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1.
We have started a program of high-resolution (0.4MIDDLE" BORDER="0">/pixel) 10MIDDLE" BORDER="0">m imaging of bipolar outflow sources using the 10MIDDLE" BORDER="0">m camera CAMIRAS. We present recent results obtained at the Canada France Hawaii Telescope which reveal extended emission or IR companions in several luminous objects. The extended emission we detected probably arises from transiently heated very small grains, while the newly discovered companions could contribute significantly to the outflow activity and extended far-IR emission usually attributed to the main optical source. 相似文献
2.
We have used the ESO 10 MIDDLE" BORDER="0">m camera, TIMMI, to image with a very high angular resolution (PFoV: 0.3MIDDLE" BORDER="0">; FWHM:0.9MIDDLE" BORDER="0">) several main-sequence star disk candidates. Information on the MIDDLE" BORDER="0">-Pictoris dust disk has been obtained in a region largely inaccessible to previous observations: 0–80 AU, with a resolution of about 5 AU after deconvolution. Another promising target for 10 MIDDLE" BORDER="0">m imaging, 51 Ophiuchi, appears point-like.based on data collected at the European Southern Observatory (ESO), La Silla, Chile 相似文献
3.
Ph. Stee 《Astrophysics and Space Science》1995,224(1-2):561-562
I present theoretical line profiles and intensity maps from an axi-symmetric radiative wind model from a rapidly rotating Be star. The introduction of a viscosity parameter in the latitude-dependent hydrodynamic code enables us to consider the effects of the viscous force in the azimuthal component of momentum equations (Araújo et al. 1994). Both velocity field and density law derived from the hydrodynamic equations have been used for solving the statistical equilibrium equations. By adopting the Sobolev approximation, we could easily obtain a good estimate of both electronic density and hydrogen level populations throughout the envelope. The numerical calculation was performed for parameters characterisic of the Be starMIDDLE" BORDER="0"> Cassiopeiae. 相似文献
4.
Further Studies Of Atmospheric Turbulence In Layers Near The Surface: Scaling The Tke Budget Above The Roughness Sublayer 总被引：2，自引：0，他引：2
The second of two experimental studies of the TKE budget conducted on sites of different roughness is described, and results are compared. The first took place within a shallow layer above a small field of mostly bare, cultivated soil; the second was carried out above a roughness sublayer of significant depth on an extensive plain of tall dry grass. Budget terms observed in the second study were scaled with a modified uMIDDLE" BORDER="0"> which compensated for effects of an unusually large stress gradient and ensured that the MIDDLE" BORDER="0">m functions would be collinear. By showing that the modification becomes negligible in smaller gradients, it is demonstrated that in normal conditions, budgets observed above significant roughness sublayers should be normalized by scaling in terms of the unreduced Reynolds stress at the sublayer's upper surface. This procedure is shown to be consistent with the expectation that TKE budgets in layers near the surface all scale in fundamentally the same way.Other findings include: (1) the fact that most MIDDLE" BORDER="0">m functions previously reported are not quite collinear is attributed to a type of overspeeding known to affect three-cup anemometers; (2) revised MIDDLE" BORDER="0">m functions, collinear and largely free of the effects of overspeeding, are determined from a well-established characteristic of the linear MIDDLE" BORDER="0">m relation for the stable case; (3) data that define collinear MIDDLE" BORDER="0">m functions can also be represented with single hyperbolic curves; (4) dissipation is found to be 10 to 15% too small to balance total TKE production in unstable and neutral conditions and to decrease with increasing z/L in thestable regime; and (5) new relations for MIDDLE" BORDER="0">MIDDLE" BORDER="0"> based on the observed behaviour of the dissipation deficit provide an improved closure for the set of equations that express the budget terms as functions of MIDDLE" BORDER="0">m and z/L. 相似文献
5.
A condition is derived for consistency of the standardMIDDLE" BORDER="0">-equation with Monin–Obukhov (MO) similarity theory of thestably-stratified surface layer. The condition is derivedby extending the procedure used to derive the analogous condition forneutral theory to stable stratification. It is shown that consistencywith MO theory requires a function of flux Richardson number, Rif, to be absorbed into either of two closure parameters, cMIDDLE" BORDER="0"> 1 or cMIDDLE" BORDER="0"> 2.Inconsistency, on the other hand, results if constant values of these are maintained for all Rif, as is done in standardapplication of the equation, and the large overpredictions ofturbulence found in such application to the one-dimensionalstable atmospheric boundary layer (1D-SBL) are traced to thisinconsistency. Guided by this, we formulate a MO-consistentMIDDLE" BORDER="0">-equation by absorbing the aforementioned function intocMIDDLE" BORDER="0"> 1, and combine this with a Level-2.5 second-orderclosure model for vertical eddy viscosity and diffusivities.Numerical predictions of the 1D-SBL by the modified model converge to a quasi-steady state, rectifying the predictive failure of the standardMIDDLE" BORDER="0"> -equation for the case.Quasi-steady predictions of non-dimensional variables agree stronglywith Nieuwstadt's theory. Qualitative accuracy of predictionsis inferred from comparisons to field data, large-eddy simulationresults and Rossby-number similarity relationships. 相似文献
6.
T.C. Teixeira J. Christensen-Dalsgaard F. Carrier C. Aerts S. Frandsen D. Stello T. Maas M. Burnet H. Bruntt J.R. de Medeiros F. Bouchy H. Kjeldsen F. Pijpers 《Astrophysics and Space Science》2003,284(1):233-236
This work reports the discovery of solar-type oscillations in thegiant star MIDDLE" BORDER="0"> Hydrae. 相似文献
7.
Present Observational Status of the Intermediate Mass Stars: δ Sct Stars, γ Dor Stars and roAp Stars
D.W. Kurtz 《Astrophysics and Space Science》2003,284(1):29-36
The present observational status of the Sct stars, MIDDLE" BORDER="0"> Dor stars and roAp stars is discussed. The Sct stars are the most intensively observed of the three groups, but it has become clear that there are severe problems in extracting asteroseismic information from them. Dozens of frequencies are observed, but hundreds of frequencies are predicted from the models; unique matches of observation and theory still elude us. The Sct stars are observationally complex – some recent `best case' campaigns are discussed. It is possible that substantial observational advances for Sct stars may need to await upcoming satellite missions. New MIDDLE" BORDER="0"> Dor stars are beingdiscovered frequently, and new behaviour is being found for them. They constitutean observationally young field. Their pulsational frequency range is being expanded, their position in the HR diagram is becoming better known (but is yet to be fully constrained), and the possibility exists of hybrid MIDDLE" BORDER="0"> Dor – Sct stars that have greatasteroseismic promise, although it is clear such stars are rare, if they do exist. It has been observationally challenging to extract more than a fewfrequencies for any MIDDLE" BORDER="0"> Dor star so far. Exciting spectroscopic discoveries of new behaviour in roAp stars promise unprecedented information about the structure of the peculiar atmospheres ofthose stars – pulsation amplitude and phase in 3D, magnetic field structurein 3D, abundance stratification in 3D, realistic T- for the most peculiarstars – as well as entirely new information about the interaction of pulsation,rotation and magnetic fields. Recent theoretical work has led to new understandingof the previously inexplicable frequency spacing of HR 1217 with new Whole Earth Telescope observations supporting this theory. An `improved oblique pulsator model' has been developed in which the pulsationaxis is not the magnetic axis; this model has passed several observationaltests and new ones are being devised to examine it further. 相似文献
8.
Ramon D. Wolstencroft S. M. Scarrott T. M. Gledhill 《Astrophysics and Space Science》1995,224(1-2):395-398
The asymmetries in the brightness structure and levels of polarization between the two sides of theMIDDLE" BORDER="0"> Pic disc are discussed. The possibility of these differences being caused by a planet, or planets, within the circumstellar disc is investigated. 相似文献
9.
The large Area Detectors (LADs) of the BATSE experiment aboard the Compton Gamma-ray Observatory have been used recently as the first hard X-ray all-sky imager at energies between 20 keV and 300 keV. The Earth occultation process is formulated in terms of a curved Radon transform convoluted by a step transform in a selected field of view (FOV) ranging from 5°×5° to 40°×40°. The Maximum Entropy Method is then used to reconstruct an image in the hard X-ray sky. Multiple images of different regions of the sky can be produced simultaneously. A source location accuracy of 0.1° for strong sources and a sensitivity limit of 100 mCrab have been achieved in an one-day integration period.Invited Paper on MIDDLE" BORDER="0">Imaging in High Energy AstronomyMIDDLE" BORDER="0">, Sept., 1994, Capri, Italyalso Universities Space Research Association 相似文献
10.
Following the discovery, by IRAS, of the dust disc around Vega and three other main sequence stars, searches have been made for other candidates. TheMIDDLE" BORDER="0">-Pic-like candidates have 12µm excesses and 100µm fluxes (unlike the Vega-like candidates), so they can be further investigated using ground-based techniques. Data are presented here, comprising 10µm spectroscopy and sub-mm observations, for several candidates from the Walker & Wolstencroft list, showing that the stars have silicate dust, and optically thick dust discs even at 1300µm. 相似文献