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1.
The process of Differential Roughness Secondary Flow (DRSF), hitherto little recognized, recently was demonstrated in a wind
tunnel and in a flume. It is suggested here the DRSF may, in the natural environment, play an important part in the persistence
and sharp definition of sand ribbons, previously initiated by other processes.
In 1980 Karl described a series of sand ribbons, alternating with exposed substrate, which he attributed to the effect of
Langmuir circulations. Although Langmuir Circulation Secondary Flow (LCSF) may indeed, in some cases, initiate sand ribbons,
the sharply-defined edges typical of these features are explained better by DRSF. 相似文献
2.
We have started a program of high-resolution (0.4/pixel) 10m imaging of bipolar outflow sources using the 10m 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
3.
We have used the ESO 10 m camera, TIMMI, to image with a very high angular resolution (PFoV: 0.3; FWHM:0.9) several main-sequence star disk candidates. Information on the -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 m imaging, 51 Ophiuchi, appears point-like.based on data collected at the European Southern Observatory (ESO), La Silla, Chile 相似文献
4.
Anthony Boccaletti Jean Schneider Wes Traub Pierre-Olivier Lagage Daphne Stam Raffaele Gratton John Trauger Kerri Cahoy Frans Snik Pierre Baudoz Raphael Galicher Jean-Michel Reess Dimitri Mawet Jean-Charles Augereau Jenny Patience Marc Kuchner Mark Wyatt Eric Pantin Anne-Lise Maire Christophe Vérinaud Samuel Ronayette Didier Dubreuil Michiel Min Michiel Rodenhuis Dino Mesa Russ Belikov Olivier Guyon Motohide Tamura Naoshi Murakami Ingrid Mary Beerer 《Experimental Astronomy》2012,34(2):355-384
SPICES (Spectro-Polarimetric Imaging and Characterization of Exoplanetary Systems) is a five-year M-class mission proposed to ESA Cosmic Vision. Its purpose is to image and characterize long-period extrasolar planets and circumstellar disks in the visible (450?C900 nm) at a spectral resolution of about 40 using both spectroscopy and polarimetry. By 2020/2022, present and near-term instruments will have found several tens of planets that SPICES will be able to observe and study in detail. Equipped with a 1.5 m telescope, SPICES can preferentially access exoplanets located at several AUs (0.5?C10?AU) from nearby stars (<25 pc) with masses ranging from a few Jupiter masses to Super Earths (??2 Earth radii, ??10 M??) as well as circumstellar disks as faint as a few times the zodiacal light in the Solar System. 相似文献
5.
Gas bubbles rising to the sea surface and unusual scattering zones on echo‐sounding records provide evidence for areas of submarine geothermal activity near Whale Island and White Island. 相似文献
6.
H. M. Pantin 《新西兰海洋与淡水研究杂志》2013,47(2):118-138
The term “diamicton” has recently been proposed as a non‐genetic name for any non‐calcareous terrigenous sediment containing a wide variety of grain sizes; the lithified equivalent is a “diamictite.” The present paper deals with the origin and classification of water‐borne diamictons. The latter have been divided by the writer into three groups: Group I. Diamictons with the coarse and fine fractions deposited simultaneously. Group II. Diamictons with the coarse and fine fractions deposited separately. Group III. Diamictons with the fine fraction derived from the coarse fraction by diagenetic alteration in place. Group I diamictons have been divided into the following types: (i) P‐diamictons, in which the fine fraction was deposited from true suspension (the coarser material being transported by suspension, saltation, or traction), (ii) M—diamictons, in which the fine (and coarse) fractions were deposited from mudflows. (iii) K‐diamictons, in which the fine fractions were deposited in the form of discrete sand‐size or pebble‐size fragments composed of lutite. Group II diamictons have been divided into the following types: (i) S‐diamictons, consisting of coarse and fine layers mixed by gravity, (ii) B‐diamictons, consisting of coarse and fine layers mixed by bioturbation. Group III diamictons, which have not been subdivided, are called D‐diamictons. P‐, M‐, and S‐diamictons have been further subdivided, and the different varieties are discussed The scheme of classification and selected examples of diamictons and diamictites are given in appropriate tables. 相似文献
7.
S. Wolf F. Malbet R. Alexander J.-P. Berger M. Creech-Eakman G. Duchêne A. Dutrey C. Mordasini E. Pantin F. Pont J.-U. Pott E. Tatulli L. Testi 《Astronomy and Astrophysics Review》2012,20(1):1-83
We present a review of the interplay between the evolution of circumstellar disks and the formation of planets, both from the perspective of theoretical models and dedicated observations. Based on this, we identify and discuss fundamental questions concerning the formation and evolution of circumstellar disks and planets which can be addressed in the near future with optical and infrared long-baseline interferometers. Furthermore, the importance of complementary observations with long-baseline (sub)millimeter interferometers and high-sensitivity infrared observations is outlined. 相似文献
8.
H. M. Pantin 《地球表面变化过程与地形》1982,7(5):503-505
The experiments of Southard and Mackintosh prove only that autosuspension did not occur under the tested conditions; these were based on the Bagnold (1963) criterion, which is unsound. An alternative criterion is re-emphasized, and a method for testing its validity suggested. Two separate derivations are given for the power required for sediment suspension. 相似文献
9.
Galdemard P. Lagage P. O. Dubreuil D. Jouan R. Masse P. Pantin E. Bockelée-Morvan D. 《Earth, Moon, and Planets》1997,78(1-3):271-277
Comet C/1995 O1 (Hale-Bopp) was observed with camiras, the Saclay mid-infrared camera, mounted on the Nordic Optical Telescope
(Roque de los Muchachos, La Palma), from April 14th to April 25th, 1997. This observing run was part of the European campaign
devoted to Hale-Bopp observations from the Canary Islands (PI R. West). camiras spectro-imaging capabilities, achieved with
a Circular Variable Filter (of spectral resolution R ≈ 50), were used to obtain spectra of the comet in the N atmospheric
window (8–13 μm) over a large field of view (52″ × 78″), at a spatial resolution of ∼1 arcsec. Data were also collected at
shorter wavelengths (in the L and M bands). The silicate dust feature around 10 μm is clearly apparent in the data. The shape
of the feature varies continuously according to the position in the field. A dust model developed at Saclay in the framework
of β-Pictoris dust disk studies was used to interpret the observations. The presence of both olivine and pyroxene with a high
degree of crystallinity is needed to account for the observations. A change in the size distribution of the grains allows
to reproduce the spatial change of the silicate feature according to the position in the field.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
10.
N. Hulamo H. Bouy M. Sterzik E. Pantin E.L. MartÍn 《Astronomische Nachrichten》2005,326(10):1022-1023
We present mid‐IR observations of a sample of very low‐mass stars and brown dwarfs in the Upper Scorpius association. The main goal of these observations is to derive the disk frequency and the disk properties of the sample in order to shed light on brown dwarf formation theories. The observations have been performed with VISIR at the Very Large Telescope (VLT, Paranal). A total of ten targets were observed and six were detected. In this paper we show preliminary results for two of them: DENIS‐PJ160334 and DENIS‐PJ161939. While the former shows mid‐IR fluxes consistent with pure photospheric emission, the latter displays strong mid‐IR excesses which are probably related with a circumstellar disk. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献