On the scheme for seeking the solution to a system of Maxwell's equations in a spherically symmetric model of the Earth-ionosphere waveguide

Author(s):  
V.N. Popov
2012 ◽  
Vol 27 (40) ◽  
pp. 1250231 ◽  
Author(s):  
HÜSNÜ BAYSAL

We have calculated the total energy–momentum distribution associated with (n+2)-dimensional spherically symmetric model of the universe by using the Møller energy–momentum definition in general relativity (GR). We have found that components of Møller energy and momentum tensor for given spacetimes are different from zero. Also, we are able to get energy and momentum density of various well-known wormholes and black hole models by using the (n+2)-dimensional spherically symmetric metric. Also, our results have been discussed and compared with the results for four-dimensional spacetimes in literature.


1998 ◽  
Vol 57 (10) ◽  
pp. 6094-6103 ◽  
Author(s):  
Masaaki Morita ◽  
Kouji Nakamura ◽  
Masumi Kasai

Author(s):  
E. L. Wolf

Maxwell’s equations describe radiated power from the Sun through space and the atmosphere to the Earth. Black-body radiation arises from matter in thermal equilibrium, as is derived in this chapter. The Stefan–Boltzmann power law is derived, and its consequences are discussed. Basics of the atmosphere are discussed, including kinetic energy arising from the condensation of water vapor to liquid water. The temperatures in the atmosphere are discussed in a layered model. The Sun’s light arrives at Earth through vacuum and the Earth’s atmosphere as electromagnetic waves described by Maxwell’s equations. In contemporary electrical engineering jargon, this is “wireless”, that connects cellphones.


2018 ◽  
Vol 14 (S343) ◽  
pp. 462-463
Author(s):  
Lars Mattsson ◽  
Christer Sandin ◽  
Paolo Ventura

AbstractWe present first results from a project aiming at a better understanding of how gas and dust interact in dust-driven winds from Asymptotic Giant Branch (AGB) stars. We are at the final stage of developing a new parallelised radiation-hydrodynamics (RHD) code for AGB-wind modelling including a new generalised implementation of drift. We also discuss first results from high-resolution box simulations of forced turbulence intended to give quantitative “3D corrections” to dust-driven winds from AGB stars. It is argued that modelling of dust-driven winds of AGB stars is a problem that may need to be treated in a less holistic way, where some parts of the problem are treated separately in detailed simulations and are parameterised back into a less detailed (1D spherically symmetric) model describing the entire picture.


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