| 1. |
- Barbato, A, et al.
(författare)
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Primary ciliary dyskinesia: a consensus statement on diagnostic and treatment approaches in children.
- 2009
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Ingår i: The European respiratory journal : official journal of the European Society for Clinical Respiratory Physiology. - : European Respiratory Society (ERS). - 0903-1936. ; 34:6, s. 1264-76
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Tidskriftsartikel (refereegranskat)abstract
- Primary ciliary dyskinesia (PCD) is associated with abnormal ciliary structure and function, which results in retention of mucus and bacteria in the respiratory tract, leading to chronic oto-sino-pulmonary disease, situs abnormalities and abnormal sperm motility. The diagnosis of PCD requires the presence of the characteristic clinical phenotype and either specific ultrastructural ciliary defects identified by transmission electron microscopy or evidence of abnormal ciliary function. Although the management of children affected with PCD remains uncertain and evidence is limited, it remains important to follow-up these patients with an adequate and shared care system in order to prevent future lung damage. This European Respiratory Society consensus statement on the management of children with PCD formulates recommendations regarding diagnostic and therapeutic approaches in order to permit a more accurate approach in these patients. Large well-designed randomised controlled trials, with clear description of patients, are required in order to improve these recommendations on diagnostic and treatment approaches in this disease.
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| 2. |
- Jorissen, A, et al.
(författare)
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On metal-deficient barium stars and their link with yellow symbiotic stars
- 2005
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Ingår i: Astronomy & Astrophysics. - 0004-6361. ; 441:3, s. 83-1135
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Tidskriftsartikel (refereegranskat)abstract
- This paper addresses the question of why metal- deficient barium stars are not yellow symbiotic stars ( YSyS). Samples of ( suspected) metal-deficient barium ( mdBa) stars and YSyS have been collected from the literature, and their properties reviewed. It appears in particular that the barium nature of the suspected mdBa stars needs to be ascertained by detailed abundance analyses. Abundances are therefore derived for two of them, HD 139409 and HD 148897, which reveal that HD 148897 should not be considered a barium star. HD 139409 is a mild barium star, with overabundances observed only for elements belonging to the first s- process peak ( Y and Zr). It is only moderately metal- poor ([ Fe/ H] = - 0.4). The evidence for binarity among mdBa stars is then reviewed, using three different methods: ( i) radial- velocity variations ( from CORAVEL observations), ( ii) Hipparcos astrometric data, and ( iii) a method based on the comparison between the Hipparcos and Tycho- 2 proper motions. An orbit is obtained for HIP 55852, whereas evidence for the ( so far unknown) binary nature of HIP 34795, HIP 76605, HIP 97874 and HIP 107478 is presented. No conclusion regarding the binary nature of HIP 11595, HIP 25161 could be reached. Two stars with no evidence for binarity whatsoever ( HIP 58596 and BD + 3. 2688) are candidates low- metallicity thermally- pulsing asymptotic giant branch stars, as inferred from their large luminosities. The reason why mdBa stars are not YSyS is suggested to lie in their different orbital period distributions: mdBa stars have on average longer orbital periods than YSyS, and hence their companion accretes matter at a lower rate, for a given mass loss rate of the giant star. The definite validation of this explanation should nevertheless await the determination of the orbital periods for the many mdBa stars still lacking periods, in order to make the comparison more significant.
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| 3. |
- Quinet, P, et al.
(författare)
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Transition probabilities and lifetimes in neutral and singly ionized osmium and the Solar osmium abundance
- 2006
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Ingår i: Astronomy & Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 448:3, s. 93-1207
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Tidskriftsartikel (refereegranskat)abstract
- Radiative lifetime measurements have been performed, with a time-resolved laser-induced fluorescence technique, for 12 levels of Os I and for 9 levels of Os II. For 9 levels of Os I and 4 levels of Os II, there were no previous experimental data available. From a comparison with new theoretical calculations, taking configuration interactions and core-polarization effects into account, it has been possible to deduce oscillator strengths for 129 transitions of Os I and 137 transitions of Os II of astrophysical interest appearing in the wavelength range 180.0-870.0 nm. These results have allowed us to revise the abundance of osmium in the solar photosphere (log epsilon(Os) = 1.25 +/- 0.11). The newly derived oscillator strengths have been applied as well to derive the osmium abundance in the carbon-rich metal-poor star HD 187861.
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