scholarly journals Proton acceleration in antiparallel collisionless magnetic reconnection: Kinetic mechanisms behind the fluid dynamics

2011 ◽  
Vol 116 (A9) ◽  
pp. n/a-n/a ◽  
Author(s):  
N. Aunai ◽  
G. Belmont ◽  
R. Smets
Keyword(s):  
Fluid Dynamics ◽  
Magnetic Reconnection ◽  
Proton Acceleration ◽  
Kinetic Mechanisms

scholarly journals Proton Acceleration near an X‐Type Magnetic Reconnection Region

1998 ◽  
Vol 494 (1) ◽  
pp. 430-437 ◽  
Author(s):  
Ken‐ichi Mori ◽  
Jun‐ichi Sakai ◽  
Jie Zhao
Keyword(s):  
Magnetic Reconnection ◽  
Proton Acceleration ◽  
Reconnection Region

scholarly journals The two-fluid dynamics and energetics of the asymmetric magnetic reconnection in laboratory and space plasmas

2018 ◽  
Vol 9 (1) ◽  
Author(s):  
M. Yamada ◽  
L.-J. Chen ◽  
J. Yoo ◽  
S. Wang ◽  
W. Fox ◽  
...  
Keyword(s):  
Fluid Dynamics ◽  
Magnetic Reconnection ◽  
Space Plasmas ◽  
Two Fluid

Proton acceleration in three-dimensional non-null magnetic reconnection

2016 ◽  
Vol 82 (5) ◽  
Author(s):  
Z. Akbari ◽  
M. Hosseinpour ◽  
M. A. Mohammadi
Keyword(s):  
Magnetic Field ◽  
Energy Distribution ◽  
Magnetic Reconnection ◽  
Electric Fields ◽  
Three Dimensional ◽  
Null Point ◽  
Proton Acceleration ◽  
Electric And Magnetic Fields ◽  
Field Lines ◽  
The Magnetic Field

In a three-dimensional non-null magnetic reconnection, the process of magnetic reconnection takes place in the absence of a null point where the magnetic field vanishes. By randomly injecting a population of 10 000 protons, the trajectory and energy distribution of accelerated protons are investigated in the presence of magnetic and electric fields of a particular model of non-null magnetic reconnection with the typical parameters for the solar corona. The results show that protons are accelerated along the magnetic field lines away from the non-null point only at azimuthal angles where the magnitude of the electric field is strongest and therefore particles obtain kinetic energies of the order of thousands of MeV and even higher. Moreover, the energy distribution of the population depends strongly on the amplitude of the electric and magnetic fields. Comparison shows that a non-null magnetic reconnection is more efficient in accelerating protons to very high GeV energies than a null-point reconnection.

Numerical Modeling of Pollution Formation in Waste-to-Energy Systems Using Computational Fluid Dynamics

2011 ◽  
Author(s):  
Alex Frank ◽  
Marco J. Castaldi ◽  
Masato R. Nakamura
Keyword(s):  
Fluid Dynamics ◽  
Gas Phase ◽  
Energy Systems ◽  
Waste To Energy ◽  
High Fidelity ◽  
Nox Formation ◽  
Pollutant Formation ◽  
Kinetic Mechanisms ◽  
Thermal Nox ◽  
Fidelity Model

This investigation has been undertaken to better understand pollutant formation in Waste-to-Energy (WTE) systems by using Computation Fluid Dynamics (CFD). An above-grate gas phase only model was built and calculated in FLUENT™ with the intent of specifically studying the factors that influence the formation of NOx. Results are shown for a typical reciprocating-grate WTE boiler operating on municipal solid waste (MSW). Contours of velocity, temperature, CO2, CO, H2O, and O2 agree well with previous modeling and data resulting in a high fidelity model that can be implemented in the next phase of this research. Preliminary data is shown for thermal NOx and the results are promising. The next phase of this research will include the development and implementation of detailed kinetic mechanisms (DKM) to model NOx formation with the current boiler presented as well as others with varying fuels.

A large rotating structure around AB Doradus A at VLBI scale

2019 ◽  
Vol 15 (S354) ◽  
pp. 189-194
Author(s):  
J. B. Climent ◽  
J. C. Guirado ◽  
R. Azulay ◽  
J. M. Marcaide
Keyword(s):  
Magnetic Reconnection ◽  
Main Sequence ◽  
Complex Structure ◽  
Main Sequence Star ◽  
Polar Cap ◽  
Vlbi Observations ◽  
Rotating Structure ◽  
Source Structure ◽  
Expected Position

AbstractWe report the results of three VLBI observations of the pre-main-sequence star AB Doradus A at 8.4 GHz. With almost three years between consecutive observations, we found a complex structure at the expected position of this star for all epochs. Maps at epochs 2007 and 2010 show a double core-halo morphology while the 2013 map reveals three emission peaks with separations between 5 and 18 stellar radii. Furthermore, all maps show a clear variation of the source structure within the observing time. We consider a number of hypothesis in order to explain such observations, mainly: magnetic reconnection in loops on the polar cap, a more general loop scenario and a close companion to AB Dor A.

Sign in / Sign up

Export Citation Format

Share Document