Effect of applied magnetic fields of physical processes in an MPD arcjet

1976 ◽  
Author(s):  
I. KIMURA ◽  
Y. ARAKAWA
Keyword(s):  
Magnetic Fields ◽  
Physical Processes

scholarly journals Planetary Magnetic Fields and Habitability in Super Earths

2018 ◽  
Vol 27 (1) ◽  
pp. 183-231 ◽  
Author(s):  
Pablo Cuartas-Restrepo
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Scaling Laws ◽  
Thermal Evolution ◽  
Solid Core ◽  
Direct Influence ◽  
Physical Processes ◽  
Planetary Magnetic Fields ◽  
Planetary Magnetic Field ◽  
Planetary Dynamos

Abstract This work seeks to summarize some special aspects of a type of exoplanets known as super-Earths (SE), and the direct influence of these aspects in their habitability. Physical processes like the internal thermal evolution and the generation of a protective Planetary Magnetic Field (PMF) are directly related with habitability. Other aspects such as rotation and the formation of a solid core are fundamental when analyzing the possibilities that a SE would have to be habitable. This work analyzes the fundamental theoretical aspects on which the models of thermal evolution and the scaling laws of the planetary dynamos are based. These theoretical aspects allow to develop models of the magnetic evolution of the planets and the role played by the PMF in the protection of the atmosphere and the habitability of the planet.

scholarly journals Formation of a strong southward IMF near the solar maximum of cycle 23

2004 ◽  
Vol 22 (2) ◽  
pp. 673-687 ◽  
Author(s):  
S. Watari ◽  
M. Vandas ◽  
T. Watanabe
Keyword(s):  
Solar Wind ◽  
Magnetic Fields ◽  
Geomagnetic Storms ◽  
Solar Maximum ◽  
Interplanetary Shocks ◽  
Physical Processes ◽  
Interplanetary Magnetic Fields ◽  
Interplanetary Physics ◽  
Solar Wind Parameters ◽  
Interplanetary Disturbance

Abstract. We analyzed observations of the solar activities and the solar wind parameters associated with large geomagnetic storms near the maximum of solar cycle 23. This analysis showed that strong southward interplanetary magnetic fields (IMFs), formed through interaction between an interplanetary disturbance, and background solar wind or between interplanetary disturbances are an important factor in the occurrence of intense geomagnetic storms. Based on our analysis, we seek to improve our understanding of the physical processes in which large negative Bz's are created which will lead to improving predictions of space weather. Key words. Interplanetary physics (Flare and stream dynamics; Interplanetary magnetic fields; Interplanetary shocks)

scholarly journals Processes in the magnetized chromosphere of the Sun

2008 ◽  
Vol 4 (S257) ◽  
pp. 121-131
Author(s):  
S. S. Hasan
Keyword(s):  
Magnetic Fields ◽  
Large Field ◽  
The Sun ◽  
Physical Processes ◽  
Flux Tubes ◽  
Weak Magnetic Fields ◽  
Space Experiments ◽  
New Space ◽  
Magnetic Network

AbstractWe review physical processes in magnetized chromospheres on the Sun. In the quiet chromosphere, it is useful to distinguish between the magnetic network on the boundaries of supergranules, where strong magnetic fields are organized in mainly vertical flux tubes and internetwork regions in the cell interiors, which have traditionally been associated with weak magnetic fields. Recent observations from Hinode, however, suggest that there is a significant amount of horizontal magnetic flux in the cell interior with large field strength. Furthermore, processes that heat the magnetic network have not been fully identified. Is the network heated by wave dissipation and if so, what is the nature of these waves? These and other aspects related to the role of spicules will also be highlighted. A critical assessment will be made on the challenges facing theory and observations, particularly in light of the new space experiments and the planned ground facilities.

scholarly journals Summary and Conclusions

2021 ◽  
pp. 221-225
Author(s):  
Donald V. Reames
Keyword(s):  
Magnetic Fields ◽  
Source Parameters ◽  
Physical Models ◽  
Current Understanding ◽  
Energy Spectra ◽  
Physical Processes ◽  
Indelible Mark ◽  
Time Profiles

AbstractIn this chapter we summarize our current understanding of SEPs, of properties of the sites of their origin and of the physical processes that accelerate or modify them. These processes can leave an indelible mark on the abundances of elements, isotopes, ionization states, anisotropies, energy spectra and time profiles of the SEPs. Transport of the ions to us along magnetic fields can impose new variations in large events or even enhance the visibility of the source parameters as the SEPs expand into the heliosphere. We lack physical models that can follow the complexity of SEP abundance variations.

scholarly journals Investigating the origin of cyclical spectral variations in hot, massive stars

2013 ◽  
Vol 9 (S302) ◽  
pp. 334-337
Author(s):  
Alexandre David-Uraz ◽  
Gregg A. Wade ◽  
Véronique Petit ◽  
Asif ud-Doula
Keyword(s):  
Magnetic Fields ◽  
Large Scale ◽  
Massive Stars ◽  
Physical Processes ◽  
Corotating Interaction Regions ◽  
Ob Stars ◽  
Wind Variability ◽  
Competing Hypotheses ◽  
Interaction Regions ◽  
Radial Pulsations

AbstractOB stars are known to exhibit various types of wind variability, as detected in their ultraviolet spectra, amongst which are the ubiquitous discrete absorption components (DACs). These features have been associated with large-scale azimuthal structures extending from the base of the wind to its outer regions: corotating interaction regions (CIRs). There are several competing hypotheses as to which physical processes may perturb the star's surface and generate CIRs, including magnetic fields and non radial pulsations (NRPs), the subjects of this paper with a particular emphasis on the former. Although large-scale magnetic fields are ruled out, magnetic spots deserve further investigation, both on the observational and theoretical fronts.

scholarly journals Physical processes in a low-power inductive plasma source in the presence of a weak magnetic field

2021 ◽  
pp. 38-43
Author(s):  
Phedor Ivandikov ◽  
Ilya Zadiriev ◽  
Elena Kralkina
Keyword(s):  
Magnetic Field ◽  
External Magnetic Field ◽  
Magnetic Fields ◽  
Low Power ◽  
Weak Magnetic Field ◽  
Discharge Plasma ◽  
Plasma Source ◽  
Axial Component ◽  
Physical Processes ◽  
Power Coupling

Research into the influence of a weak external magnetic field (<150 G) on the efficiency of power coupling to plasma and on the structure of axial RF fields in plasma is presented. Power coupling to the discharge plasma as well as the structure of the axial component of RF magnetic fields are shown to depend on the external magnetic field’s magnitude in a nonmonotous manner.

Physical processes in the channel of propagation of CO2 laser pulses during the generation of electric and magnetic fields

2021 ◽  
pp. 85-91
Author(s):  
S.F. Balandin ◽  
◽  
V.A. Donchenko ◽  
V.F. Myshkin ◽  
V.A. Khan ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Co2 Laser ◽  
Laser Pulses ◽  
Physical Processes ◽  
Radiation Propagation ◽  
Electric And Magnetic Fields ◽  
Modes Of Interaction ◽  
Long Paths

The mechanisms of generation of electric and magnetic fields during the propagation of microsecond pulses of a CO2 laser in the atmosphere over long paths are considered. The range of radiated waves selected for research is substantiated. The power of the source required for the realization of the pre-breakdown and breakdown modes of interaction of radiation with the medium is estimated. The dependence of the observed signals on the conditions of radiation propagation is investigated. Comparison of theoretical estimates and results of outdoorexperiments is carried out.

scholarly journals Coronal Magnetic Fields Deduced from Radio Methods

1993 ◽  
Vol 141 ◽  
pp. 249-257 ◽  
Author(s):  
A. Krüger ◽  
J. Hildebrandt
Keyword(s):  
Magnetic Fields ◽  
Solar Atmosphere ◽  
Active Regions ◽  
Physical Processes ◽  
Poor Knowledge ◽  
X Ray ◽  
The Poor ◽  
Coronal Magnetic Fields ◽  
Spectral Ranges ◽  
Different Levels

AbstractMajor problems of the physics of the solar atmosphere and processes of solar activity are due to the poor knowledge of the magnetic fields outside the photosphere. Unique methods to determine magnetic fields in the corona and chromosphere make use of radio observations in close connection with information obtained in other spectral ranges e.g. the optical and X-ray regions. Based on relevant emission and propagation processes, the basic radio methods providing information on the parent magnetic fields are summarized. Signatures in the microwave and meter wave regions are used to derive magnetic field parameters at different levels in the solar atmosphere of active regions during quiet and flaring conditions. Implications on fine and gross structures are briefly discussed and consequences on acting physical processes mentioned.

Sign in / Sign up

Export Citation Format

Share Document