1,904 research outputs found
Stellar laboratories III. New Ba V, Ba VI, and Ba VII oscillator strengths and the barium abundance in the hot white dwarfs G191-B2B and RE0503-289
For the spectral analysis of high-resolution and high-signal-to-noise (S/N)
spectra of hot stars, state-of-the-art non-local thermodynamic equilibrium
(NLTE) model atmospheres are mandatory. These are strongly dependent on the
reliability of the atomic data that is used for their calculation. Reliable Ba
V - VII oscillator strengths are used to identify Ba lines in the spectra of
the DA-type white dwarf G191-B2B and the DO-type white dwarf RE0503-289 and to
determine their photospheric Ba abundances. We newly calculated Ba V - VII
oscillator strengths to consider their radiative and collisional bound-bound
transitions in detail in our NLTE stellar-atmosphere models for the analysis of
Ba lines exhibited in high-resolution and high-S/N UV observations of G191-B2B
and RE0503-289. For the first time, we identified highly ionized Ba in the
spectra of hot white dwarfs. We detected Ba VI and Ba VII lines in the Far
Ultraviolet Spectroscopic Explorer (FUSE) spectrum of RE0503-289. The Ba VI /
Ba VII ionization equilibrium is well reproduced with the previously determined
effective temperature of 70000 K and surface gravity of . The Ba
abundance is (mass fraction, about 23000 times the
solar value). In the FUSE spectrum of G191-B2B, we identified the strongest Ba
VII line (at 993.41 \AA) only, and determined a Ba abundance of (about 265 times solar). Reliable measurements and calculations
of atomic data are a pre-requisite for stellar-atmosphere modeling. Observed Ba
VI - VII line profiles in two white dwarfs' (G191-B2B and RE0503-289)
far-ultraviolet spectra were well reproduced with our newly calculated
oscillator strengths. This allowed to determine the photospheric Ba abundance
of these two stars precisely.Comment: 36 pages, 8 figure
Stellar laboratories: new Ge V and Ge VI oscillator strengths and their validation in the hot white dwarf RE 0503-289
State-of-the-art spectral analysis of hot stars by means of non-LTE
model-atmosphere techniques has arrived at a high level of sophistication. The
analysis of high-resolution and high-S/N spectra, however, is strongly
restricted by the lack of reliable atomic data for highly ionized species from
intermediate-mass metals to trans-iron elements. Especially data for the latter
has only been sparsely calculated. Many of their lines are identified in
spectra of extremely hot, hydrogen-deficient post-AGB stars. A reliable
determination of their abundances establishes crucial constraints for AGB
nucleosynthesis simulations and, thus, for stellar evolutionary theory.
In a previous analysis of the UV spectrum of RE 0503-289, spectral lines of
highly ionized Ga, Ge, As, Se, Kr, Mo, Sn, Te, I, and Xe were identified.
Individual abundance determinations are hampered by the lack of reliable
oscillator strengths. Most of these identified lines stem from Ge V. In
addition, we identified Ge VI lines for the first time. We calculated Ge V and
Ge VI oscillator strengths to consider their radiative and collisional
bound-bound transitions in detail in our non-LTE stellar-atmosphere models for
the analysis of the Ge IV - VI spectrum exhibited in high-resolution and
high-S/N UV spectra of RE 0503-289. We identify four Ge IV, 37 Ge V, and seven
Ge VI lines. Most of these are identified for the first time in any star. We
reproduce almost all Ge IV, Ge VI, and Ge VI lines in the observed spectrum of
RE 0503-289 (Teff = 70 kK, log g = 7.5) at log Ge = -3.8 +/- 0.3 (mass
fraction, about 650 times solar).
Reliable measurements and calculations of atomic data are a prerequisite for
stellar-atmosphere modeling. Our oscillator-strength calculations have allowed,
for the first time, Ge V and Ge VI lines to be successfully reproduced in a
white dwarf's spectrum and to determine its photospheric Ge abundance.Comment: 54 pages, 8 figure
Complete spectral energy distribution of the hot, helium-rich white dwarf RX J0503.9-2854
In the line-of-sight toward the DO-type white dwarf RX J0503.9-2854, the
density of the interstellar medium (ISM) is very low, and thus the
contamination of the stellar spectrum almost negligible. This allows us to
identify many metal lines in a wide wavelength range from the extreme
ultraviolet to the near infrared. In previous spectral analyses, many metal
lines in the ultraviolet spectrum of RX J0503.9-2854 have been identified. A
complete line list of observed and identified lines is presented here. We
compared synthetic spectra that had been calculated from model atmospheres in
non-local thermodynamical equilibrium, with observations. In total, we
identified 1272 lines (279 of them were newly assigned) in the wavelength range
from the extreme ultraviolet to the near infrared. 287 lines remain
unidentified. A close inspection of the EUV shows that still no good fit to the
observed shape of the stellar continuum flux can be achieved although He, C, N,
O, Al, Si, P, S, Ca, Sc, Ti, V, Cr, Mn, Fe, Cr, Ni Zn, Ga, Ge, As, Kr, Zr, Mo,
Sn, Xe, and Ba are included in the stellar atmosphere models. There are two
possible reasons for the deviation between observed and synthetic flux in the
EUV. Opacities from hitherto unconsidered elements in the model-atmosphere
calculation may be missing and/or the effective temperature is slightly lower
than previously determined.Comment: 92 pages, 45 figure
Household decision-making about delivery in health facilities: evidence from Tanzania.
This study investigated how partners' perceptions of the healthcare system influence decisions about delivery-location in low-resource settings. A multistage population-representative sample was used in Kasulu district, Tanzania, to identify women who had given birth in the last five years and their partners. Of 826 couples in analysis, 506 (61.3%) of the women delivered in the home. In multivariate analysis, factors associated with delivery in a health facility were agreement of partners on the importance of delivering in a health facility and agreement that skills of doctors are better than those of traditional birth attendants. When partners disagreed, the opinion of the woman was more influential in determining delivery-location. Agreement of partners regarding perceptions about the healthcare system appeared to be an important driver of decisions about delivery-location. These findings suggest that both partners should be included in the decision-making process regarding delivery to raise rates of delivery at facility
Equity of Inpatient Health Care in Rural Tanzania:\ud A Population- and Facility-Based Survey
To explore the equity of utilization of inpatient health care at rural Tanzanian health centers through the use of a short wealth questionnaire.Methods: Patients admitted to four rural health centers in the Kigoma Region of Tanzania from May 2008 to May 2009 were surveyed about their illness, asset ownership and demographics. Principal component analysis was used to compare the wealth of the inpatients to the wealth of the region’s general population, using data from a previous population-based survey. Among inpatients, 15.3% were characterized as the most poor, 19.6% were characterized as very poor, 16.5% were characterized as poor, 18.9% were characterized as less poor, and 29.7% were characterized as the least poor. The wealth distribution of all inpatients (p < 0.0001), obstetric inpatients (p < 0.0001), other inpatients (p < 0.0001), and fee-exempt inpatients (p < 0.001) were significantly different than the wealth distribution in the community population, with poorer patients underrepresented among inpatients. The wealth distribution of pediatric inpatients (p = 0.2242) did not significantly differ from the population at large. The findings indicated that while current Tanzanian health financing policies may have improved access to health care for children under five, additional policies are needed to further close the equity gap, especially for obstetric inpatients.\u
Stellar laboratories. IX. New Se V, Sr IV - VII, Te VI, and I VI oscillator strengths and the Se, Sr, Te, and I abundances in the hot white dwarfs G191-B2B and RE 0503-289
To analyze spectra of hot stars, advanced non-local thermodynamic equilibrium
(NLTE) model-atmosphere techniques are mandatory. Reliable atomic data is for
the calculation of such model atmospheres.
We aim to calculate new Sr IV - VII oscillator strengths to identify for the
first time Sr spectral lines in hot white dwarf (WD) stars and to determine the
photospheric Sr abundances. o measure the abundances of Se, Te, and I in hot
WDs, we aim to compute new Se V, Te VI, and I VI oscillator strengths.
To consider radiative and collisional bound-bound transitions of Se V, Sr IV
- VII, Te VI, and I VI in our NLTE atmosphere models, we calculated oscillator
strengths for these ions.
We newly identified four Se V, 23 Sr V, 1 Te VI, and three I VI lines in the
ultraviolet (UV) spectrum of RE0503-289. We measured a photospheric Sr
abundance of 6.5 +3.8/-2.4 x 10**-4 (mass fraction, 9500 - 23800 times solar).
We determined the abundances of Se (1.6 +0.9/-0.6 x 10**-3, 8000 - 20000), Te
(2.5 +1.5/-0.9 x 10**-4, 11000 - 28000), and I (1.4 +0.8/-0.5 x 10**-5, 2700 -
6700). No Se, Sr, Te, and I line was found in the UV spectra of G191-B2B and we
could determine only upper abundance limits of approximately 100 times solar.
All identified Se V, Sr V, Te VI, and I VI lines in the UV spectrum of
RE0503-289 were simultaneously well reproduced with our newly calculated
oscillator strengths.Comment: 26 pages, 5 figure
Separatism in Belgium and Possible Variants of Its Development
Розглядається проблема сепаратизму в Бельгії. Аналізуються історичні моменти зародження конфлікту, сучасний стан, а також пропонуються можливі варіанти розвитку конфлікту.
Kruk A. P. Separatism in Belgium and Possible Variants of Its Development. We consider the problem of separatism in Belgium. Historical inception of the conflict, the current status is analyzed. Possible variants development of conflict is offered
Management of Critical Machine Settings for Accelerators at CERN
In high energy and high intensity accelerators as the LHC, the energy stored in the beams is orders of magnitude above the damage level of accelerator components like magnets. Uncontrolled release of this energy can lead to serious damage of equipment and long machine downtimes. In order to cope with these potential risks Protection Systems were developed at CERN including two software systems: MCS (Management of Critical Settings) and RBAC (Role Based Access Control). RBAC provides an authentication and authorization facility for access to the critical parts of the control system. A second layer of security is provided by MCS which ensures that critical parameters are coherent within the software and hardware components and can only be changed by an authorized person. The MCS system is aimed at the most critical parameters in either potentially dangerous equipment or protection devices (e.g. Beam Loss Monitors). It is complementary to the RBAC infrastructure. Both systems are fully integrated in the control system for the LHC and SPS and were successfully commissioned already before first beam in the LHC. This paper will describe the MCS architecture, current status and its operational deployment in the LHC
Stellar laboratories IV. New Ga IV, Ga V, and Ga VI oscillator strengths and the gallium abundance in the hot white dwarfs G191-B2B and RE0503-289
For the spectral analysis of high-resolution and high-signal-to-noise (S/N)
spectra of hot stars, advanced non-local thermodynamic equilibrium (NLTE) model
atmospheres are mandatory. These atmospheres are strongly dependent on the
reliability of the atomic data that are used to calculate them. Reliable Ga IV
- VI oscillator strengths are used to identify Ga lines in the spectra of the
DA-type white dwarf G191-B2B and the DO-type white dwarf RE0503-289 and to
determine their photospheric Ga abundances. We newly calculated Ga IV - VI
oscillator strengths to consider their radiative and collisional bound-bound
transitions in detail in our NLTE stellar-atmosphere models for analyzing of Ga
lines exhibited in high-resolution and high-S/N UV observations of G191-B2B and
RE0503-289. We unambiguously detected 20 isolated and 6 blended (with lines of
other species) Ga V lines in the Far Ultraviolet Spectroscopic Explorer (FUSE)
spectrum of RE0503-289. The identification of Ga IV and Ga VI lines is
uncertain because they are weak and partly blended by other lines. The
determined Ga abundance is 3.5 +/- 0.5 x 10**-5 (mass fraction, about 625 times
solar). The Ga IV / GA V ionization equilibrium, which is a very sensitive
indicator for the effective temperature, is well reproduced in RE0503-289. We
identified the strongest Ga IV lines (1258.801, 1338.129 A) in the HST/STIS
(Hubble Space Telescope / Space Telescope Imaging Spectrograph) spectrum of
G191-B2B and measured a Ga abundance of 2.0 +/- 0.5 x 10**-6 (about 22 times
solar). Reliable measurements and calculations of atomic data are a
prerequisite for stellar-atmosphere modeling. Observed Ga IV - V line profiles
in two white dwarf (G191-B2B and RE0503-289) ultraviolet spectra were well
reproduced with our newly calculated oscillator strengths. For the first time,
this allowed us to determine the photospheric Ga abundance in white dwarfs.Comment: 127 pages, 6 figure
- …