Magnetic Storm

Kesuksesan teknologi Feromagnetisme Energy menyebabkan banyak fihak ingin menghadangnya agar tidak masuk ke dunia komersial. Keuntungan PLTMn adalah:
1) Sumber aliran listrik gratis, ajeg, dan stabil; 2) Ramah lingkungan, tidak menimbulkan emisi gas dan kimia berbahaya, dan tidak menghasilkan panas lebih; 3) Dapat dioperasikan pada kondisi cuaca apapun, sangat dingin atau sangat panas, baik di dalam maupun di luar ruangan; 4) Bentuknya bisa kecil dan murah dengan bahan-bahan yang mudah ditemukan di mana-mana; 5) Hampir tidak memerlukan perawatan, bila ada, biaya perawatannya murah.

Preliminary results of an analysis of satellite and ground-based measurements during extremely strong magnetic storms at the end of October 2003 are presented, including some numerical modeling. The geosynchronous satellites Ekspress-A2and Ekspress-A3, and the low-altitude polar satellites Coronas-F and Meteor-3M carried out measurements of charged particles (electrons, protons, and ions) of solar and magnetospheric origin in a wide energy range. Disturbances of the geomagnetic field caused by extremely high activity on the Sun were studied at more than twenty magnetic stations from Lovozero (Murmansk region) to Tixie (Sakha-Yakutia). Unique data on the dynamics of the ionosphere, riometric absorption, geomagnetic pulsations, and aurora observations at mid-latitudes are obtained.

A year after the extreme events on the Sun, in the heliosphere, and on the Earth in October-November 2003 [Veselovsky et al., 2004; Panasyuk et al., 2004; Yermolaev et al., 2005], a similar situation was also observed in November 2004. The main data observed when the strongest magnetic storm with Dst = -373 nT occurred on the Earth are presented in the paper prepared mainly by the participants of the last year's collaboration of native researchers of extreme events. The disturbance of the Sun, solar wind, and magnetosphere during the considered period was weaker than during the similar period in 2003 with respect to a number of parameters; nevertheless, the presented data indicate that the decline phase of solar cycle 23 is one of the most active intervals over the entire period of comprehensive studies of the solar-terrestrial coupling owing to the events that occurred in autumn 2003 and 2004.

The main data on observations of the Sun, interplanetary medium, and magnetosphere, obtained mainly by home researchers during the strongest magnetic storm of November 20, 2003 (Dst=-472 nT), are presented in the work. This period corresponds ...

Reliable, repeatable Earthquake forecast is a subject surrounded by controversy and scepticism. What is clear, is that reliable forecast could be the single most effective tool for earthquake disaster management. Roughly a third of the world's population live in areas that are at risk and, every year since the beginning of the twentieth century earthquakes have caused an average of

The dependence of plasma bubble occurrence
in the eveningside ionosphere, with magnetic activity during
the period years 2001–2004, is studied here based on
the TEC observations gathered by ground-based GPS receivers
which are located in the equatorial and low-latitude
regions in East Asia. The observed plasma bubbles consist
of the plasma-bubble events in the equatorial (stations
GUAM, PIMO and KAYT), and low-latitude regions (stations
WUHN, DAEJ and SHAO). It is shown that most equatorial
plasma-bubble events commence at 20:00 LT, and may
last for >60 min. The magnetic activity appears to suppress
the generation of equatorial plasma bubbles with a time delay
of more than 3 h (4–9 h). While in the low-latitude regions,
most plasma-bubble events commence at about 23:00 LT and
last for <45 min. The best correlation between Kp and lowlatitude
plasma-bubble occurrence is found with an 8–9 h delay,
a weak correlation exists for time delays of 6–7 h. This
probably indicates that over 3 h delayed disturbance dynamo
electric fields obviously inhibit the development of plasma
bubbles in the pre-midnight sector.

The High-altitude Nuclear Detonation (HND) experiments were carried between 1958/62 by both the United States of America (USA) and the former Union of Soviet Socialist Republics (USSR); the Starfish HND resulted in many phenomena, it discharged great amount of beta particles and debris, releasing intense gamma radiation which ionized atoms and molecules, resulting in Compton electrons and the production of Electromagnetic Pulse (EMP); the experiment also produced intense magnetic field, measured worldwide, with magnitude inversely proportional to square of the radial distance; the graph near the detonation center gave similar characteristics to the Magnetic Storms (MS); these characteristics were analyzed, whereas in both phenomenon, an External Magnetic Field-Moment (ExMFM) was produced; both the source and magnitude of the produced ExMFM were also analyzed and a mechanisms suggested for EMP production; characteristics regulating both phenomena are disclosed and elaborated from different perspectives; it is with hope that this will help in the process towards better understanding to some aspects related to the ExMF production in which if managed will be an advancement of the long awaited alternative renewable energy.

Over the past five years our understanding and appreciation of the ionosphere and thermosphere have changed dramatically with the realization that they are strongly coupled to each other and the magnetosphere. The experimental technology that made this advance possible is chains of GPS receivers and imaging, both from the ground and from space. Added to this technology is the progress of modeling the ionosphere and thermosphere and the promise of modeling the magnetosphere including its interaction with the ionosphere. With these tools we now know that the mid-latitude ionosphere, once thought to inactive, is the home to vast movements of ionization during magnetic storms followed by global changes in thermospheric winds and chemistry leading to a complex ionosphere during the recovery period. At the regional scale TIDS, electrobouyancy waves, and irregularities indicate that ionosphere is even more complex than these early results suggest. Given this progress now is an appropriate time to inquire and debate what is required for future progress. Three major goals come to mind. First a global understanding of the thermosphere and how it responds to magnetic storms is essential. In part this will be achieved through modeling but obtaining the required inputs and validating the models will be a challenge. No in situ measurements of thermospheric winds and composition outside the tropics is currently planned although thermospheric composition through imaging from MEO or GEO may be possible. Next a global understanding of the inner magnetosphere, the (partial) ring current, electric fields, and the interaction of currents with ionospheric conductivity gradients is required. The inner magnetosphere is likely responsible for the process called positive-phase ionospheric storms but the combination of measurements plus models has yet to reproduce the existing observations. The Radiation Belt Storm Probes may be able to contribute to this goal with an electric field instrument. Lastly an investigation of the ionosphere at the regional scale will require imaging either by dense arrays of GPS receivers or by regional imagers in orbit with a resolution of 10 km. The DASI program and narrow field imagers from GEO may contribute to this goal. Finally one should keep in mind that much of positive-phase ionospheric storms occur on the dayside where we have the least information and the greatest difficulty in imaging the ionosphere.