high value practices as actionable for increased investment of resources. At the same time, resources allocated toward areas of low perceived value could be reduced
Safety attitudes and behavioral intentions of municipal waste disposal drivers
The Theory of Planned Behavior was used to study factors useful for predicting Behavioral Intentions to commit unsafe acts while driving for commercial drivers working for municipal waste management operations centers. The Theory of Planned Behavior was found to be moderately effective in predicting behavioral intentions, particularly through the constructs of Attitude and Perceived Control. Driver perceptions of safety climate, self-assessed personal safety performance, risk aversion, and attitudes toward behavioral factors associated with engaging in risky behaviors while operating motor vehicles were studied. Risk aversion and driver perception of their own safety performance were also useful predictors of intention
Chandra Contaminant Migration Model
High volatility cleans OBFs and low volatility produces a high build-up at OBF centers; only a narrow (factor of 2 or less) volatility range produces the observed spatial pattern. Simulations predict less accumulation above outer S-array CCDs; this may explain, in part, gratings/imaging C/MnL discrepancies. Simulations produce a change in center accumulation due solely to DH heater ON/OFF temperature change; but a 2nd contaminant and perhaps a change in source rate is also required. Emissivity E may depend on thickness; another model parameter. Additional physics, e.g., surface migration, is not warranted at this time. At t approx. 14 yrs, model produced 0.22 grams of contaminant, 0.085 grams remaining within ACIS cavity; 7 percent (6mg) on OBFs
On the Short-Period Eclipsing High-Mass X-ray Binary in NGC 4214
We present the results of our study of the luminous (L_{X} ~ 10^{39} erg/s)
X-ray binary CXOU J121538.2+361921 in NGC 4214, the high mass X-ray binary with
the shortest known orbital period. Using Chandra data, we confirm the ~13,000 s
(3.6 hr) eclipse period, and an eclipse duration of ~2000 s. From this, we
estimate a mass ratio M_2/M_1 >~ 3 and a stellar density of about 6 g cm^{-3},
which implies that the donor must be a Wolf-Rayet or a stripped Helium star.
The eclipse egress is consistently much slower than the ingress. This can be
explained by denser gas located either in front of the compact object (as
expected for a bow shock) or trailing the donor star (as expected for a shadow
wind, launched from the shaded side of the donor). There is no change in X-ray
spectral shape with changing flux during the egress, which suggests either
variable partial covering of the X-ray source by opaque clumps or, more likely,
a grey opacity dominated by electron scattering in a highly ionized medium. We
identify the optical counterpart from Hubble images. Photometry blueward of
~5500 Ang indicates a bright (M_{B} = -3.6 +/- 0.3 mag, for a range of
plausible extinctions), hot (T = 90,000 +/- 30,000 K) emitter, consistent with
the Wolf-Rayet scenario. There is also a bright (M_{I} ~ -5.2 mag), cool (T =
2700 +/- 300 K) component consistent with an irradiated circumbinary disk or
with a chance projection of an unrelated asymptotic giant branch star along the
same line of sight.Comment: 20 pages, 4 MB, accepted for publication in Ap
Discovery of a 3.6-hr Eclipsing Luminous X-Ray Binary in the Galaxy NGC 4214
We report the discovery of an eclipsing X-ray binary with a 3.62-hr period
within 24" of the center of the dwarf starburst galaxy NGC 4214. The orbital
period places interesting constraints on the nature of the binary, and allows
for a few very different interpretations. The most likely possibility is that
the source lies within NGC 4214 and has an X-ray luminosity of up to 7 e38
ergs/s. In this case the binary may well be comprised of a naked He-burning
donor star with a neutron-star accretor, though a stellar-mass black-hole
accretor cannot be completely excluded. There is no obvious evidence for a
strong stellar wind in the X-ray orbital light curve that would be expected
from a massive He star; thus, the mass of the He star should be <3-4 solar
masses. If correct, this would represent a new class of very luminous X-ray
binary -- perhaps related to Cyg X-3. Other less likely possibilities include a
conventional low-mass X-ray binary that somehow manages to produce such a high
X-ray luminosity and is apparently persistent over an interval of years; or a
foreground AM Her binary of much lower luminosity that fortuitously lies in the
direction of NGC 4214. Any model for this system must accommodate the lack of
an optical counterpart down to a limiting magnitude of 22.6 in the visible.Comment: 7 pages, ApJ accepted versio
Lynx X-Ray Observatory: Response to the First Astro 2020 Decadal Survey Request for Information
This document serves as the Lynx Teams response to the first Request For Information (RFI) from the 2020 Decadal Survey in Astronomy and Astrophysics. Detailed answers to all of the questions asked in this RFI can be found in the Lynx Concept Study Report, Supplementary Technology Roadmaps, and the Lynx Cost Book
Implications of the Observed Ultraluminous X-Ray Source Luminosity Function
We present the X-ray luminosity function (XLF) of ultraluminous X-ray (ULX) sources with 0.3-10.0 keV luminosities in excess of 10(sup 39) erg/s in a complete sample of nearby galaxies. The XLF shows a break or cut-off at high luminosities that deviates from its pure power law distribution at lower luminosities. The cut-off is at roughly the Eddington luminosity for a 90-140 solar mass accretor. We examine the effects on the observed XLF of sample biases, of small-number statistics (at the high luminosity end) and of measurement uncertainties. We consider the physical implications of the shape and normalization of the XLF. The XLF is also compared and contrasted to results of other recent surveys
Ultraluminous X-ray Source Correlations with Star-Forming Regions
Maps of low-inclination nearby galaxies in Sloan Digitized Sky Survey u-g,
g-r and r-i colors are used to determine whether Ultraluminous X-ray sources
(ULXs) are predominantly associated with star-forming regions of their host
galaxies. An empirical selection criterion is derived from colors of HII
regions in M81 and M101 that differentiates between the young, blue stellar
component and the older disk and bulge population. This criterion is applied to
a sample of 58 galaxies of Hubble type S0 and later and verified through an
application of Fisher's linear discriminant analysis. It is found that 60%
(49%) of ULXs in optically-bright environments are within regions blueward of
their host galaxy's HII regions compared to only 27% (0%) of a control sample
according to the empirical (Fisher) criterion. This is an excess of 3-sigma
above the 32% (27%) expected if the ULXs were randomly distributed within their
galactic hosts. This indicates a ULX preference for young, approximately <10
Myr, OB associations. However, none of the ULX environments have the morphology
and optical brightness suggestive of a massive young super star cluster though
several are in extended or crowded star-forming (blue) environments that may
contain clusters unresolved by Sloan imaging. Ten of the 12 ULX candidates with
estimated X-ray luminosities in excess of 3e39 erg/s are equally divided among
the group of ULX environments redward of HII regions and the group of optically
faint regions. This likely indicates that the brightest ULXs turn on at a time
somewhat later than typical of HII regions; say 10-20 Myr after star formation
has ended. This would be consistent with the onset of an accretion phase as the
donor star ascends the giant branch if the donor is a <20 solar-mass star.Comment: 13 pages, accepted to Ap
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