共查询到20条相似文献，搜索用时 291 毫秒
1.
即将用于新疆奇台110 m射电望远镜(Qi Tai radio Telescope,QTT)的促动器需在-40~60℃范围内满足±15μm的精度要求。由于在无任何补偿的情况下,热误差可以达到约400μm,因此需要建立热误差模型,以预测促动器位移随温度的变化规律,并在此基础上进行位移主动控制补偿,从而保证促动器在给定温度下能满足定位精度的要求。首先,结合模型基本要求与显著性检验,从促动器上的16个温度测量点中优选出一个最适合模型建立的点;然后,采用灰色预测理论建立促动器的热误差模型;最后,根据实际情况对该模型进行修正。研究表明:创新地采用统计学与工程实践相结合的方式选取测温点,建立的热误差模型可以指导促动器的位移主动控制补偿,从而使促动器在要求的-40~60℃范围内达到±15μm±4μm的定位精度。 相似文献
2.
Yu. V. Pisanko 《Solar System Research》2005,39(5):426-430
The Parker model is modified to describe a rapid temperature increase from the region of temperature minimum to the coronal base and to relate the electron density in the region of the temperature minimum (～0.85×1011 cm?3 according to the modified model) to that at the orbit of the Earth (～7.42 cm?3 according to the model). The coronal temperature reaches its maximum (1.8×106 K) at the Parker critical point; physical processes at this point are left beyond the scope of the model. It is suggested to consider the expanding solar corona as a self-heating system in which heating of the solar corona is related to the transonic regime of its expansion, which is maintained by the high coronal temperature. 相似文献
3.
《Chinese Astronomy and Astrophysics》1982,6(3):243-247
We have analysed the finite temperature λφ4 model in the Robertson Walker metric, taking into consideration spontaneous symmetry breaking, particle production and symmetry recovery through phase transition under a high temperature, and found that it is possible to have a cosmological model free of singularities. Such a model begins in the singularity-free, horizon-free, Beltrami-Anti-de Sitter state. Continual production of particles keeps on raising its temperature until a critical temperature TC is reached, when a phase change takes place, and the universe is transformed into a radiation-dominated, thermally-expanding Friedmann state. This phase transition corresponds to a big-bang without, however, an antecedent singularity. 相似文献
4.
We analyze the spatial distribution of the intensity of radio emission from a cool filament in terms of the generalized Kippenhahn-Schluter model. Based on a numerical calculation of the centimeter radio emission and using the temperature transition layer model by Anzer and Heinzel (1999), we show that two symmetric brightening bands must be observed near the filament. The absence of any bands during observations with a sufficient angular resolution suggests that a different type of model is realized: a model with a narrow (unobservable) temperature transition layer across a magnetic field, in particular, a Kuperus-Raadu-type model. 相似文献
5.
6.
The surface temperature of a planet with an atmosphere depends, amongst other factors, on the atmospheric chemical composition and surface pressure. However, the detailed calculation of surface temperature variations as a function of atmospheric composition is extremely complex. We therefore present in this paper a simplified model which can be used to follow surface temperature changes over periods up to the lifetime of the solar system. We apply this model to a number of chemical constituents of interest in studying the evolution of planetary atmospheres (with special reference to the Earth). 相似文献
7.
本文简略介绍了MSISE90大气密度模型，它是以提高低高度大气密度计算精度为目标，基于MSIS86模式，采用不相干散射雷达和卫星质谱仪测量资料，在半经验公式的基础上进行拟合处理而成；并指出了Hedin对该模型的修正之处。并将该模型应用于GPS无线电掩星反演中性地球大气参数的先验温度序列的生成。 相似文献
8.
Donald F. Neidig Jr. 《Solar physics》1973,33(1):63-67
The brightness temperature curve of the quiet Sun at millimeter wavelengths suggests a possible inversion in the mid-millimeter range. Interpreting this as a result of an actual inversion in the chromospheric temperature structure, and example of a model chromoshere is presented whose calculated temperature curve exhibits such an inversion. This model is then tested for radial brightness distribution at millimeter wavelengths. Comparing the calculated distributions at 3.2 mm and 6 mm with eclipse measurements made with parabolic cylinders at 3.2 mm and 8.6 mm shows qualitative agreement, allowing for instrumental smoothing. It is conluded that a chromospheric temperature inversion, either actual or effective, could account for the inversion suggested by millimeter data and also the complex brightness distributions measured during eclipses with parabolic cylinders. 相似文献
9.
A simple analytical model is developed from which we have calculated the temperature throughout the lunar interior resulting
from internal heat sources and the imposition of surface temperature boundary conditions. The surface temperature is determined
almost entirely by the balance of solar heating and surface reradiation; as a consequence this temperature is latitude dependent,
decreasing towards the lunar poles. The internal solution shows that the latitude effect exists almost undiminished to great
depths within the Moon.
It is suggested that this dependence on latitude may have a significant effect on the Moon’s thermal evolution. Using the
liquefaction model the high concentration of lunar maria at low latitudes may be explained. 相似文献
10.
Association between winter temperature in China and upper air circulation over East Asia revealed by canonical correlation analysis 总被引：2，自引：0，他引：2
Canonical correlation analysis (CCA) was used to study the relationship between the winter temperature in China and the circulation at 500 hPa over East Asia. CCA identifies a number of paired patterns that depend on Principle Component (PC) truncation of the two fields. Retaining more PCs usually gives more physically meaningful CCA patterns, but the leading paired pattern has often less explained variance. When fewer PCs are adopted, the leading pattern possesses larger variance. However, it is often distorted in comparison with PC or rotated PC patterns. Various combinations with different PC and CCA patterns remained were tried, which shows that retaining as many PCs as possible and using the first several CCAs instead of only the first give most reasonable connection mechanisms. A statistical downscaling model based on CCA modes linking temperature with circulation was established to quantify the extent to which temperature variation can be explained by circulation. The model was optimised by varying numbers of the PCs and the CCA modes retained. With 13th PC truncation in the circulation and 8th PC truncation in the temperature as well as five CCA modes retained, the optimal CCA model is achieved based on cross-validation. The optimal downscaling model accounts for 47.5% temperature variance on average. However, there is a remarkable regional difference, which ranges from 10% to 70% in brier-based score (BBS). It is concluded that 500-hPa circulation is strongly linked to surface temperature in parts of the country, but it alone is not sufficient to achieve a successful statistical downscaling of the temperature for whole China. 相似文献
11.
A model of the transition layer of an active region of the Sun is presented based on radio observations. The model is deduced by using the Laplace transform of the brightness temperature and the hydrostatic equilibrium equation. A rational function, well-behaved in the coronal region, has been used to represent the observed brightness temperature. The model indicates the existence of a very steep temperature gradient and suggests the presence of a constant conductive flux from the corona into the chromosphere. Both these conclusions are quantitatively in a very good agreement with those deduced from the UV emission lines observations, thus removing a previous discrepancy between radio and optical based models. It is also shown that the presence of a weak magnetic field does not alter the above conclusions. 相似文献
12.
Richard J. Defouw 《Solar physics》1970,14(1):42-61
The convective stability of a simple model chromosphere is investigated. The model chromosphere consists of protons, electrons, and hydrogen atoms in the ground state; ionization is collisional and recombination is radiative. The analysis indicates stability when the kinetic temperature (T) is less than 17 500K (assuming T increases with height). However, for T > 17 500K, the model chromosphere is overstable in the absence of magnetic fields provided the temperature inversion is sufficiently steep. For smaller values of the temperature gradient, field-free regions are stable if the density is small and monotonically unstable if it is large. In the presence of a magnetic field, the model chromosphere is monotonically unstable for T > 17 500K, regardless of the temperature gradient.The convective instability of the model chromosphere results from the fact that the plasma is thermally unstable for T > 17 500K. Thermally unstable regions of the solar atmosphere, although not represented in detail by the model, should behave in a similar fashion.Field-free regions of the solar chromosphere are probably not monotonically unstable, but overstability is possible and may explain the origin of chromospheric oscillations with periods less than 200 sec. It is suggested that spicules result from the monotonic instability of magnetic regions. A similar instability in the corona may be responsible for the large Doppler spreading of radar echoes.Elementary considerations of thermal balance predict that the temperature gradient should diverge at levels of marginal stability. The chromospheric region of spicule formation and the corona should therefore both be bounded below by abrupt temperature jumps. 相似文献
13.
We have developed a coupled atmosphere and ocean model of Titan's surface. The atmospheric model is a 1-D spectrally-resolved radiative-convective model. The ocean thermodynamics are based upon solution theory. The ocean, initially composed of CH4, becomes progressively enriched in ethane over time. The partial pressures of N2 and CH4 in the atmosphere are dependent on the ocean temperature and composition. We find that the resulting system is stable against a runaway greenhouse. Accounting for the decreased solar luminosity, we find that Titan's surface temperature was about 20 K colder 4 Gyr ago. Without an ocean, but only small CH4 lakes, the temperature change is 12 K. In both cases we find that the surface of Titan may have been ice covered about 3 Gyr ago. In the lakes case condensation of N2 provides the ice, whereas in the ocean case the ocean freezes. The dominant factor influencing the evolution of Titan's surface temperature is the change in the solar constant--amplified, if an ocean is present, by the temperature dependence of the solubility of N2. Accretional heating can dramatically alter the surface temperature; a surface thermal flux of 500 erg cm-2 sec-1, representative of small levels of accretional heating, results in a approximately 20 K change in surface temperatures. 相似文献
14.
The structure of the cosmic microwave background temperature is studied in the context of a Bianchi type-V tilted cosmological model. First integrals of the equations for the null geodesics are found by use of the symmetries of the model, enabling the celestial temperature distribution to be found. The quadrupole and dipole moments are calculated for some models, suggesting that the observed anisotropy in the cosmic microwave background can be understood in the context of a Bianchi type-V model of the Universe. The apparent magnitude-redshift relations are also calculated for these models. 相似文献
15.
P. R. Wilson 《Solar physics》1969,9(2):303-314
In paper I of this series it was shown that Edmonds' center-limb rms intensity fluctuation data provided strong evidence for
the existence of a maximum in the horizontal temperature fluctuation near 250 km (optical depth 0.7). The data also gave a
much less reliable indication of a second temperature fluctuation maximum approximately 100 km below this level. Two models,
model 1 exhibiting a single temperature fluctuation maximum and model 2 which has two temperature fluctuation maxima, were
put forward as worthy of further investigation.
In this paper the theoretical mean limb-darkening for these models is compared with the observed limb-darkening. Neither is
satisfactory and several modifications are discussed. Models of the first type can be made to fit these data only by making
adjustments which appear to be inconsistent with convection as an explanation of the temperature fluctuations. Further, the
agreement with the fluctuation data is now less satisfactory. However, a modified model of the second type is developed which
is consistent with the convection hypothesis, which is in good agreement with the mean limb-darkening and is in qualitative
agreement with the fluctuation data.
This is interpreted as providing some evidence that the photospheric granulation arises from a shallow convection layer at
the base of the photosphere. 相似文献
16.
Ilias M. Vardavas 《Solar physics》1987,108(2):403-410
A radiative-convective climate model was used to explore the response of the mean global vertical temperature structure to a variation in the solar UV flux over the solar cycle. The model predicted a cooling of the troposphere and a warming of the stratosphere from solar minimum to solar maximum. The response of the atmospheric temperature to solar UV variations was found to be moderated by a concomitant change in the mean global stratospheric ozone content. 相似文献
17.
In the present work, we employ a nonlocal Nambu–Jona–Lasinio (NJL) model with a Gaussian form factor that is dependent on the spatial components of the momentum (3D-FF). Focusing on the temperature-baryon chemical potential plane, we investigate some aspects of the phase diagram. Initially, we propose an assumption that the range of interactions in momentum space may be modified by temperature, allowing us to obtain the critical temperature values based on lattice QCD (LQCD) predictions. Subsequently, we consider this model within a hybrid framework to examine the effects of temperature, together with neutrino trapping, in compact object configurations. 相似文献
18.
Yvette Cuny 《Solar physics》1971,16(2):293-313
An interpretation is given of the observations of the continuous solar radiation in the spectral range 600–1700 Å. The model allows for deviations from LTE of H, C, Si and S, and is in hydrostatic equilibrium. The predicted intensity from 1680 to 1520 Å has virtually no dependence on the electron temperature variation in the optical depth range 10–3–4 × 10–5, at 5000 Å; the brightness temperature is compatible with a low electronic temperature minimum near the optical depth 10–4. The model of the low chromosphere is characterized by a steep temperature gradient. The model satisfies observations at millimeter wavelengths. 相似文献
19.
Using data covering the 2.6–10 Å wavelength range from the OSO-5 satellite a four-parameter model of the emitting region in a flare process is derived. The thermal emission spectrum of Landini and Fossi is used to calculate the plasma parameters, electron temperature and emission measure. The X-ray flare data is explained by a model which treats the source volume as two time-varying temperature regions. 相似文献
20.
Ralph D. Lorenz Hasso B. Niemann Dan N. Harpold Stanley H. Way John C. Zarnecki 《Meteoritics & planetary science》2006,41(11):1705-1714
Abstract— A simple thermal model is developed to determine the temperature history of the inlet tube of the Huygens probe gas chromatograph mass spectrometer (GCMS) after its fortuitous emplacement on the surface of Saturn's moon Titan. The model parameters are adjusted to match the recorded temperature history of a nearby heater, taking into account heat losses by conduction to the rest of the probe and to Titan's cold atmosphere. The model suggests that after impact when forced convective cooling ceased, the inlet temperature rose from ?110 K to an asymptotic value of only ?145 K. This requires that the inlet was embedded in a surface that acted as an effective heat sink, most plausibly interpreted as wet or damp with liquid methane. The data appear inconsistent with a tar or dry, fine‐grained surface, and the inlet was not warm enough to devolatilize methane hydrate. 相似文献