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11.
Thawed permafrost could cause a serious stability problem for foundations and oil-wells in cold regions. A non-damage testing procedure, employing the Bender Element Method, was used for permafrost samples collected from a continuous frozen core obtained from the North Slope of Alaska, USA. The wave velocity and modulus of thawed permafrost were investigated on various isotropic confining pressure from 0 kPa to 400 kPa per 100 kPa. The received shear wave propagation was recorded, and the elastic wave theory was used to calculate shear modulus. Finally, the shear modulus affected by confining pressure, water content and dry density were analyzed and discussed, and a regression formulation of shear modulus based on the Janbu Model for thawed silty and sandy permafrost were proposed and validation. 相似文献
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Wind is a great source of renewable energy in western Alaska.Consistent winds blow across the barren tundra underlain by warm permafrost in the winter season,when the energy demand is the highest.Foundation engineering in warm permafrost has always been a challenge in wind energy development.Degrading warm permafrost poses engineering issues to design,construction,and operation of wind turbines.This paper describes the foundation design of a wind turbine built in western Alaska.It presents a system for response monitoring and load assessment,and data collected from September 2013 to March 2014.The dynamic properties are assessed based on the monitoring data,and seasonal changes in the dynamic properties of the turbine tower-foundation system and likely resonance between the spinning blades and the tower structure are discussed.These analyses of a wind turbine in warm permafrost are valuable for designing or retrofitting of foundations in warm permafrost. 相似文献
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L. Morales-Rueda M.D. Still P. Roche J.H. Wood J.J. Lockley 《Monthly notices of the Royal Astronomical Society》2002,329(3):597-604
We study the absorption lines present in the spectra of the long-period cataclysmic variable GK Per during its quiescent state, which are associated with the secondary star. By comparing quiescent data with outburst spectra we infer that the donor star appears identical during the two states and the inner face of the secondary star is not noticeably irradiated by flux from the accreting regions. We obtain new values for the radial velocity semi-amplitude of the secondary star, , a projected rotational velocity, and consequently a measurement of the stellar mass ratio of GK Per, . The inferred white dwarf radial velocities are greater than those measured traditionally using the wings of Doppler-broadened emission lines suspected to originate in an accretion disc, highlighting the unsuitability of emission lines for mass determinations in cataclysmic variables. We determine mass limits for both components in the binary, and . 相似文献
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P. A. Woudt D. Kilkenny E. Zietsman B. Warner N. S. Loaring C. Copley A. Kniazev P. Väisänen M. Still R. S. Stobie E. B. Burgh K. H. Nordsieck J. W. Percival D. O'Donoghue D. A. H. Buckley 《Monthly notices of the Royal Astronomical Society》2006,371(3):1497-1502
We report the serendipitous discovery of the Sloan Digital Sky Survey (SDSS) star SDSS J160043.6+074802.9 to be a very rapid pulsator. The variation is dominated by a frequency near 8380 μHz (period = 119.33 s) with a large amplitude (0.04 mag) and its first harmonic at 16760 μHz (59.66 s; 0.005 mag). In between these frequencies, we find at least another eight variations with periods between 62 and 118 s and amplitudes between about 0.007 and 0.003 mag; weaker oscillations might also be present. Preliminary spectrograms from the performance verification phase of the Southern African Large Telescope indicate that SDSS J160043.6+074802.9 is a spectroscopic binary consisting of an sdO star and a late-type main-sequence companion. This makes it the first unambiguous detection of such an sdO star to pulsate, and certainly the first found to exhibit multifrequency variations. 相似文献
16.
E. Leibowitz M. Orio R. Gonzalez-Riestra Y. Lipkin J.-U. Ness S. Starrfield M. Still E. Tepedelenlioglu 《Monthly notices of the Royal Astronomical Society》2006,371(1):424-430
The classical nova V4743 Sgr was observed with XMM–Newton for about 10 h on 2003 April 4, 6.5 months after optical maximum. At this time, this nova had become the brightest supersoft X-ray source ever observed. In this paper, we present the results of a time-series analysis performed on the X-ray light curve (LC) obtained in this observation, and in a previous shorter observation done with Chandra 16 d earlier. Intense variability, with amplitude as large as 40 per cent of the total flux, was observed both times. Similarities can be found between the two observations in the structure of the variations. Most of the variability is well represented as a combination of oscillations at a set of discrete frequencies lower than 1.7 mHz. At least five frequencies are constant over the 16 d time interval between the two observations. We suggest that a period in the power spectrum of both LCs at the frequency of 0.75 mHz and its first harmonic are related to the spin period of the white dwarf (WD) in the system, and that other observed frequencies are signatures of non-radial WD pulsations. A possible signal with a 24 000 s period is also found in the XMM–Newton LC: a cycle and a half are clearly identified. This period is consistent with the 24 278 s periodicity discovered in the optical LC of the source and thought to be the orbital period of the nova binary stellar system. 相似文献
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M. D. Still S. R. Duck & T. R. Marsh 《Monthly notices of the Royal Astronomical Society》1998,299(3):759-767
We report on time-series optical spectrophotometry of the low-inclination intermediate polar RX J0558+5353. This object exhibits coherent continuum and Hα line variations on both the orbital and white dwarf spin cycles. Despite the absence of a well-determined conjunction phase, the spectroscopic ephemeris combined with a favourable comparison with better-studied systems suggests that the impact between gas stream and accretion disc, or magnetosphere, drives orbital phenomena. Continuum variations over the spin cycle are consistent with previous broad-band data and indicate that accretion occurs on two poles of the primary star. We find no significant spin pulsations in the integrated line emission, but do detect variations in the resolved line profiles of Hα. Pulsed profiles are also suggestive of two-pole accretion. Double-peaked Hα line profiles and the non-detection of beat behaviour between the orbital and spin frequencies provide evidence for partial-disc transport in the system. 相似文献
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T. D. C. Ash A. P. Reynolds P. Roche A. J. Norton M. D. Still L. Morales-Rueda 《Monthly notices of the Royal Astronomical Society》1999,307(2):357-364
We report new radial velocity observations of V779 Cen, the optical companion to the X-ray pulsar Cen X-3. Two sets of results at two epochs yield very different radial velocity amplitudes. We demonstrate there are problems with the first set, not least that they are incompatible with the observed duration of the X-ray eclipse for all inclination angles. The anomalously high radial velocities are probably a result of changes in the outflow behaviour of the companion star. Although there is no reason to doubt the results from the second epoch when viewed in isolation, given the anomalous radial velocities of the first epoch, they must be treated with caution. Using these data, the semi-amplitude of the resulting radial velocity curve is found to be 24.4±4.1 km s−1 . Given the accurately measured semi-amplitude of the orbit of the pulsar, 414.3±0.9 km s−1 , the mass ratio of the system is 0.059±0.010. The inclination of the system is found to be 702±27, assuming that the optical component fills its Roche lobe, and that the system is in synchronous rotation. Hence the mass of the neutron star is 1.21±0.21 M⊙ , and the mass of the optical companion is 20.5±0.7 M⊙ . This is a smaller uncertainty than previously reported values, and is consistent with the canonical neutron star mass of 1.4 M⊙ .
In addition, we use our spectra to determine the spectral class of V779 Cen to be O6-7II-III. 相似文献
In addition, we use our spectra to determine the spectral class of V779 Cen to be O6-7II-III. 相似文献
20.
J. R. Barnes A. Collier Cameron T. A. Lister G. R. Pointer M. D. Still 《Monthly notices of the Royal Astronomical Society》2005,356(4):1501-1508
We present Doppler images of the young K5V–K7V rapid rotator LO Peg from seven nights of continuous spectroscopy obtained in 1998 from July 04 to July 10. The images reveal the presence of a strong polar cap with appendages extending to mid-latitudes, but no star-spots are seen below 15°. We briefly discuss the distribution of spots in light of recent flux transport simulations, which are able to reproduce the observed latitude dependence. With the full time series of spectra, of which 314 are useful, many phases are observed three times over the seven nights of observations. Using star-spots as tracers of a solar-like latitudinal differential rotation in our image reconstructions, we find that the equatorial regions complete one more rotation than the polar regions every 181 ± 35 d . LO Peg is the second coolest star for which such a measurement has been made using indirect imaging methods. The degree of latitudinal shear is less than that seen in G and early K dwarfs, suggesting a trend in which differential rotation decreases with stellar mass in (pre-)main-sequence objects. 相似文献