87 resultados para Variations (Organ)
Resumo:
Spectroscopic observations of 51 Pegasi and tau Bootis show no periodic changes in the shapes of their line profiles; these results for 51 Peg are in significant conflict with those reported by Gray & Hatzes. Our detection limits are small enough to rule out nonradial pulsations as the cause of the variability in tau Boo, but not in 51 Peg. The absence of line shape changes is consistent with these stars' radial velocity variability arising from planetary mass companions.
Resumo:
The stars 51 Pegasi and tau Bootis show radial velocity variations that have been interpreted as resulting from companions with roughly Jovian mass and orbital periods of a few days. Gray and Gray & Hatzes reported that the radial velocity signal of 51 Peg is synchronous with variations in the shape of the line lambda 6253 Fe I; thus, they argue that the velocity signal arises not from a companion of planetary mass but from dynamic processes in the atmosphere of the star, possibly nonradial pulsations. Here we seek confirming evidence for line shape or strength variations in both 51 Peg and tau Boo, using R = 50,000 observations taken with the Advanced Fiber Optic Echelle. Because of our relatively low spectral resolution, we compare our observations with Gray's line bisector data by fitting observed line profiles to an expansion in terms of orthogonal (Hermite) functions. To obtain an accurate comparison, we model the emergent line profiles from rotating and pulsating stars, taking the instrumental point-spread function into account. We describe this modeling process in detail. We find no evidence for line profile or strength variations at the radial velocity period in either 51 Peg or in tau Boo. For 51 Peg, our upper limit for line shape variations with 4.23 day periodicity is small enough to exclude with 10 sigma confidence the bisector curvature signal reported by Gray & Hatzes; the bisector span and relative line depth signals reported by Gray are also not seen, but in this case with marginal (2 sigma ) confidence. We cannot, however, exclude pulsations as the source of 51 Peg's radial velocity variation because our models imply that line shape variations associated with pulsations should be much smaller than those computed by Gray & Hatzes; these smaller signals are below the detection limits both for Gray & Hatzes's data and for our own. tau Boo's large radial velocity amplitude and v sin i make it easier to test for pulsations in this star. Again we find no evidence for periodic line shape changes, at a level that rules out pulsations as the source of the radial velocity variability. We conclude that the planet hypothesis remains the most likely explanation for the existing data.
Resumo:
Organ donation plays a major role in the management of patients with single organ failure of the kidneys, liver, pancreas, heart, or lung, or with combined organ failure of heart and lung (such as in cystic fibrosis) or of kidney and pancreas (such as in diabetes). A shortage of transplant organs has resulted in long waits for transplantation. Currently about 500 people in the United Kingdom die each year because of a shortage of donated organs,1 and at 31 March 2011 almost 7000 patients were waiting for a kidney transplant1 and would be having costly dialysis with serious morbidity and impact on quality of life. This shortage of organs is partly the result of relatively low numbers of road traffic deaths (lower than in many countries) but is also the result of inefficiencies in the donor identification and consent processes. This article summarises the most recent recommendations from the National Institute for Health and Clinical Excellence (NICE) on improving donor identification and consent rates for deceased organ donation.2
Resumo:
Musical Score. Commissioned by Pauline Kim Harris. A virtuosic set of variations on the famous Talking Heads song for solo violin.
