排序方式： 共有34条查询结果，搜索用时 15 毫秒
1.
This paper focuses on different ways of characterizing the solar radiative regime of a day and the stability of this regime. The days may be stratified in classes of cloud shade, observed total cloud cover amount, daily averaged clearness index, and fractal dimension of the solar global irradiance signal. A new Boolean parameter related to solar irradiance fluctuation is defined, namely the sunshine stability number. The time averaged value of the sunshine stability number is used for the characterization of the radiative regime stability during a given time interval. Ranking the days from the view-point of the stability of their radiative regime is performed by using the daily average value of the sunshine stability number and appropriately defined values of disorder and complexity, respectively. Measurements performed in the Romanian town of Timisoara (latitude 45°46?? N, longitude 21°25?? E and 85?m altitude above mean sea level) are used here. They refer to time series of global and diffuse solar irradiance recorded at 15-s time interval between sunrise and sunset during all the days in 2009. 相似文献
2.
3.
V. Badescu 《Theoretical and Applied Climatology》2002,72(1-2):127-136
Summary A model that uses two parameters to describe the state of the sky is presented. The parameters are the total cloud amount
and a new two-value parameter – the sunshine number – stating whether the sun is covered or uncovered by clouds. Regression
formulae to compute instantaneous cloudy sky global and diffuse irradiance on a horizontal surface are proposed. Fitting these
relationships to Romanian data shows low bias errors for global radiation but larger errors for diffuse radiation. The model’s
accuracy is significantly higher than one based on total cloud amount alone. The model is used to generate time-series of
solar radiation data. A first approximate relationship, neglecting auto-correlation of the sunshine number, is used in the
computations.
Received July 17, 2001 Revised November 7, 2001 相似文献
4.
5.
O. Vaduvescu M. Birlan A. Tudorica A. Sonka F.N. Pozo A.D. Barr D.J. Asher J. Licandro J.L. Ortiz E. Unda-Sanzana M. Popescu A. Nedelcu D. Dumitru R. Toma I. Comsa C. Vancea D. Vidican C. Opriseanu T. Badescu M. Badea M. Constantinescu 《Planetary and Space Science》2011,59(13):1632-1646
We report on the follow-up and recovery of 100 program NEAs, PHAs and VIs using the ESO/MPG 2.2 m, Swope 1 m and INT 2.5 m telescopes equipped with large field cameras. The 127 fields observed during 11 nights covered 29 square degrees. Using these data, we present the incidental survey work which includes 558 known MBAs and 628 unknown moving objects mostly consistent with MBAs from which 58 objects became official discoveries. We planned the runs using six criteria and four servers which focus mostly on faint and poorly observed objects in need of confirmation, follow-up and recovery. We followed 62 faint NEAs within one month after discovery and we recovered 10 faint NEAs having big uncertainties at their second or later opposition. Using the INT we eliminated four PHA candidates and VIs. We observed in total 1286 moving objects and we reported more than 10,000 positions. All data were reduced by the members of our network in a team effort, and reported promptly to the MPC. The positions of the program NEAs were published in 27 MPC and MPEC references and used to improve their orbits. The O−C residuals for known MBAs and program NEAs are smallest for the ESO/MPG and Swope and about four times larger for the INT whose field is more distorted. For the astrometric reduction, the UCAC-2 catalog is recommended instead of USNO-B1. The incidental survey allowed us to study statistics of the MBA and NEA populations observable today with 1–2 m facilities. We calculate preliminary orbits for all unknown objects, classifying them as official discoveries, later identifications and unknown outstanding objects. The orbital elements a, e, i calculated by FIND_ORB software for the official discoveries and later identified objects are very similar with the published elements which take into account longer observational arcs; thus preliminary orbits were used in statistics for the whole unknown dataset. We present a basic model which can be used to distinguish between MBAs and potential NEAs in any sky survey. Based on three evaluation methods, most of our unknown objects are consistent with MBAs, while up to 16 unknown objects could represent NEO candidates and four represent our best NEO candidates. We assessed the observability of the unknown MBA and NEA populations using 1 and 2 m surveys. Employing a 1 m facility, one can observe today fewer unknown objects than known MBAs and very few new NEOs. Using a 2 m facility, a slightly larger number of unknown than known asteroids could be detected in the main belt. Between 0.1 and 0.8 new NEO candidates per square degree could be discovered using a 2 m telescope. 相似文献
6.
Roelof D. Schuiling Viorel Badescu Richard B. Cathcart Piet. A. L. C. Van Overveld 《Marine Georesources & Geotechnology》2013,31(1-2):25-37
ABSTRACT Ocean gulfs offer a means of artificially creating a depression, which can be used for a regionally significant hydroelectric macroproject. We examine here the case for a dam at the Strait of Hormuz that blocks a large gulf situated in an arid region. A 35 m evaporation of this concentration basin will reduce its watery surface area by ～53% and allow generation of ～2.050 MW (or possibly ～2.500 MW) of electricity. Our conclusion is that the proposed Electricity Development Infrastructure Node (EDIN) is a feasible and desirable macroproject. If the macroproject starts in the near-term future, it would require a significant change in the logistics of oil and gas transport from this region. Alternatively, it can be considered as an attractive future solution for the energy requirements of the region after exhaustion of its oil and gas reserves. 相似文献
7.
Francisco González-Sánchez Antoni Camprubí Eduardo González-Partida Rafael Puente-Solís Carles Canet Elena Centeno-García Viorel Atudorei 《Mineralium Deposita》2009,44(3):343-361
Northeastern Mexico hosts numerous epigenetic stratabound carbonate-hosted low-temperature hydrothermal deposits of celestine,
fluorite, barite and zinc-lead, which formed by replacement of Mesozoic evaporites or carbonate rocks. Such deposits can be
permissively catalogued as Mississippi Valley-type (MVT) deposits. The deposits studied in the state of Coahuila are associated
with granitic and metasedimentary basement highs (horsts) marginal or central to the Mesozoic Sabinas Basin. These horsts
controlled the stratigraphy of the Mesozoic basins and subsequently influenced the Laramide structural pattern. The Sabinas
Basin consists of ~6,000-m-thick Jurassic to Cretaceous siliciclastic, carbonate and evaporitic series. The MVT deposits are
mostly in Barremian and in Aptian-Albian to Cenomanian formations and likely formed from basinal brines that were mobilized
during the Laramide orogeny, although earlier diagenetic replacement of evaporite layers (barite and celestine deposits) and
lining of paleokarstic cavities in reef carbonates (Zn–Pb deposits) is observed. Fluid inclusion microthermometry and isotopic
studies suggest ore formation due to mixing of basinal brines and meteoric water. Homogenization temperatures of fluid inclusions
range from 45°C to 210°C; salinities range from 0 to 26 wt.% NaCl equiv., and some inclusions contain hydrocarbons or bitumen.
Sulfur isotope data suggest that most of the sulfur in barite and celestine is derived from Barremian to Cenomanian evaporites.
Regional geology and a compilation of metallogenic features define the new MVT province of northeastern Mexico, which comprises
most of the state of Coahuila and portions of the neighboring states of Nuevo León, Durango and, perhaps extends into Zacatecas
and southern Texas. This province exhibits a regional metal zonation, with celestine deposits to the south, fluorite deposits
to the north and barite and Zn–Pb deposits mostly in the central part. 相似文献
8.
Two-dimensional (2D) and one-dimensional (1D) shallow-water models are used to evaluate the seashore effects of the tsunami
generated by an asteroid impacting the western regions of the Black Sea about 208 km from the coast. The tsunami’s speed and
the effects on the coastal regions depend on many factors, among which the most important is asteroid size. The tsunami generated
by a 250-m asteroid reaches the nearest land location in 24 min and needs about 2 h to arrive at all Black Sea coast. The
run-up value is about 7 m high on the Turkish and Crimean coasts. In the western Black Sea regions the wave height is two
or three times smaller. The run-up values strongly depend on bathymetry and topography peculiarities. The run-in value in
case of the tsunami generated by a 1,000-m asteroid is up to eight times larger than in case of a 250-m impactor, depending
on location. The results reported herein are upper limit values. In case of the 250-m asteroid, the real wave amplitude may
be up to two times smaller. The uncertainty factor decreases in case of larger asteroids. Ways of diminishing the social consequences
are briefly discussed. 相似文献
9.
Two new Boolean parameters are defined: the sunshine number (related to the state of the sky) and the sunshine stability number (which is as a measure of the fluctuation of the radiative regime). Elementary statistical and sequential properties of both parameters are presented in this paper. Actinometric and meteorological data measured at 15?s lag during 2009 in Timisoara (Romania, southeastern Europe) are used. The yearly series of daily averaged sunshine number has negative skewness and kurtosis. The series of daily averaged sunshine stability number has positive skewness and kurtosis. The series of daily averaged values of sunshine number are best described by an ARIMA(0,1,2) model. ARIMA(0,1,0) and ARIMA(0,2,0) models (associated with an appropriately defined white noise) may be used for synthesis of the sunshine number time series. The first model is to be preferred for practical reasons. The series of daily averaged values of sunshine stability number are best described by an ARIMA(2,2,1) model. The ARIMA(0,0,0) model is recommended to be used for generating time series of sunshine stability number. This model may be used for any particular day during the year and the only parameter depending on the day is the white noise standard deviation. A relationship between the white noise standard deviation and the daily averaged sunshine stability number is proposed. 相似文献
10.
V. Badescu 《Meteorology and Atmospheric Physics》2001,78(3-4):195-204
Summary
Stationarity of daily averaged surface pressure time series on Mars can be obtained (by differencing) for short time intervals
only. Large pressure variance intervals are usually associated with the dust storm season. Medium and small pressure variance
intervals can be found usually during clear sky periods. General auto-regressive integrated moving average (ARIMA) models
were developed for daily average pressure forecasting at Viking Lander sites. A procedure to find the “appropriate” model
for a given time series was developed. It is based on various degrees of differencing the original time series and a t-statistics-assisted
estimation of the significance of the fitted coefficients. A method employing the cumulative spectrum of the residuals was
used to check the models. ARIMA (3,2,3) seems to be the most “appropriate” model to forecasting the daily average surface
pressure on Mars.
Received December 16, 1999/Revised October 17, 2000 相似文献