The effect of interplanetary parameters as observed in geomagnetic storms in dependence on geomagnetic latitude

Summary The purpose of this study was to determine to what extent the effect of interplanetary parameters is reflected in the separate storms in dependence on geomagnetic latitude. The results were obtained by studying 5 storms of February 1967 and 1968 recorded at 6 observatories between latitude 5.7° and 53.5° with small differences in local time. These results concern the dynamic pressure of the solar wind and the function of the interplanetary electric field, which approximates the plasma injection into the ring current. This is also associated with the decay time of the storm ring. In most cases the dependence of the effect of the investigated parameters on latitude was proved and expressed in terms of quantitative relations with a reasonable degree of correlation. The derived constants were used in a model of time variations of the storm-time geomagnetic field. The storm-time variations, constructed using this model, mostly agree, as regards their main features, with the real variations, whereas differences can be observed in details, namely of a local nature.

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mam maua maum, a nm uu nam naam u nu amuu auumu maum um. mam mm 5 , aumua a 1967. u 1968. m amuu um ¶rt;uana 5, 7°–53,5° nu auuu m u. mam aam ¶rt;uau ¶rt;au ma u uu nam mu n, m annuum uu na m. mu a u ana¶rt;a m ma. um a auum ma u¶rt; naam m um n¶rt;m¶rt;ua u a aa um nu ¶rt;mam mnu uu. nm u una ¶rt;u uuaum n u. ¶rt; auauu u am ¶rt;mumu, u ¶rt;ma mam m mu num a aama.

     

The intensity of the main phase of geomagnetic storms in relation to the parameters of the solar wind

Summary On the basis of investigating 10 storms (1965–1967) good correlation was found between the density of the solar wind energy (₂=1/2mNv²) and the intensity of the main phase of the geomagnetic storms, expressed in terms of the maximum decrease of the horizontal intensity (B=H/cos). The relation between ₂, or Nv², and B could then be used to determine the quantities and ₀ ( is the factor expressing the increase in energy density in the magnetosphere, ₀ is the energy density of the particles in a quiet magnetosphere). A comparison with the directly observed distribution of the energy density of the particles in the magnetosphere indicates that the computed value of ₀ seems to be realistic. The magnitude of the factor will have to be checked again.     

Geomagnetic latitude aspects of the effect of the interplanetary parameters on geomagnetic storms

Summary In this work the previous author's results concerning the geomagnetic effect of the interplanetary parameters in dependence on geomagnetic latitude are verified, complemented and presented with better accuracy. Data of 7 intensive storms recorded in 1973–79 at 5 observatories with slight differences in local time and with the appropriate latitude distribution limited by real possibilities have been analysed. Even in these cases the derived values of the constants determining the dependence of storm-time variations of the geomagnetic field upon both the dynamic pressure of the solar wind(P) and the interplanetary electric field(E_y) vary relatively regularly with geomagnetic latitude. The anomaly of Dst and DR-variations from the Almeria Observatory (AE) evident in some intensive storms is pointed out here. Unlike the previous work the time characteristics () of the ring current decay have been studied from the standpoint of the main (_m) and recovery (_r) phases of the storm. This yields higher values of _r as compared to from the above mentioned work. On the other hand, a large decrease in the values of _r was observed in some cases at a latitude of about 40°, as in the earlier study. Actually this phenomenon does not occur in all intensive storms as could be expected. As to the investigated storms, _m seems to be independent of geomagnetic latitude and much lower in its magnitude than _r.     

Supply of energy to the magnetosphere during the main phase of magnetic storms

au u¶rt;um u mu ¶rt; umu u amu, aa aum, u nuu anmuaum n mu , a ma u n¶rt;nu, m amau uu aum mu u( a a) nnua nu u nam nmama aum mu, aa naam uu . au mmuu mu u a auu ¶rt;a aaua a ¶rt;am a mum uumuu naam ¶rt;a na u ama, n¶rt; a¶rt; uu nu aua ¶rt;nuuaum n mu u. mu ¶rt; num uu, a mmmuu namu naamau , ¶rt; m¶rt; u aua nuu anmuaum n, auam mn uu, a m naama .     

Environmental Impact Assessment of High Pressure Water Scrubbing Biogas Upgrading Technology

The aim of this work was to assess the burdens of a process in terms of environmental and health impacts, resource depletion issues, and energy demand based on the ability of the Life Cycle Assessment methodology to link the environmental impacts with the mass and energy flows. The analysis was done in terms of process and environmental performances of high pressure water scrubbing (HPWS) system applied for biogas upgrading. The application of process simulation based on the Aspen Plus® software has been considered as supportive for the calculation of mass and energy balances. Data processed using GaBi 4: Software showed that global warming, acidification, and human toxicity potentials were the main impact categories associated with the HPWS process. These indicators are largely related to the exhaust gas from the desorption column and the indirect emissions generated during energy consumption. The life cycle inventory study resulted in the development of a database with a vast inventory of data regarding HPWS technology. A basis for assessing potential improvements in the environmental performance of the system is provided. Future studies in this area will address the economical evaluation of the HPWS technology, so as to maximize economic efficiency and minimize environmental impacts.     

Effect of the ns component of the interplanetary magnetic field on geomagnetic storms

Summary The individual storm-time variations of the geomagnetic field were compared with the variations of the B_z-component of the interplanetary magnetic field over 24 and 48-hour intervals of storm time. Good correlation between B_z and Dst was observed in about one half of the 166 cases analysed (1965–72), the time lag of the manifestations of the interplanetary field at the Earth's surface having been taken into account. The effect of the B_z-field is reflected to a considerably larger extent in intense storms (Dst –80 nT). Good correlation was observed in 80% of the total number of 35 intense storms. Preliminary investigations have shown that Dst-variations, constructed from B_z-data using the relations derived herein, are quite close to the observed, particularly as regards the main phase (3 examples are given).