Laser ablated carbon plume flow dynamics under magnetic field

2009 ◽  
Vol 105 (8) ◽  
pp. 084909 ◽  
Author(s):  
Kedar A. Pathak ◽  
Abhilash J. Chandy
Keyword(s):  
Magnetic Field ◽  
Flow Dynamics ◽  
Plume Flow

scholarly journals Poloidal Flow in Axisymmetric Pulsar Magnetospheres

1985 ◽  
Vol 38 (1) ◽  
pp. 97 ◽  
Author(s):  
RR Burman
Keyword(s):  
Magnetic Field ◽  
Model Building ◽  
Symmetry Axis ◽  
Flow Dynamics ◽  
Hydrodynamic Equations ◽  
Poloidal Magnetic Field ◽  
Plasma Drift ◽  
Field Lines ◽  
Limiting Case ◽  
The Magnetic Field

This paper deals with dissipation-free flow in steadily rotating axisymmetric pulsar magnetospheres; for each species, relativistic inertia is balanced by the Lorentz force. Knowledge of integrals of the motion, including a complete integral for the limiting case of purely toroidal flow, is used to manipulate the fundamental electromagnetic and hydrodynamic equations into convenient forms. Consideration of the flow dynamics, incorporating plasma drift across the magnetic field and injection along it, provides the physical basis of a description of flow in which the poloidal motion is closely tied to the poloidal magnetic field lines (L. Mestel el al. to be published 1985). Particular attention is paid to flows whose toroidal part tends towards corotation as the symmetry axis is approached, and implications of the results for model building are discussed.

scholarly journals Stellar Winds of Classical T Tauri Stars

1997 ◽  
Vol 163 ◽  
pp. 780-781
Author(s):  
Gemot Paatz ◽  
Max Camenzind
Keyword(s):  
Magnetic Field ◽  
Magnetic Flux ◽  
Flux Tube ◽  
T Tauri Stars ◽  
Flow Dynamics ◽  
Magnetic Flux Tube ◽  
Stellar Winds ◽  
T Tauri ◽  
Tube Function

AbstractWe present calculations of the structure of magnetized winds of classical T Tauri stars (TTSs) in an axisymmetric, stationary, polytropic approximation in a given magnetosphere (i.e. we do not selfconsistently take into account the influence of the flow dynamics on the structure of the underlying magnetosphere). According to the widely accepted model of CTTSs the magnetosphere is dominated by a strong stellar magnetic field (B* ≃ 1 kG) which may be of dipolar type. The behaviour of the magnetic flux-tube function yields valuable constraints on the wind solutions.

scholarly journals Steady Natural Convection Heat and Mass Transfer Due to a Horizontal Line Source in the Presence Of Magnetic Field and Chemical Reaction

2018 ◽  
Vol 7 (3.31) ◽  
pp. 168
Author(s):  
Venkat Rao Kanuri ◽  
Sridevi Dandu ◽  
Santhi Gottumukkala ◽  
Nagubabeswara Rao Cheemalapati
Keyword(s):  
Magnetic Field ◽  
Mass Transfer ◽  
Prandtl Number ◽  
Chemical Reaction ◽  
Line Source ◽  
Schmidt Number ◽  
Horizontal Line ◽  
Transport Parameters ◽  
Centre Line ◽  
Plume Flow

Natural convective heat and mass transfer due to a horizontal line source at an adiabatic plate and plane plume flow are analyzed in the presence of magnetic field and chemical reaction. The case of an isothermal plate and a plate of varying temperature are also discussed. Certain qualitatively distinct behaviours of the transport parameters noticed are - for an adiabatic plate as well as an isothermal plate, the transport parameters have exhibited asymptotic behaviour with the Prandtl number and Schmidt number. For Plume flow centre line velocity has exhibited asymptotic behaviour with Prandtl number and Schmidt number. Transport parameters diminished but centre line velocity of the Plume increased with increasing magnetic field. Chemical reaction is seen to increase centre line velocity/Sherwood number and diminish skin friction/Nusselt number. Comparison of the results at an adiabatic plate with those at an isothermal plate and a plate of varying temperature is made.       

Magnetic-field strengths from optical polarization data

1967 ◽  
Vol 31 ◽  
pp. 381-383
Author(s):  
J. M. Greenberg
Keyword(s):  
Magnetic Field ◽  
Optical Polarization ◽  
Polarization Data ◽  
Term Model ◽  
Source Of Information ◽  
Field Strengths

Van de Hulst (Paper 64, Table 1) has marked optical polarization as a questionable or marginal source of information concerning magnetic field strengths. Rather than arguing about this–I should rate this method asq+-, or quarrelling about the term ‘model-sensitive results’, I wish to stress the historical point that as recently as two years ago there were still some who questioned that optical polarization was definitely due to magnetically-oriented interstellar particles.

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.

Structure in the radiation of the galactic disk

1967 ◽  
Vol 31 ◽  
pp. 355-356
Author(s):  
R. D. Davies
Keyword(s):  
Magnetic Field ◽  
Galactic Disk ◽  
Galactic Magnetic Field ◽  
Measured Polarization

Observations at various frequencies between 136 and 1400 MHz indicate a considerable amount of structure in the galactic disk. This result appears consistent both with measured polarization percentages and with considerations of the strength of the galactic magnetic field.

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