scholarly journals General Formula for Impulse Losses in the Process of Emission of Neutrino Pairs by Electrons in a Magnetic Field

2021 ◽  
Vol 7 (9) ◽  
pp. 27-31
Author(s):  
B. Gajiyeva
Keyword(s):  
Magnetic Field ◽  
General Formula ◽  
Opposite Direction ◽  
Asymmetric Transmission ◽  
Polarized Electrons ◽  
Radiation Losses ◽  
The Magnetic Field

Considered formula pulsed radiation losses pairs neutrinos electrons in a magnetic field. Gas consisting of polarized electrons in the direction of the magnetic field and spins composed of polarized electrons in the opposite direction of the magnetic field would receive a different impulse due to the asymmetric transmission of the impulse.

scholarly journals Wood ants express uncertainty when engaging with magnetic cues for directional guidance

2021 ◽  
Author(s):  
Thomas Stephen Collett ◽  
Andrew O Philippides
Keyword(s):  
Magnetic Field ◽  
Opposite Direction ◽  
Horizontal Direction ◽  
Cylindrical Wall ◽  
Black Stripe ◽  
Wood Ants ◽  
Route Direction ◽  
Correct Direction ◽  
Correct Path ◽  
The Magnetic Field

Wood ants were trained indoors to follow a route in a chosen magnetic direction from the centre of a small, circular arena to find a drop of sucrose at the edge. The arena, surrounded by a white cylindrical wall, was in the centre of a 3D coil system that generated an inclined Earth strength magnetic field in any horizontal direction. Between trials, the chosen magnetic training direction was rotated to a new orientation. Tests were given without food and with fresh or reversed paper on the floor of the arena. In a significant number of tests, ants left the centre facing the goal, or in the opposite direction, but they mostly failed to reach the goal. Tests given early in the day, before any training, show that ants remember the magnetic route direction overnight. On some training trials, the position of the sucrose was also indicated by a black stripe. Not uncommonly, ants first moved in the opposite direction to the stripe before switching to the correct direction. Travel away from the reward seems to express the ant's uncertainty about the correct path to take. Tests show that this uncertainty may stem from competing directional cues linked to the room, suggesting that ants are reluctant to rely on magnetic information alone. We conclude that ants can remember a route direction defined by an Earth-strength magnetic field and that they express any uncertainty about the correct direction by moving for a stretch in the opposite direction. In a second experiment, an upright and an inverted triangle were fixed 90° from each other to the inside of the cylinder. Sucrose was placed beneath one of the triangles, dependent on the direction of the magnetic field. Ants failed to master this task and to approach the magnetically cued triangle. Instead, they preferred to approach the upright triangle. The ants were again uncertain of the correct direction and expressed this uncertainty through paths that had segments directed towards both the inverted and the upright triangles.

Magnetic fields of the spinning bodies

2015 ◽  
Vol 12 (04) ◽  
pp. 1550046
Author(s):  
Kostadin Trenčevski
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
General Formula ◽  
Rigid Bodies ◽  
Thomas Precession ◽  
The Earth ◽  
Spinning Bodies ◽  
The Magnetic Field

In this paper we show that the Thomas precession of the spinning bodies, which is in general case constrained in all rigid bodies, induces magnetic field of the spinning bodies. This is one of the main reasons for the magnetic field of the spinning bodies. The general formula for this magnetic field is deduced and if it is applied to the Earth, its magnetic field changes between 0.295 G at the equator and 0.59 G at the poles, assuming that the density inside the Earth is uniform.

scholarly journals On the field of force near the neutral point produced by two equal coaxial coils, with special reference to the Campbell standard of mutual inductance

1925 ◽  
Vol 107 (744) ◽  
pp. 716-724 ◽  
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Special Reference ◽  
Opposite Direction ◽  
Mutual Inductance ◽  
Common Axis ◽  
The Common ◽  
Small Change ◽  
The Magnetic Field ◽  
A Current

When a current is passed through two equal coaxial coils so that the component of the magnetic fields parallel to the common axis add, there is a circle, mid-way between the two coils, at which the magnetic field is zero. At all points in the plane of that circle lying outside it, the field of force is in one direction, and at all points within the circle it is in the opposite direction. It is evident, therefore, that if a coaxial turn of wire be placed in the plane of the circle, the mutual inductance between the two coils will be a maximum, when the wire coincides with the circle, and any small change in the radius of the turn will affect the value of the mutual inductance only to the second order of small quantities.

Die Energiebilanz eines Wasserstoffbogens in axialem Magnetfeld

1965 ◽  
Vol 20 (3) ◽  
pp. 475-484 ◽  
Author(s):  
Udo Heidrich
Keyword(s):  
Magnetic Field ◽  
Electrical Power ◽  
Homogeneous Magnetic Field ◽  
Hydrogen Atmosphere ◽  
Arc Length ◽  
Radial Temperature ◽  
Cylindrically Symmetric ◽  
Radiation Losses ◽  
Current Voltage ◽  
The Magnetic Field

The numerical solution of the energy balance of a cylindrically symmetric hydrogen arc immersed in an axial, strong, homogeneous magnetic field led to the current-voltage-characteristic and the radial temperature distribution. Three types of arc models were used, each with different assumptions on radiation losses. The results show that, by the reduction of the thermal conductivity perpendicular to the magnetic field for a fully ionized plasma, the necessary electrical power is diminished for temperatures along the axis higher than about 2·104°K. For example, an arc with 1 cm radius in a hydrogen atmosphere of 5 · 104 dyne/cm2, in an external magnetic field of 20 kGauss, a temperature along the axis of 105°K requires about 3,5 kW per cm arc length. Of this, radiation losses account for about 0,5 kW per cm. However, without a superimposed magnetic field the electrical power is about 200 kW per cm.

Adiabatic transverse waves in a conducting gas

1971 ◽  
Vol 6 (2) ◽  
pp. 249-255 ◽  
Author(s):  
B. Roberts ◽  
C. Sozou
Keyword(s):  
Magnetic Field ◽  
Opposite Direction ◽  
Axial Direction ◽  
The Other ◽  
Rankine Vortex ◽  
Transverse Waves ◽  
The Core ◽  
The Magnetic Field

This paper is an investigation of the effect of a magnetic field on transverse waves in a perfectly conducting gas which is rotating like a Rankine vortex about the axis of a cylinder. The magnetic field is assumed to be in the axial direction. There are three waves: two waves are rotating in the same direction as the gas, one faster and the other slower than the core speed of the gas, and one wave rotates in the opposite direction.

scholarly journals Attenuation of non-adiabatic oscillations in a cartesian prominence fibril

2007 ◽  
Vol 3 (S247) ◽  
pp. 173-177 ◽  
Author(s):  
R. Soler ◽  
R. Oliver ◽  
J. L. Ballester
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Thermal Conduction ◽  
Finite Width ◽  
Solar Prominence ◽  
Radiation Losses ◽  
Fine Structures ◽  
The Magnetic Field

AbstractOne of the typical features shown by observations of solar prominence oscillations is that they are quickly damped in time by one or several not well-known mechanisms. In addition, recent high resolution observations have revealed that the prominence fine structures, called fibrils, can oscillate with their own periods, independently from the rest of the prominence. The main aim of the present work is to study the attenuation of oscillations supported by a single prominence fibril. We consider an equilibrium made of a prominence plasma Cartesian slab of finite width embedded in a coronal medium, and assume non-adiabatic effects (thermal conduction, radiation losses and heating) as damping mechanisms. The magnetic field is taken uniform and parallel to the slab axis. We find that the efficiency of the non-adiabatic effects as damping mechanisms is different for each magnetoacoustic mode. The obtained values of the damping time are compatible with those observed in the case of the slow modes, but the fast modes are much less attenuated.

Diamagnetic Levitation for Passive Tilt Sensors

2007 ◽  
Vol 998 ◽  
Author(s):  
Lihong Jiao ◽  
Martin Winistöerfer
Keyword(s):  
Magnetic Field ◽  
External Magnetic Field ◽  
External Field ◽  
Opposite Direction ◽  
Weak Magnetic Field ◽  
Magnetic Force ◽  
Diamagnetic Susceptibility ◽  
Diamagnetic Levitation ◽  
Tilt Sensors ◽  
The Magnetic Field

ABSTRACTWhen diamagnetic materials are exposed to an external magnetic field, a weak magnetic field in the opposite direction to the external field is induced and a magnetic force is generated causing diamagnetic materials to be expelled from the external magnetic field. The magnitude of the force increases with increase of the magnitude of diamagnetic susceptibility, χm. In this study, the levitation of graphite in the magnetic field was investigated.

Observing the galactic magnetic field

1967 ◽  
Vol 31 ◽  
pp. 375-380
Author(s):  
H. C. van de Hulst
Keyword(s):  
Magnetic Field ◽  
Fair Agreement ◽  
Solar Neighbourhood ◽  
Galactic Magnetic Field ◽  
The Magnetic Field

Various methods of observing the galactic magnetic field are reviewed, and their results summarized. There is fair agreement about the direction of the magnetic field in the solar neighbourhood:l= 50° to 80°; the strength of the field in the disk is of the order of 10-5gauss.

Evolution of Large-Scale Coronal Structures

1994 ◽  
Vol 144 ◽  
pp. 29-33
Author(s):  
P. Ambrož
Keyword(s):  
Magnetic Field ◽  
Field Line ◽  
Large Scale ◽  
Coronal Magnetic Field ◽  
Source Surface ◽  
Solar Cycles ◽  
Characteristic Relationship ◽  
The Magnetic Field ◽  
Coronal Structures

AbstractThe large-scale coronal structures observed during the sporadically visible solar eclipses were compared with the numerically extrapolated field-line structures of coronal magnetic field. A characteristic relationship between the observed structures of coronal plasma and the magnetic field line configurations was determined. The long-term evolution of large scale coronal structures inferred from photospheric magnetic observations in the course of 11- and 22-year solar cycles is described.Some known parameters, such as the source surface radius, or coronal rotation rate are discussed and actually interpreted. A relation between the large-scale photospheric magnetic field evolution and the coronal structure rearrangement is demonstrated.

Emergence of Twisted Magnetic Flux Related Sigmoidal Brightening

2000 ◽  
Vol 179 ◽  
pp. 263-264
Author(s):  
K. Sundara Raman ◽  
K. B. Ramesh ◽  
R. Selvendran ◽  
P. S. M. Aleem ◽  
K. M. Hiremath
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Magnetic Flux ◽  
Ultra Violet ◽  
Active Regions ◽  
Morphological Properties ◽  
Energy Storage And Conversion ◽  
The Sun ◽  
X Rays ◽  
The Magnetic Field

Extended AbstractWe have examined the morphological properties of a sigmoid associated with an SXR (soft X-ray) flare. The sigmoid is cospatial with the EUV (extreme ultra violet) images and in the optical part lies along an S-shaped Hαfilament. The photoheliogram shows flux emergence within an existingδtype sunspot which has caused the rotation of the umbrae giving rise to the sigmoidal brightening.It is now widely accepted that flares derive their energy from the magnetic fields of the active regions and coronal levels are considered to be the flare sites. But still a satisfactory understanding of the flare processes has not been achieved because of the difficulties encountered to predict and estimate the probability of flare eruptions. The convection flows and vortices below the photosphere transport and concentrate magnetic field, which subsequently appear as active regions in the photosphere (Rust & Kumar 1994 and the references therein). Successive emergence of magnetic flux, twist the field, creating flare productive magnetic shear and has been studied by many authors (Sundara Ramanet al.1998 and the references therein). Hence, it is considered that the flare is powered by the energy stored in the twisted magnetic flux tubes (Kurokawa 1996 and the references therein). Rust & Kumar (1996) named the S-shaped bright coronal loops that appear in soft X-rays as ‘Sigmoids’ and concluded that this S-shaped distortion is due to the twist developed in the magnetic field lines. These transient sigmoidal features tell a great deal about unstable coronal magnetic fields, as these regions are more likely to be eruptive (Canfieldet al.1999). As the magnetic fields of the active regions are deep rooted in the Sun, the twist developed in the subphotospheric flux tube penetrates the photosphere and extends in to the corona. Thus, it is essentially favourable for the subphotospheric twist to unwind the twist and transmit it through the photosphere to the corona. Therefore, it becomes essential to make complete observational descriptions of a flare from the magnetic field changes that are taking place in different atmospheric levels of the Sun, to pin down the energy storage and conversion process that trigger the flare phenomena.

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