The Impact of the Anomalous Magnetic Field of the Earth on Demographic Indices (using Latvia as an example)

The increase of cosmic radiation on 23 February 1956 by solar radiation exhibited in the first minutes a high peak at European stations that were lying in direct impact zones for particles coming from a narrow angle near the sun, whilst other stations received no radiation for a further time of 10 minutes and more. An hour later all stations in intermediate and high latitudes recorded solar radiation in a distribution as would be expected if this radiation fell into the geomagnetic field in a fairly isotropic distribution. The intensity of the solar component decreased at this time at all stations according to the same hyperbolic law (~t–2).It is shown, that this decreasing law, as well as the increase of the impact zones on the earth, can be understood as the consequence of an interstellar magnetic field in which the particles were running and bent after their ejection from the sun.Considering the bending in the earth's magnetic field, one can estimate the direction of this field from the times of the very beginning of the increase in Japan and at high latitudes. The lines of magnetic force come to the earth from a point with astronomical co-ordinates near 12·00, 30° N. This implies that within the low accuracy they have the direction of the galactic spiral arm in which we live. The field strength comes out to be about 0·7 × 10–6gauss. There is a close agreement with the field, that Fermi and Chandrasekhar have derived from Hiltner's measurements of the polarization of starlight and the strength of which they had estimated to the same order of magnitude.

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Investigation of the Earth Ionosphere Using the Radio Emission of Pulsars

Open Astronomy ◽

10.1515/astro-2017-0147 ◽

2013 ◽

Vol 22 (1) ◽

Cited By ~ 3

Author(s):

O. M. Ulyanov ◽

A. I. Shevtsova ◽

D. V. Mukha ◽

A. A. Seredkina

Keyword(s):

Magnetic Field ◽

Radio Emission ◽

Dispersion Measure ◽

Pulsar Radio ◽

The Earth ◽

Lack Of Information ◽

Rotation Measure ◽

System Data ◽

Gps System ◽

The Impact

AbstractThe investigation of the Earth ionosphere both in a quiet and a disturbed states is still desirable. Despite recent progress in its modeling and in estimating the electron concentration along the line of sight by GPS signals, the impact of the disturbed ionosphere and magnetic field on the wave propagation still remains not sufficiently understood. This is due to lack of information on the polarization of GPS signals, and due to poorly conditioned models of the ionosphere at high altitudes and strong perturbations. In this article we consider a possibility of using the data of pulsar radio emission, along with the traditional GPS system data, for the vertical and oblique sounding of the ionosphere. This approach also allows to monitor parameters of the propagation medium, such as the dispersion measure and the rotation measure using changes of the polarization between pulses. By using a selected pulsar constellation it is possible to increase the number of directions in which parameters of the ionosphere and the magnetic field can be estimated.

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How radial and quasi radial IMF impact the Earth's magnetopause's size, location, and shape. Does this impact generate Dawn-Dusk asymmetry in the magnetosheath?: Global 3D Kinetic Simulations.

10.5194/egusphere-egu21-9675 ◽

2021 ◽

Author(s):

Suleiman Baraka ◽

Olivier Le Contel ◽

Lotfi Ben-Jaffel ◽

Bill Moore

Keyword(s):

Magnetic Field ◽

Maximum Density ◽

Bow Shock ◽

Temperature Anisotropy ◽

Pressure System ◽

Particle In Cell ◽

The Earth ◽

The Impact ◽

Shape And Size ◽

Dipole Tilt

The boundary between the solar wind (SW) and the Earth&#8217;s magnetosphere, named the magnetopause (MP), is highly dynamic. Its location and shape can vary as a function of different SW parameters such as density, velocity, and interplanetary magnetic field (IMF) orientations. We employ a 3D kinetic Particle-In-Cell (IAPIC) code to simulate these effects. &#160;We investigate the impact of radial (B = Bx) and quasi-radial (Bz < Bx, By) IMF on the shape and size of Earth&#8217;s MP for a dipole tilt of 31o using both maximum density steepening and pressure system balance methods for identifying the boundary. We find that, compared with northward or southward-dominant IMF conditions, the MP position expands asymmetrically by 8 to 22% under radial IMF. In addition, we construct the MP shape along the tilted magnetic equator and the OX axes showing that the expansion is asymmetric, not global, stronger on the MP flanks, and is sensitive to the ambient IMF. Finally, we investigate the contribution of SW backstreaming ions by the bow shock to the MP expansion, the temperature anisotropy in the magnetosheath, and a strong dawn-dusk asymmetry in MP location.

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Magnetic to the Core - Communicating paleomagnetism with hands-on activities

10.5194/egusphere-egu2020-7269 ◽

2020 ◽

Author(s):

Annique van der Boon ◽

Greig Paterson ◽

Janine Kavanagh ◽

Andy Biggin

Keyword(s):

Magnetic Field ◽

General Public ◽

Magnetic Polarity ◽

Lessons Learned ◽

Family Science ◽

The Core ◽

The Earth ◽

Hands On ◽

The Uk ◽

The Impact

With geoscience student numbers dwindling, there is a strong need for Earth scientists to enthuse a new generation of prospective students. We created several hands-on activities to introduce members of the general public of all ages to the fundamentals of, and current research in paleomagnetism. We developed these activities at different outreach events in the UK, such as a family science fair (at the Ness Gardens) and a holiday workshop (at the Victoria Gallery & Museum). In the first week of July, 2019, we contributed to the Royal Society Summer Science Exhibition, a science exhibition in London with almost 14,000 visitors of the general public, including many school groups. Visitors came from all educational backgrounds. We had a stand that consisted of 4 hands-on experiments, and an informative backdrop. The four activities allowed visitors to explore the range of tasks that a paleomagnetist does, from the collection and measurement of samples to understanding the behaviour of the Earth&#8217;s magnetic field. Visitors could measure real lavas from Iceland on a custom-built magnetometer that was designed specifically for outreach, and determine the magnetic polarity of the samples. We also created an information booklet with &#8217;10 things you might not know about Earth&#8217;s magnetic field&#8217;, which is openly available under a CC-license. To measure the impact of our stand on visitors&#8217; knowledge of paleomagnetism, we designed a quiz. Our results show that especially for school kids, our stand had a significant impact on their knowledge of the Earth&#8217;s magnetic field. In this contribution we share lessons learned through designing the &#8216;Magnetic to the Core&#8217; stand, hands-on activities and evaluations.

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Implantation of Earth’s atmospheric ions into the nearside and farside lunar soil: implications to geodynamo evolution

10.5194/egusphere-egu2020-7762 ◽

2020 ◽

Author(s):

Yong Wei ◽

Jun Zhong ◽

Fei He ◽

Hui zhang

Keyword(s):

Magnetic Field ◽

Interplanetary Space ◽

Charged Particles ◽

Lunar Soil ◽

Geological History ◽

The Moon ◽

The Earth ◽

N Enrichment ◽

Size And Morphology ◽

The Impact

Earth&#8217;s present dipolar magnetic field extends into the interplanetary space and interacts with the solar wind, forming a magnetosphere filled up with charged particles mostly originating from the Earth&#8217;s atmosphere. In the elongated tail of the magnetosphere, the particles were observed to move either Earthward or tailward with different speeds at different locations, even outside the Moon&#8217;s orbit. We hypothesize that the lunar soil, on both the nearside and farside, should have been impacted by these particles during the geological history, and the impact was controlled by the size and morphology of the magnetosphere. We predict that the farside soil could also have the features similar to those in the nearside soil, e.g., 15N-enrichment. Furthermore, we may infer the evolution of the magnetosphere and atmosphere by examining the implanted particles in the lunar soil from both sides. This hypothesis could provide an alternative way to study the evolution of Earth&#8217;s dynamo and atmosphere.

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An updated summary digital map of the anomalous magnetic field of Russia as a base for geo-modeling

10.5194/egusphere-egu21-3292 ◽

2021 ◽

Author(s):

Tamara Litvinova

Keyword(s):

Magnetic Field ◽

Secular Variation ◽

Geomagnetic Field ◽

Test Site ◽

High Frequency Component ◽

Primary Role ◽

Crust And Upper Mantle ◽

Digital Map ◽

Anomalous Magnetic Field ◽

The Earth

A digital map of the anomalous magnetic field &#160;(AMF) of Russia has been created over 12 years in the monitoring (update) mode. The map was built from the level of the normal magnetic field &#1058; n VSEGEI-1965 &#160;at a scale of 1: 2,500,000 using materials that were not previously involved in the process of summary mapping, taking into account modern digital technologies. The base of digital cartographic data contains grids on the network of 2,500 &#215;2,500 and 5,000&#215;5,000 m and cartographic projects in * .mxd. The anomalous component is of particular interest in the study of geodynamic processes and dynamic environments in the earth's crust and upper mantle. It is believed that the anomalous (short-wave or high-frequency) component, being a quasi-stationary (Lugovenko V.N., 1982) function of the general geomagnetic field, almost does not change over time. However, when calculating it, the primary role is played by the correct registration of the secular variation and the normal field, which change both in time and in space, and these changes are closely related to the dynamic processes inside the Earth. The works of T. Nagata (1969), F. Stacey (1974, 1977), Yu.P. Skovorodkin and L.S. Bezugloy (1980), V.A. Shapiro (1983) and others showed that the anomalous magnetic field of the Earth is also characterized by temporary changes associated with the dynamics of field sources, manifested in anomalies of the secular course. There is a connection between the secular variation anomalies and regional medium-scale anomalies. Within the Manchazh regional anomaly, the anomalous magnetic field increases monotonically at a rate of up to &#177;5 nT per year. It has been established that the source of the Manchazh anomaly is a block of rocks with increasing remanent magnetization, the mechanism of which is still unclear. The relationship between AMF changes with changes in the seismic regime and with individual earthquakes is evidenced by changes in the amplitudes of temporary changes in the local field from 5-8 nT at the Carpathian geodynamic test site and up to 30-80 nT during the Moneron earthquake on southern Sakhalin. Changes up to the first tens of nT AMFs were recorded several days before the Tashkent earthquake (Ulomov, 1967). During this earthquake, the author of this article observed the glow of the atmosphere, which indicates strong short-term changes in the variable geomagnetic field, which caused ionization processes in the surface layers of the atmosphere. The Earth's magnetic field is 99% generated by its internal sources and reacts sensitively to nonequilibrium phase transitions of a different hierarchical class, which are the basis for the self-organization of the planet Earth system. On the map of magnetic anomalies of Russia, geostructures of different orders of rectilinear, circular, arcuate mosaic forms of anomalies are clearly distinguished, grouped into systems, the shape and size of which allows to reasonably judge the geodynamic conditions of their formation.&#160;

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Can we explain the low geo-effectiveness of the fast halo CMEs in 2002 with EUHFORIA?

10.5194/egusphere-egu2020-5543 ◽

2020 ◽

Author(s):

Brigitte Schmieder ◽

Stefaan Poedts ◽

Christine Verbeke

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Disk Center ◽

Magnetic Clouds ◽

The Sun ◽

The Earth ◽

Halo Cmes ◽

The Impact ◽

The Magnetic Field ◽

Ambient Solar Wind

In 2002 (Cycle 23), a weak impact on the magnetosphere of the Earth has been reported for six halo CMEs related to six X-class flares and with velocities higher than 1000 km/s. The registered Dst minima are all between -17 nT and -50 nT.&#160; A study of the Sun-Earth chain of phenomena related to these CMEs reveals that four of them have a source at the limb and two have a source close to the solar disk center (Schmieder et al., 2020). All of CME magnetic clouds had a low z&#8209;component of the magnetic field, oscillating between positive and negative values.We performed a set of EUHFORIA simulations in an attempt to explain the low observed Dst and the observed magnetic fields. We study the degree of deviation of these halo CMEs from the Sun-Earth axis and as well as their deformation and erosion due to their interaction with the ambient solar wind (resulting in magnetic reconnections) according to the input of parameters and their chance to hit other planets. The inhomogeneous nature of the solar wind and encounters&#160; are also important parameters influencing the impact of CMEs on planetary magnetospheres.&#160;

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Formation of Lunar Craters and Bright Rays as a Result of Meteorite Impacts

Symposium - International Astronomical Union ◽

10.1017/s0074180900178404 ◽

1962 ◽

Vol 14 ◽

pp. 415-418

Author(s):

K. P. Stanyukovich ◽

V. A. Bronshten

Keyword(s):

Explosive Charge ◽

The Moon ◽

Meteorite Impacts ◽

The Earth ◽

Lunar Craters ◽

The Impact

The phenomena accompanying the impact of large meteorites on the surface of the Moon or of the Earth can be examined on the basis of the theory of explosive phenomena if we assume that, instead of an exploding meteorite moving inside the rock, we have an explosive charge (equivalent in energy), situated at a certain distance under the surface.

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