WASP-14b: 7.3 M_J transiting planet in an eccentric orbit     

Y. C. Joshi  D. Pollacco  A. Collier Cameron  I. Skillen  E. Simpson  I. Steele  R. A. Street  H. C. Stempels  D. J. Christian  L. Hebb  F. Bouchy  N. P. Gibson  G. Hébrard  F. P. Keenan  B. Loeillet  J. Meaburn  C. Moutou  B. Smalley  I. Todd  R. G. West  D. R. Anderson  S. Bentley  B. Enoch  C. A. Haswell  C. Hellier  K. Horne  J. Irwin  T. A. Lister  I. McDonald  P. Maxted  M. Mayor  A. J. Norton  N. Parley  C. Perrier  F. Pont  D. Queloz  R. Ryans  A. M. S. Smith  S. Udry  P. J. Wheatley  D. M. Wilson 《Monthly notices of the Royal Astronomical Society》2009,392(4):1532-1538

We report the discovery of a 7.3 M _J exoplanet WASP-14b, one of the most massive transiting exoplanets observed to date. The planet orbits the 10th-magnitude F5V star USNO-B1 11118−0262485 with a period of 2.243 752 d and orbital eccentricity   e = 0.09  . A simultaneous fit of the transit light curve and radial velocity measurements yields a planetary mass of 7.3 ± 0.5 M _J and a radius of 1.28 ± 0.08 R _J. This leads to a mean density of about 4.6 g cm⁻³ making it the densest transiting exoplanets yet found at an orbital period less than 3 d. We estimate this system to be at a distance of  160 ± 20  pc. Spectral analysis of the host star reveals a temperature of  6475 ± 100 K, log  g = 4.07  cm s⁻² and   v sin  i = 4.9 ± 1.0  km s⁻¹, and also a high lithium abundance,  log  N (Li) = 2.84 ± 0.05  . The stellar density, effective temperature and rotation rate suggest an age for the system of about 0.5–1.0 Gyr.  相似文献   

Evidence for energy injection and a fine-tuned central engine at optical wavelengths in GRB 070419A     

A. Melandri  C. Guidorzi  S. Kobayashi  D. Bersier  C. G. Mundell  P. Milne  A. Pozanenko  W. Li  A. V. Filippenko  Y. Urata  M. Ibrahimov  I. A. Steele  A. Gomboc  R. J. Smith  N. R. Tanvir  E. Rol  K. Huang 《Monthly notices of the Royal Astronomical Society》2009,395(4):1941-1949

We present a comprehensive multiwavelength temporal and spectral analysis of the 'fast rise exponential decay' GRB 070419A. The early-time emission in the γ-ray and X-ray bands can be explained by a central engine active for at least 250 s, while at late times the X-ray light curve displays a simple power-law decay. In contrast, the observed behaviour in the optical band is complex (from 10² up to 10⁶ s). We investigate the light-curve behaviour in the context of the standard forward/reverse shock model; associating the peak in the optical light curve at ∼450 s with the fireball deceleration time results in a Lorenz factor  Γ≈ 350  at this time. In contrast, the shallow optical decay between 450 and 1500 s remains problematic, requiring a reverse shock component whose typical frequency is above the optical band at the optical peak time for it to be explained within the standard model. This predicts an increasing flux density for the forward shock component until   t ∼ 4 × 10⁶ s  , inconsistent with the observed decay of the optical emission from   t ∼ 10⁴ s  . A highly magnetized fireball is also ruled out due to unrealistic microphysic parameters and predicted light-curve behaviour that is not observed. We conclude that a long-lived central engine with a finely tuned energy injection rate and a sudden cessation of the injection is required to create the observed light curves, consistent with the same conditions that are invoked to explain the plateau phase of canonical X-ray light curves of γ-ray bursts.  相似文献   

Thermal equilibria of coronal magnetic arcades     

C. D. C. Steele  E. R. Priest 《Solar physics》1990,127(1):65-94

A coronal magnetic arcade can be thought of as consisting of an assembly of coronal loops. By solving equations of thermal equilibrium along each loop and assuming a base temperature of 2 × 10⁴ K, the thermal structure of the arcade can be found. By assuming a form for the plasma pressure in the arcade, the possible thermal structures can be shown to depend on three parameters. Arcades can contain hot loops with summits hotter than 400 000 K, cool loops at temperatures less than 80 000 K along their lengths, hot-cool loops with cool summits and cool footpoints but hotter intermediate portions, and warm loops, cooler than 80 000 K along most of their lengths but with summits as hot as 400 000 K. For certain arcades, there exist regions where more than one kind of loop is possible. If the parameters describing the arcade are varied, it is possible for non-equilibrium to occur when a type of solution ceases to exist. For example, hot or warm loops can cease to exist so that only cool solutions are possible when the arcade size or pressure is decreased, while warm or cool loops may give way to hot-cool loops when the heating is reduced or the pressure is increased.  相似文献   

Non-equilibrium of a cylindrical magnetic arcade     

C. D. C. Steele  A. W. Hood  E. R. Priest  T. Amari 《Solar physics》1989,123(1):127-141

A cylindrically-symmetric magnetic arcade with its axis on the photosphere is perturbed by means of an alteration in the pressure along the base. The perturbation is examined with a view to finding equilibrium configurations close to the original equilibrium. It is found that equilibria can only be found when the integral of the excess pressure along the base is zero. In other cases no equilibria can be found and the arcade is likely either to collapse or, in the case of a coronal mass ejection, to erupt. For an initial arcade whose field increases linearly with radial distance from the axis, the neighbouring equilibria have been found.  相似文献   

A quantum-mechanical study of the (110) surface of sphalerite (ZnS) and its interaction with Pb<Superscript>2+</Superscript> species     

H. M. Steele  K. Wright  I. H. Hillier 《Physics and Chemistry of Minerals》2003,30(2):69-75

 The structure of the (110) surface of sphalerite has been studied using mainly quantum-mechanical (QM) methods. The experimentally observed puckering of the surface is well reproduced by periodic plane wave density functional calculations. Water adsorption on this surface is modelled using this QM approach and is used to judge the accuracy of less computationally demanding cluster methods. A cluster model, thus validated, is used to study the possible modes of interaction of Pb²⁺ ions with the (110) surface. It is found that adsorption of hydrated PbO and PbOH⁺ is energetically feasible and leads to Pb–O distances compatible with REFLEXAFS data. Received: 22 April 2002 / Accepted: 23 October 2002 Acknowledgements We thank EPSRC for support of this research.  相似文献   

Results of the radiological North Sea Programme RANOSP 1974 to 1976     

Dr. Hans Kautsky  Dr. Douglas F. Jefferies  Dr. A. Kenneth Steele 《Ocean Dynamics》1980,33(4):152-157

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Amoeboid olivine aggregates in the Allende meteorite     

Lawrence Grossman  Ian M Steele 《Geochimica et cosmochimica acta》1976,40(2):149-155

Greyish-brown, irregularly-shaped aggregates composed predominantly of olivine make up ~2% of the Allende meteorite by volume. Many of the aggregates are constructed of subspherical lumps of micron-sized crystals of olivine, pyroxene, nepheline and sodalite surrounded by coarsergrained olivine. Rarely, anorthite, spinel and perovskite are also present. The olivine ranges in composition from Fo64 to Fo99. Pyroxenes range from aluminous diopside to hedenbergite to very Al-rich and Ti-Al-rich varieties. The nepheline contains 1.6–2.4% K₂O and 1.6–5.2% CaO but the sodalite is significantly poorer in these elements. The spinel contains 2.1–13.4% FeO. Textural information and oxygen isotopic data suggest that the aggregates are composed of primary, solid condensates from the solar nebula. The perovskite. spinel and Ti-Al-rich pyroxenes are the remains of high-temperature condensates but the olivine compositions and the presence of feldspathoids indicate that some of the grains continued to react with the solar nebular vapor in the temperature range 500–900°K.  相似文献   

Wind driven currents near a coast     

H. D. Dooley  J. H. Steele 《Ocean Dynamics》1969,22(5):213-223

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Volatile Phase Separation in Silicic Magmas at Bajo de la Alumbrera Porphyry Cu-Au Deposit, NW Argentina   总被引：7，自引：0，他引：7  

Anthony C. Harris    Vadim S. Kamenetsky    Noel C. White  David A. Steele 《Resource Geology》2004,54(3):341-356

Abstract. At the Bajo de la Alumbrera porphyry Cu-Au deposit, NW Argentina, several key textural elements preserve evidence for volatile separation. Interconnected miarolitic cavities, while being studied extensively in granites, have now been recognized in intrusions related to porphyry Cu mineralization. Pods of saccharoidal quartz are connected by narrow, anastomosing zones of graphic quartz-alkali feldspar intergrowths and ragged biotite (with lesser apatite and magnetite). Their connectivity can be as much as 15 cm; however, more commonly, the interconnected miarolitic cavities are approximately 1 to 2 mm across and 5 cm or less, long. Features such comb-quartz layered textures and magmatic-hydrothermal veins (P veins), combined with aqueous fluid phase equilibria from fluid inclusions, better constrain physical models of exsolution. We interpret these textures in the context of vapour phase formation, coalescence and accumulation in an evolving silicic magma. Recognition of textures, such as the interconnected miarolitic cavities reported here, may provide a simple exploration tool for porphyry Cu deposits, helping explorers to recognize evidence for a potentially fertile intrusions.  相似文献   

Use of Rain and Dry Deposition Compositions for Interpreting Ground-Water Chemistry     

George H. Wagner  Kenneth F. Steele 《Ground water》1985,23(5):611-616

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