Calibration of base flow separation methods with streamflow conductivity   总被引：1，自引：0，他引：1  

Stewart M  Cimino J  Ross M 《Ground water》2007,45(1):17-27

The conductivity mass-balance (CMB) method can be used to calibrate analytical base flow separation methods. The principal CMB assumptions are base flow conductivity is equal to streamflow conductivity at lowest flows, runoff conductivity is equal to streamflow conductivity at highest flows, and base flow and runoff conductivities are assumed to be constants over the period of record. To test the CMB assumptions, fluid conductivities of ground water, surface runoff, and streamflow were measured during wet and dry conditions in a 12-km(2) stream basin. Ground water conductivities at wells varied an average of 6% from dry to wet conditions, while stream conductivities varied 58%. Shallow ground water conductivity varied significantly with distance from the stream, with lowest conductivities of 87 microS/cm near the divide, a maximum of 520 microS/cm 59 m from the stream, and 215 microS/cm 22 m from the stream. Runoff conductivities measured in three rain events remained nearly constant, with lower conductivities of 35 microS/cm near the divide and 50 microS/cm near the stream. The CMB method was applied to the records from 10 USGS stream-gauging stations in Texas, Kentucky, Georgia, and Florida to calibrate the USGS base flow separation technique, HYSEP, by varying the time parameter 2N*. There is a statistically significant relationship between basin areas and calibrated values of 2N*, expressed as N = 0.46A(0.44), with N in days and A in km(2). The widely accepted relationship N = 0.83A(0.2) is not valid for these basins. Other analytic methods can also be calibrated with the CMB method.  相似文献   

Hydrodynamic and water column properties at six stations associated with mussel farming in Pelorus sound, 1984–85     

M. M. Gibbs  M. R. James  S. E. Pickmere  P. H. Woods  B. S. Shakespeare  R. W. Hickman 《新西兰海洋与淡水研究杂志》2013,47(3):239-254

Mussel farming places a benthic organism in a pelagic environment; it is therefore important to understand the driving force that transports the food to the mussels. The hydrodynamic regimes in the sidearms and embayments in Pelorus Sound are dominated by the lunar tide, and a net estuarine circulation in the main channel flowing inwards along the bottom and outwards along the top. Salinity gradients extend throughout the sound from the river inflows, with strongest density stratification in the sidearms and embayments: nearest the head of the sound. There, the water column is separated at the pycnocline into upper and lower layers which tend to move in different directions or at different velocities. Local circulation patterns modify tidal flushing patterns, producing extended residence times in some embayments, whereas other embayments off the side of the main channel tend to be flushed more rapidly by through‐flow water and have shorter residence times than would otherwise be expected. The changing inflow of fresh water modifies the local hydraulic regimes in the inner sounds, especially during flood conditions.  相似文献   

Evidence of a significant wind‐driven circulation in Akaroa Harbour. Part 1: Data obtained during the September‐November, 1998 field survey     

Darlene N. Heuff  Robert H. Spigel  Alex H. Ross 《新西兰海洋与淡水研究杂志》2013,47(5):1097-1109

Part 1 (P1) of a two‐part study of Akaroa Harbour, Bank's Peninsula, New Zealand, presents observational evidence of the development of a significant wind‐driven circulation in association with strong northerly and southerly wind events. These are common throughout the year though during the 3‐month field campaign (during the Southern Hemisphere spring of 1998) northerly wind events dominated. This wind‐driven circulation resulted in the weakening of density stratification within the Harbour, mixing the water column to depth over a significant portion of the study area.  相似文献   

Indicators of abundance and spatial distribution of lobsters (Homarus americanus) from standard traps     

M. John Tremblay  Carl Macdonald  Ross R. Claytor 《新西兰海洋与淡水研究杂志》2013,47(1):387-399

Indicators of abundance for American lobster (Homarus americanus) based on 8 years of trap catch rates (catch‐per‐unit‐effort, CPUE) were evaluated. Volunteer harvesters recorded count, sex and size of lobsters captured in standard traps on a daily basis during the fishing season in coastal Nova Scotia, Canada. We examined the extent to which standardised CPUEs of prerecruits predict the future catches of legal sizes and explored spatial patterns in the abundance of lobsters of different size and reproductive status. The standardised CPUE of prerecruits was correlated with legal size catches in only one of five areas examined. This area had a strong signal of incoming recruitment. Improving the capacity of prerecruit CPUE for predicting legal size catches several years later most likely lies with model incorporation of variables associated with catchability. The spatial distribution of catch rates showed that the area with the highest historical landings per unit area also had the highest relative abundance of prerecruits. The spatial distribution data point to further areas of research related to recruitment processes in lobster in coastal Nova Scotia.  相似文献   

The EVE Doppler Sensitivity and Flare Observations     

H. S. Hudson  T. N. Woods  P. C. Chamberlin  L. Fletcher  G. Del Zanna  L. Didkovsky  N. Labrosse  D. Graham 《Solar physics》2011,273(1):69-80

The Extreme-ultraviolet Variability Experiment (EVE; see Woods et al., 2009) obtains continuous EUV spectra of the Sun viewed as a star. Its primary objective is the characterization of solar spectral irradiance, but its sensitivity and stability make it extremely interesting for observations of variability on time scales down to the limit imposed by its basic 10 s sample interval. In this paper we characterize the Doppler sensitivity of the EVE data. We find that the 30.4 nm line of He ii has a random Doppler error below 0.001 nm (1 pm, better than 10 km s⁻¹ as a redshift), with ample stability to detect the orbital motion of its satellite, the Solar Dynamics Observatory (SDO). Solar flares also displace the spectrum, both because of Doppler shifts and because of EVE’s optical layout, which (as with a slitless spectrograph) confuses position and wavelength. As a flare develops, the centroid of the line displays variations that reflect Doppler shifts and therefore flare dynamics. For the impulsive phase of the flare SOL2010-06-12, we find the line centroid to have a redshift of 16.8 ± 5.9 km s⁻¹ relative to that of the flare gradual phase (statistical errors only). We find also that high-temperature lines, such as Fe xxiv 19.2 nm, have well-determined Doppler components for major flares, with decreasing apparent blueshifts as expected from chromospheric evaporation flows.  相似文献   

Large-eddy Simulations of Flow Over Forested Ridges   总被引：4，自引：4，他引：0  

Andrew N. Ross 《Boundary-Layer Meteorology》2008,128(1):59-76

Large-eddy simulations (LES) of flow over a series of small forested ridges are performed, and compared with numerical simulations using a one-and-a-half order mixing length closure scheme. The qualitative and quantitative similarity between these results provides some confidence in the results of recent analytical and numerical studies of flow over forested hills using first-order mixing length schemes. Time series of model velocities at various locations within the canopy allow the application of various experimental techniques to study the turbulence in the LES. The application of conditional analysis shows that the structure of the turbulence over a forested hill is broadly similar to that over flat ground, with sweeps and ejections dominating. Differences are seen across the hill, particularly associated with regions of mean flow separation and recirculation near the summit and in the lee of the hill. Detailed comparison of derived mixing lengths from the LES with the assumed values used in mixing-length closure schemes show that the mixing length varies with location across the hill and with height in the canopy. This is consistent with previous wind-tunnel measurements, and demonstrates that a constant mixing-length assumption is not strictly valid within the canopy. Despite this, the first-order mixing-length schemes do give similar results both for the mean flow and the turbulence in such situations.  相似文献   

Red giant stellar collisions in the Galactic Centre     

James E. Dale  Melvyn B. Davies  Ross P. Church  Marc Freitag 《Monthly notices of the Royal Astronomical Society》2009,393(3):1016-1033

We show that collisions with stellar-mass black holes can partially explain the absence of bright giant stars in the Galactic Centre, first noted by Genzel et al. We show that the missing objects are low-mass giants and asymptotic giant branch stars in the range  1–3 M_⊙  . Using detailed stellar evolution calculations, we find that to prevent these objects from evolving to become visible in the depleted K bands, we require that they suffer collisions on the red giant branch, and we calculate the fractional envelope mass losses required. Using a combination of smoothed particle hydrodynamic calculations, restricted three-body analysis and Monte Carlo simulations, we compute the expected collision rates between giants and black holes, and between giants and main-sequence stars in the Galactic Centre. We show that collisions can plausibly explain the missing giants in the  10.5 < K < 12  band. However, depleting the brighter  ( K < 10.5)  objects out to the required radius would require a large population of black hole impactors which would in turn deplete the  10.5 < K < 12  giants in a region much larger than is observed. We conclude that collisions with stellar-mass black holes cannot account for the depletion of the very brightest giants, and we use our results to place limits on the population of stellar-mass black holes in the Galactic Centre.  相似文献   

Determining the spin of two stellar-mass black holes from disc reflection signatures     

R. C. Reis  A. C. Fabian  R. R. Ross  J. M. Miller 《Monthly notices of the Royal Astronomical Society》2009,395(3):1257-1264

We present measurements of the dimensionless spin parameters and inner-disc inclination of two stellar-mass black holes. The spin parameter of SWIFT J1753.5−0127 and GRO J1655−40 is estimated by modelling the strong reflection signatures present in their XMM–Newton observations. Using a newly developed, self-consistent reflection model which includes the blackbody radiation of the disc as well as the effect of Comptonization, blurred with a relativistic line function, we infer the spin parameter of SWIFT J1753.5−0127 to be  0.76^+0.11_−0.15  . The inclination of this system is estimated at  55°⁺²₋₇  . For GRO J1655−40, we find that the disc is significantly misaligned to the orbital plane, with an innermost inclination of  30°⁺⁵₋₁₀  . Allowing the inclination to be a free parameter, we find a lower limit for the spin of 0.90, this value increases to that of a maximal rotating black hole when the inclination is set to that of the orbital plane of J1655−40. Our technique is independent of the black hole mass and distance, uncertainties in which are among the main contributors to the spin uncertainty in previous works.  相似文献   

Theoretical models of planetary nebulae II: NGC 4361, an unusual high-excitation nebula     

L. H. Aller  J. E. Ross  C. D. Keyes  S. J. Czyzak 《Astrophysics and Space Science》1979,64(2):347-357

NGC 4361 is an extremely high excitation, low-density, very inhomogeneous nebula. New spectroscopic data obtained with the Anglo-Australian telescope, together with published material, have been re-interpreted with the aid of theoretical nebular models that permit an estimation of its chemical composition. Helium may be slightly more abundant than in an ordinary planetary, although this is far from certain. Nitrogen, oxygen, and neon appear to be deficient by a factor of 3 or 4 compared with an ordinary planetary nebula. Argon is likewise deficient but the factor is more difficult to establish, partly because of the nebular inhomogeneity and partly because of uncertainties in cross-sections. THe nebula is material bounded and optically thin in the hydrogen continuum. In contrast to other high-excitation nebulae, the low-excitation condensations appear to have been destroyed by penetration of ionizing radiation.  相似文献   

On the evolution of rifted continental margins: comparison of models and observations for the Nova Scotian margin     

Christopher Beaumont  Charlotte E. Keen  Ross Boutilier 《Geophysical Journal International》1982,70(3):667-715

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