New brown dwarf candidates in the Pleiades     

T. Eisenbeiss  M. Moualla  M. Mugrauer  T.O.B. Schmidt  St. Raetz  R. Neuhuser  Ch. Ginski  M.M. Hohle  A. Koeltzsch  C. Marka  W. Rammo  A. Reithe  T. Roell  M. Va&#x;ko 《Astronomische Nachrichten》2009,330(5):439-458

We have performed deep, wide‐field imaging on a ∼0.4 deg² field in the Pleiades (Melotte 22). The selected field was not yet target of a deep search for low mass stars and brown dwarfs. Our limiting magnitudes are R ∼ 22 mag and I ∼ 20 mag, sufficient to detect brown dwarf candidates down to 40 M_J. We found 197 objects, whose location in the (I, R – I) color magnitude diagram is consistent with the age and the distance of the Pleiades. Using CTK R and I as well as JHK photometry from our data and the 2MASS survey we were able to identify 7 new brown dwarf candidates. We present our data reduction technique, which enables us to resample, calibrate, and co‐add many images by just two steps. We estimate the interstellar extinction and the spectral type from our optical and the NIR data using a two‐dimensional χ² fitting (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Planetary transit observations at the University Observatory Jena: XO‐1b and TrES‐1     

St. Raetz  M. Mugrauer  T.O.B. Schmidt  T. Roell  T. Eisenbeiss  M.M. Hohle  N. Tetzlaff  M. Va&#x;ko  A. Seifahrt  Ch. Broeg  J. Koppenhoefer  R. Neuhuser 《Astronomische Nachrichten》2009,330(5):475-481

We report on observations of transit events of the transiting planets XO‐1b and TrES‐1 with a 25 cm telescope of the University Observatory Jena. With the transit timings for XO‐1b from all 50 available XO, SuperWASP, Transit Light Curve (TLC)‐Project‐ and Exoplanet Transit Database (ETD)‐data, including our own I ‐band photometry obtained in March 2007, we find that the orbital period is P = (3.941501 ± 0.000001) d, a slight change by ∼3 s compared to the previously published period. We present new ephemeris for this transiting planet. Furthermore, we present new R ‐band photometry of two transits of TrES‐1. With the help of all available transit times from literature this allows us to refine the estimate of the orbital period: P = (3.0300722 ± 0.0000002) d. Our observations will be useful for future investigations of timing variations caused by additional perturbing planets and/or stellar spots and/or moons (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

A comparison of local simulations and reduced models of MRI-induced turbulence     

Pierre Lesaffre  Steven A. Balbus  Henrik Latter 《Monthly notices of the Royal Astronomical Society》2009,396(2):779-787

We run mean-field shearing-box numerical simulations with a temperature-dependent resistivity and compare them to a reduced dynamical model. Our simulations reveal the co-existence of two quasi-steady states, a 'quiet' state and an 'active' turbulent state, confirming the predictions of the reduced model. The initial conditions determine on which state the simulation ultimately settles. The active state is strongly influenced by the geometry of the computational box and the thermal properties of the gas. Cubic domains support permanent channel flows, bar-shaped domains exhibit eruptive behaviour, and horizontal slabs give rise to infrequent channels. Meanwhile, longer cooling time-scales lead to higher saturation amplitudes.  相似文献   

Dust Detection by the Wave Instrument on STEREO: Nanoparticles Picked up by the Solar Wind?     

Meyer-Vernet  N.  Maksimovic  M.  Czechowski  A.  Mann  I.  Zouganelis  I.  Goetz  K.  Kaiser  M. L.  St. Cyr  O. C.  Bougeret  J.-L.  Bale  S. D. 《Solar physics》2009,256(1-2):463-474

Solar Physics - The STEREO wave instrument (S/WAVES) has detected a very large number of intense voltage pulses. We suggest that these events are produced by impact ionisation of nanoparticles...  相似文献   

STEREO SECCHI and S/WAVES Observations of Spacecraft Debris Caused by Micron-Size Interplanetary Dust Impacts     

St. Cyr  O. C.  Kaiser  M. L.  Meyer-Vernet  N.  Howard  R. A.  Harrison  R. A.  Bale  S. D.  Thompson  W. T.  Goetz  K.  Maksimovic  M.  Bougeret  J.-L.  Wang  D.  Crothers  S. 《Solar physics》2009,256(1-2):475-488

Early in the STEREO mission observers noted that the white-light instruments of the SECCHI suite were detecting significantly more spacecraft-related “debris” than any previously flown coronagraphic instruments. Comparison of SECCHI “debris storms” with S/WAVES indicates that almost all are coincident with the most intense transient emissions observed by the radio and plasma waves instrument. We believe the debris is endogenous (i.e., from the spacecraft thermal blanketing), and the storms appear to be caused by impacts of large interplanetary dust grains that are detected by S/WAVES. Here we report the observations, compare them to interplanetary dust distributions, and document a reminder for future spacebased coronagraphic instrument builders.

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Preface     

Eric R. Christian  Michael L. Kaiser  Therese A. Kucera  O. C. St. Cyr  Lidia van Driel-Gesztelyi  Cristina H. Mandrini 《Solar physics》2009,256(1-2):1-2

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A Multi-Wavelength Simultaneous Study of the Composition of the Halley Family Comet 8P/Tuttle     

E. Jehin  D. Bockelée-Morvan  N. Dello Russo  J. Manfroid  D. Hutsemékers  H. Kawakita  H. Kobayashi  R. Schulz  A. Smette  J. Stüwe  M. Weiler  C. Arpigny  N. Biver  A. Cochran  J. Crovisier  P. Magain  H. Rauer  H. Sana  R. J. Vervack  H. Weaver  J.-M. Zucconi 《Earth, Moon, and Planets》2009,105(2-4):343-349

We report on simultaneous optical and infrared observations of the Halley Family comet 8P/Tuttle performed with the ESO Very Large Telescope. Such multi-wavelength and coordinated observations are a good example of what can be done to support space missions. From high resolution optical spectroscopy of the CN (0,0) 388 nm and NH₂ (0,9,0) 610 nm bands using UVES at UT2 we determined ¹²C/¹³C = 90 ± 10 and ¹⁴N/¹⁵N = 150 ± 20 in CN and we derived a nuclear spin temperature of NH₃ of 29 ± 1 K. These values are similar to those found in Oort-Cloud and Jupiter Family comets. From low resolution long slit spectroscopy with FORS1 at UT2 we determined the CN, C₃ and C₂ production rates and the parent and daughter scale lengths up to 5.2 10⁵ km tailward. From high resolution IR spectroscopy with CRIRES at UT1 we measured simultaneously the production rates and mixing ratios of H₂O, HCN, C₂H₂, CH₄, C₂H₆, and CH₃OH.  相似文献   

Solubility of Pt in sulphide mattes: Implications for the genesis of PGE-rich horizons in layered intrusions   总被引：1，自引：0，他引：1  

Raúl O.C. Fonseca  Ian H. Campbell  Hugh St. C. O&#x;Neill  Charlotte M. Allen 《Geochimica et cosmochimica acta》2009,73(19):5764-5777

The partitioning of Pt in sulphide melt (matte) has been studied as a function of fS₂ and fO₂ at 1200 and 1300 °C. The results show that the solubility of Pt in mattes increases strongly with increasing fS₂ and decreases weakly with increasing fO₂. The increase in Pt solubility with increasing fS₂ is attributed to Pt dissolving in the melt as a sulphide species and the weak inverse dependence of Pt solubility on fO₂ to the diluting effect of increasing O in the melt at high fO₂. These results, coupled with measurements of Pt solubility in silicate melts taken from the literature, allow the calculation of Pt matte/silicate-melt partition coefficients () for a range of conditions pertinent to the formation of Pt-rich horizons in layered intrusions. The calculated values range between 10⁷ and 10¹¹, depending on fO₂ and fS₂, several orders of magnitude higher than previously published values. Our preferred value for for conditions appropriate to the Merensky Reef is 10⁷ and for the Stillwater Pt-rich horizon 10⁸. The new results are consistent with the magmatic hypothesis for Pt-rich horizons in layered intrusions.  相似文献   

PULSE: a finite element code for solving adiabatic nonradial pulsation equations     

Pierre Brassard  Stéphane Charpinet 《Astrophysics and Space Science》2008,316(1-4):107-112

We briefly present the nonradial adiabatic pulsation code PULSE first developped for white dwarf asteroseismology and now used to compute adiabatic oscillation properties for various types of stellar objects. Numerical tests show that the code is able to provide the accuracy (for a given stellar model) required to deal with the precision in frequency expected from the COROT long runs. While the ultimate objective is to compare the output of various pulsation codes (see these proceedings), we already emphasize problems that need to be addressed concerning, in particular, the mesh resolution of the input stellar models and its impact on the accuracy at which frequencies can be computed.  相似文献   

Description and recognition of potassic-richterite,an amphibole supergroup mineral from the Pajsberg ore field,Värmland,Sweden     

Holtstam  Dan  Cámara  Fernando  Skogby  Henrik  Karlsson  Andreas  Langhof  Jörgen 《Mineralogy and Petrology》2019,113(1):7-16

Mineralogy and Petrology - Potassic-richterite, ideally AKB(NaCa)CMg5TSi8O22W(OH)2, is recognized as a valid member of the amphibole supergroup (IMA-CNMNC 2017–102). Type material is from the...  相似文献