电离层胶片频高图数字化转换与分析研究

The ionogram acquired with the ionospheric vertical sounding method is the oldest data in the history of ionospheric research. Using of modern microelectronics and computer technology to digitalize, analyse and preserve the huge amount of historical film ionogram has become more and more important and urgent. This paper introduced the progress of the film ionogram digitalization by using digital image processing technologies to correct and repair film ionogram and convert them in an exchangeable format. An analysis and conversion software, basing on this method, has been developed for the film ionogram analysis, and then it introduces the application of this software by combining the SAO Explorer program for Wuhan film ionogram and pseudo-color ionogram in Yamagawa in Japan. It shows that our method is reliable，and the developed software is used friendly and provides a positive solution in digitalization and analysis of huge amount of historical film ionogram. Firstly, we briefly introduce the film ionogram and the process of its digitalization. By observing a amount of film ionogram, we obtain some common characteristics of the digitalized film ionogram following as: (1) the image rotation are caused by scanning; (2) the vertical axis of a large number of film ionogram exist more or less tilt and bending ; (3) coordinates of the film ionogram appear the non-uniformity phenomena result from the instability of driving motor rotation and the error of altitudinal cursor orientation. Moreover, based on the characteristics of the film ionogram and the SAO Explorer software which is widely used for the digital ionogram analysis in the world, a new method has been developed for film ionogram procession. The method contains the image geometric correction and film ionogram format conversion. The image geometric correction includes such as image rotation correction, vertical correction and coordinates scale correction. After geometric correction, the BMP file format images will be converted to the SBF file format images. Then, we also discuss the data format converting methods, which include two methods of the image data mapping basing on the normalization and logarithm, and the method of the preprocessing of the noise filtering and the threshold setting. Combining with SAO Explorer software, we successfully obtain ionospheric parameters and electron profile from the converted SBF file format digital ionograms. Based on the above method, we developed the software for the film ionogram to realize its correction analysis and conversion of the image format, and then give a introduction for its function and operation. Subsequently, the software are applied into the Wuhan film ionogram which separately observed in the high solar activity year and the low in 1980s last century. The results reveal the converted SBF digital ionogram almost preserve the all echo information of the film ionogram. Furthermore, we expressly discuss the application to the Wuhan film ionogram in 1958 in order to validate the applicability and credibility of the software. And it is showed that the important information of the film ionogram are maintained into the SBF digital ionogram. It is represented that there is credibility for conversion of the software when it applied in the older film ionogram. In sum, this software could apply to the digitalization and analysis of huge amount of historical film ionogram. Last, we extended the function of the software by bring some new conversion method and used it to apply to the pseudo-color ionogram of yamagawa in Japan. The results show that the converted ionogram information basically maintain the importantly ionogram information and the error of scaling of converted SBF file format image is almost acceptable, though there is no preprocessing for the original ionogram. Hence, we could extend the applicable range of the software and apply it to all kinds of simulative ionogram imaging by improving the method and software.

AE指数的可靠性研究

Auroral electrojet index (AE) are usually used to quantitatively describe the activity of the geomagnetic field in the polar region. AE is a means to identify the level of a substorm as well. The auroral electrojet indices (AU, AL, and AE) have served well for more than four decades as measures of magnetospheric substorm activity. However, as substorm studies have progressed considerably during the past several years, the accuracy of the present electrojet indices have become an important issue. Thus it is fortunate for us to reexamine and evaluate the accuracy of the present electrojet indices and improve them if necessary. For a better use of the present indices and for future improvement we examine the limitations of the auroral electrojet indices as an accurate quantitative measure of the auroral electrojets and magnetospheric substorms. Some of the limitations arise from the data availability and also from the present simplified scheme in deriving them, but some of them originate in the definition themselves. In the present paper, we analyze the characteristics of aurora, ionospheric current system and the AE index. It is noted that for the pseudo-breakup events the variations of AE ( > 500 nT) clearly show the sudden increase and slow decrease phases. However, aurora does not expand to poleward or equatorward, and the ionospheric currents presents the features of the magnetic convection. We mainly focus on investigating what time the AE could be used to identify the subtorm.

电离层垂直TEC映射函数的实验观测与统计特性

When used in the determining the total electron content (TEC), which may be the most important ionospheric parameter, the worldwide GPS observation brings a revolutionary change in the ionospheric science. There are three steps in the data processing to retrieve GPS TEC: (1) to estimate slant TEC from the measurements of GPS signals; (2) to map the slant TEC into vertical; and (3) to interpolate the vertical TEC into grid points. In this scientific dissertation we focus our attention on the second step, the mapping theory and method to convert slant TEC into vertical. This is conventionally done by multiplying on the slant TEC a mapping function which is usually determined by certain models of electron density profile. Study of the vertical TEC mapping function is of significance in GPS TEC measurement. This paper first reviews briefly the three steps in GPS TEC mapping process. Then we compare the vertical TEC mapping function which were respectively calculated from the electron density profiles of the ionospheric model and retrieved from the observation of worldwide GPS TEC. We also perform the statistical analysis on the observational mapping functions. The main works and results are as follows: 1. We calculated the vertical TEC mapping functions for both SLM and Chapman models, and discussed the modulation of the ionosphere height to the mapping functions. We use two simple models, single layer model (SLM) and Chapman models, of the ionospheric electron density profiles to calculate the vertical TEC mapping function. In the case of the SLM, we discuss the control of the ionospheric altitude, i.e., the layer height hipp, to the mapping function. We find that the mapping function decreases rapidly as hipp increases. For the Chapman model we study also the control mapping function by both ionospheric altitude indicated by the peak electron density height hmF2, and the scale height, H, which present the thickness of the ionosphere. It is also found that the mapping function decreases rapidly as hmF2 increases. and it also decreases as H increases. 2. Then we estimate the mapping functions from the GPS observations and compare them with those calculated from the electron density models. We first, proposed a new method to estimate the mapping functions from GPS TEC data. This method is then used to retrieve the observational mapping function from both the slant TEC (TECS) provided by International GPS Service (IGS）and vertical TEC provide by JPL Global Ionospheric Maps (GIMs). Then we compare the observational mapping function with those calculated from the electron density models, SLM and Chapman. We find that the values of the observational mapping functions are much smaller than that from the model mapping functions, when the zenith angle is large enough. We attribute this to the effect of the plasmasphere which is above about 1000 km. 3. We statistically analyze the observational mapping functions and reveal their climatological changes. Observational mapping functions during 1999-2007 are used in our statistics. The main results are as follows. (1) The observational mapping functions decrease obviously with the decrement of the solar activity which is represented by the F10.7 index; (2) In annual variations of the observational mapping functions, the semiannual component is found at low-latitudes, and the remarkable seasonal variations at mid- and high-latitudes. (3) The diurnal variation of the observational mapping functions is that they are large in daytime and small at night, they become extremely small in the early morning before sunrise. (4) The observational mapping functions change with latitudes that they are smaller at lower latitudes and larger at higher. All of the above variations of the observational mapping functions are explained by the existence of the plasmasphere, which changes more slowly with time and more rapidly with latitude than the ionosphere does . In summary, our study on the vertical TEC mapping function imply that the ionosphere height has a modulative effect on the mapping function. We first propose the concept of the 'observational mapping functions' , and provide a new method to calculate them. This is important in improving the TEC mapping. It may also possible to retrieving the plasmaspheric information from GPS observations.

Millstone Hill电离层F层等效风场的气候学研究

Neutral winds and electric fields in the ionospheric F layer play important roles in the variations of the ionosphere, and also affect the thermospheric circulation via the close coupling between the ionosphere and the thermosphere. By now, the neutral winds and electric drifts are generally observed with ground-based Fabry-Perot interferometers (FPI) and incoherent scatter radars (ISR), rockets, and satellite-borne instrument. Based on the servo theory, the ionospheric equivalent winds, which include the information of both the neutral winds and electric fields, can be derived from these characteristic parameters observed by ionosondes. This indirect derivation has potential values in climatological researches and space weather forecast. With the data set of the incoherent scatter radar observations at Millstone Hill, USA, from 1976 to 2006, we statistically analyzed the climatological variations of the vertical component of the equivalent winds (VEWs) over Millstone Hill, which are derived from the ionospheric key parameters (the peak electron number density and peak height of the F2 layer, NmF2 and hmF2) on the basis of the servo theory, Liu's method, and measurements from the ion line-of-sight velocity as well. The main results of this analysis are summarized as follows: (1) The values of VEWs over Millstone Hill during nighttime are stronger than in the daytime, and the upward drift dominates most of the day. In 1993, Hagan found that the component of the neutral winds in the magnetic meridion in daytime is weaker than during nighttime under both solar maximum and minimum conditions; he also found that the equatorward winds dominate most of the day. Both results suggest that the thermosphere in Millstone Hill is modulated by the aurorally driven high-latitude circulation cell; that is, during geomagnetic quiet periods, the average auroral activity is strong enough to drive thermospheric circulation equatorward for most of the day at Millstone Hill. Moreover, since ion drag is the strongest during daytime when F region densities are enhanced by photoionization, the wind speeds are smaller during the daytime than in the nighttime. (2) There is equinoctial symmetry in VEWs at Millstone Hill. The amplitudes and phases of VEWs in spring are quite similar to those in autumn. In contrast, the nighttime upward drift in winter is weaker than in summer and the difference becomes more significant with increasing solar activity. This solstice asymmetry indicates that, the aurorally driven circulation in the northern hemisphere at Millstone Hill latitude is weaker in winter due to arctic darkness, because the subsolar point is in the southern hemisphere. (3) The comparison of the VEWs derived from three methods, i.e., the servo theory, Liu's method, and the ISR ion line-of-sight velocity measurements, indicates that the amplitudes and main phase tendencies of these VEWs accord well with each other during nighttime hours. However, the case in the daytime is relatively worse. This daytime discrepancy can be explained in terms of the effects of photochemical processes and the choices of the servo constants. A larger servo constant gives a stronger plasma drift in daytime. Therefore, this study tells how important to choose a suitable constant for deriving VEWs at Millstone Hill.

磁层－电离层电流的暴时变化以及主磁场对空间环境的影响

Two problems are studied in this thesis, the relationship of the magneto-spheric - ionospheric current systems during storms, and the effects of the main field to the space environment. The thesis includes three parts. 1. Magnetic disturbances caused by magnetospheric - ionospheric current systems Transient variations of the geomagnetic field at middle-low latitudes are mainly caused by the ionospheric dynamo current (IDC), the symmetric ring current (SRC), the partial ring current-region II field-aligned current-ionospheric current system (PRFI), and the region I field-aligned current-ionospheric current system (FACI). The storm on May 1 ～ 6, 1998 is analyzed. Firstly, the S_q-field caused by IDC current is removed by using the modified Hibberd's method in which the effect of SRC is considered. The neglect of SRC-field can give as much as 40% error in S_q-field evaluation. Secondly, the disturbance fields at the middle and low latitudes are separated according to their origins. As a result, the disturbance caused by FACI-current is an important part of the asymmetrical depression of H-component in middle and low latitudes during storms. The results show that the relative intensity of the Sq-field increases in the main phase of the storm and decreases in the recovery phase. The latitudinal gradient of the Sq-field is positive during the whole storm. The storm of May 1 ～ 6, 1998 contains two events. In the first event on May 2, the SRC-field is similar to Dst index. But in the second event on May 4 ～ 5, the SRC-field delays to Dst index, and the SRC-field depresses while the PRFI- and FACI-fields recovery. 2. Analysis of S_q~p variation in CGM coordinates In order to study the conjugation of geomagnetic variations between northern and southern hemispheres, we use the corrected geomagnetic coordinates (CGM) instead of the geomagnetic coordinates (GM) to analyze the S_q~P equivalent current system. The CGM coordinates are built up by International Geomagnetic Reference Field (IGRF) model. The S_q~p variations and equivalent current systems in the northern and southern polar regions are more symmetrical in CGM coordinates than in GM co-ordinates. This fact implies that the current distributions in polar regions are governed by the configuration of the geomagnetic field lines. As the elaborate structure of S_q~p current system in quiet time is obtained, we summarize the seasonal variation of the electrojet in quiet time. 3. The magnetospheric configuration of non-parallel-dipole model The magnetospheric configurations are calculated for two possible geomag-netic field models during the geomagnetic field reversals. These models are the dipole field with the axis to the sun and the quadrupole field model. We use the finite element method to solve the magnetic equation, and use the surface evolution method to solve the equilibrium equation. The results show that the main field greatly affects the space environment.

Interaction between coronal mass ejections and the solar wind

Jones, R. A.; Breen, A. R.; Fallows, R. A.; Canals, A.; Bisi, M. M.; Lawrence, G. (2007). Interaction between coronal mass ejections and the solar wind, Journal of Geophysical Research, 112, Issue A8 RAE2008

Radio tomography: A new experimental technique

Pryse, Sian, 'Radio tomography: A new experimental technique', Surveys in Geophysics (2003) 24 pp.1-38 RAE2008

Evidence for the tongue of ionization under northward interplanetary magnetic field conditions

Pryse, Sian; Middleton, H. R.; Kersley, L.; Bust, G. S., 'Evidence for the tongue of ionization under northward interplanetary magnetic field conditions', Journal of Geophysical Research (2005) 110(A7) pp.A07301 RAE2008

Large-scale structure of the fast solar wind

Breen, Andrew; Bisi, M.M.; Fallows, R.A.; Habbal, S.R., (2007) 'Large-scale structure of the fast solar wind', Journal of Geophysical Research 112(A6) pp.A06101 RAE2008

Midlatitude daytime D region ionosphere variations measured from radio atmospherics

We measured the midlatitude daytime ionospheric D region electron density profile height variations in July and August 2005 near Duke University by using radio atmospherics (or sferics for short), which are the high-power, broadband very low frequency (VLF) signals launched by lightning discharges. As expected, the measured daytime D region electron density profile heights showed temporal variations quantitatively correlated with solar zenith angle changes. In the midlatitude geographical regions near Duke University, the observed quiet time heights decreased from ∼80 km near sunrise to ∼71 km near noon when the solar zenith angle was minimum. The measured height quantitative dependence on the solar zenith angle was slightly different from the low-latitude measurement given in a previous work. We also observed unexpected spatial variations not linked to the solar zenith angle on some days, with 15% of days exhibiting regional differences larger than 0.5 km. In these 2 months, 14 days had sudden height drops caused by solar flare X-rays, with a minimum height of 63.4 km observed. The induced height change during a solar flare event was approximately proportional to the logarithm of the X-ray flux. In the long waveband (wavelength, 1-8 Å), an increase in flux by a factor of 10 resulted in 6.3 km decrease of the height at the flux peak time, nearly a perfect agreement with the previous measurement. During the rising and decaying phases of the solar flare, the height changes correlated more consistently with the short, rather than the long, wavelength X-ray flux changes. © 2010 by the American Geophysical Union.

The 2003 November 14 occultation by Titan of TYC 1343-1865-1

We observed a stellar occultation by Titan on 2003 November 14 from La Palma Observatory using ULTRACAM with three Sloan filters: u, g, and i (358, 487, and 758 nm, respectively). The occultation probed latitudes 2°?S and 1°?N during immersion and emersion, respectively. A prominent central flash was present in only the i filter, indicating wavelength-dependent atmospheric extinction. We inverted the light curves to obtain six lower-limit temperature profiles between 335 and 485 km (0.04 and 0.003 mb) altitude. The i profiles agreed with the temperature measured by the Huygens Atmospheric Structure Instrument [Fulchignoni, M., and 43 colleagues, 2005. Nature 438, 785 791] above 415 km (0.01 mb). The profiles obtained from different wavelength filters systematically diverge as altitude decreases, which implies significant extinction in the light curves. Applying an extinction model [Elliot, J.L., Young, L.A., 1992. Astron. J. 103, 991 1015] gave the altitudes of line of sight optical depth equal to unity: 396±7 and 401±20 km (u immersion and emersion); 354±7 and 387±7 km (g immersion and emersion); and 336±5 and 318±4 km (i immersion and emersion). Further analysis showed that the optical depth follows a power law in wavelength with index 1.3±0.2. We present a new method for determining temperature from scintillation spikes in the occulting body's atmosphere. Temperatures derived with this method are equal to or warmer than those measured by the Huygens Atmospheric Structure Instrument. Using the highly structured, three-peaked central flash, we confirmed the shape of Titan's middle atmosphere using a model originally derived for a previous Titan occultation [Hubbard, W.B., and 45 colleagues, 1993. Astron. Astrophys. 269, 541 563].

The effect of triclabendazole ("Fasinex") on protein synthesis by the liver fluke, Fasciola hepatica

The effect of the active sulphoxide metabolite of the anthelmintic triclabendazole (TCBZ-SX, 15-50 mu g ml(-1)) on the incorporation of radioactively labelled [C-14] leucine by adult Fasciola hepatica tissue slices was measured by liquid scintillation counting. In addition, the ability of the microfilament-disrupting drug, cytochalasin B, and the microtubule-disrupting drug, tubulozole-C, to inhibit protein synthesis, was assessed by similar methods and compared with TCBZ-SX. The established protein synthesis inhibitors, cycloheximide and actinomycin D were used as positive controls. All the drugs showed a significant inhibition of protein synthesis, albeit to different extents; however, TCBZ-SX was the most potent, with no significant difference between its effect and that of cycloheximide or actinomycin D. Moreover, the concentration of TCBZ-SX, above 15 mu g ml(-1), had little further influence on incorporation of [C-14] leucine. This investigation demonstrates the inhibitory effect of TCBZ-SX, cytochalasin B and tubulozole-C on protein synthesis in F. hepatica and confirms the qualitative observations made in several previous ultrastructural studies.

THE EFFECT OF DIAMPHENETHIDE ON PROTEIN-SYNTHESIS BY THE LIVER FLUKE, FASCIOLA-HEPATICA

The effect of the deacetylated (amine) metabolite of diamphenethide (DAMD, 10 mug ml-1) on the uptake and incorporation by adult Fasciola hepatica of radioactively labelled precursors of DNA, RNA and protein synthesis ([H-3]thymidine, [H-3]uridine and [H-3]leucine, respectively) was measured by liquid scintillation counting. Comparison was made between the effects of DAMD and those of specific inhibitors of DNA, RNA and protein synthesis, namely, 5-fluorouracil, cordycepin and cycloheximide, respectively. DAMD caused a significant decrease in the overall uptake and incorporation of [H-3]uridine by F. hepatica, decreased the incorporation of [H-3]leucine and also caused a significant decrease in the overall protein content of the flukes. The effect of DAMD was similar to that of cycloheximide (I x 10(-3) M), a potent inhibitor of protein synthesis, which also caused a significant decrease in the incorporation of [H-3]leucine by the fluke and a decrease in the overall protein content of the fluke. Cordycepin(100 mug ml-1) caused a significant decrease in the protein content of the fluke, but had no effect on the uptake or incorporation of [H-3]uridine. 5-Fluorouracil (I x 10(-4) m) did not affect the uptake or incorporation of VH]thymidine, nor did it decrease the protein content of the fluke. The results indicate that DAMD inhibits protein synthesis by F. hepatica, possibly by inhibiting RNA synthesis. The results are also consistent with previous morphological investigations involving DAMD.

Gastric emptying in patients with flatulent dyspepsia, with and without gallbladder disease

It has been suggested that the symptoms of flatulent dyspepsia are caused by a functional disturbance of the upper gastrointestinal tract. The aim of this study was to investigate delayed gastric emptying as the basis of symptoms in patients with and without gallbladder disease and after cholecystectomy. There were 13 dyspeptic patients with gallbladder disease, 12 with normal gallbladders, and 13 post-cholecystectomy patients. Gastric emptying was measured by means of a 99mTc-labelled scrambled egg meal and external scintillation counter. The rate of emptying in the symptomatic groups was compared with that in 24 asymptomatic normal control subjects and 12 non-dyspeptic patients with gallbladder disease. Delayed gastric emptying tended to occur in patients with gallbladder disease with and without dyspepsia and was not specifically associated with symptoms.

The effect of hypobaric hypoxia on misonidazole binding in normal and tumour-bearing mice

The effect of hypobaric hypoxia on the in vivo binding of misonidazole was investigated in normal mice and mice bearing T50/80 or CA NT mammary carcinomas. After the intraperitoneal injection of radiolabelled misonidazole, mice were randomised to breathe either room air or air at 0.5 atmospheres. The distribution of misonidazole in liver, kidney, heart, spleen and tumour tissue, 24 h later, was studied by scintillation counting and by autoradiography. Significantly higher misonidazole binding occurred in the livers (x2.5), kidneys (x2.4), spleens (x2.9) and hearts (x1.8) of hypoxic mice compared to controls. Hypobaric hypoxia was associated with a greater than four-fold increase in misonidazole binding within T50/80 tumours. However, significantly higher binding was not demonstrated within CA NT tumours after exposure of tumour-bearing animals to hypoxic conditions. In autoradiographs of hypoxic liver, labelling was intense in regions near to hepatic veins but sparse in areas surrounding portal tracts. This pattern was striking and consistent. In hypoxic kidney, labelling was most intense over tubular cells, less intense over glomeruli and sparse in the renal medulla. It is likely that the hepatic and renal cortical distributions of misonidazole binding reflect local oxygen gradients.