Magnetic field and pressure effects in

2005 ◽  
Vol 359-361 ◽  
pp. 272-274 ◽  
Author(s):  
Takao Ebihara ◽  
Tetsuro Takahashi ◽  
Koji Tezuka ◽  
Masato Hedo ◽  
Yoshiya Uwatoko ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Pressure Effects

PRESSURE EFFECTS ON HIGH-Tc SUPERCONDUCTORS CURRENT TRANSFER

1991 ◽  
Vol 05 (20) ◽  
pp. 3255-3265 ◽  
Author(s):  
V.M. SVISTUNOV ◽  
A.I. D’YACHENKO ◽  
V. YU. TARENKOV
Keyword(s):  
Magnetic Field ◽  
High Pressure ◽  
Magnetic Fields ◽  
Pressure Effects ◽  
High Magnetic Fields ◽  
Magnetic Field Direction ◽  
Current Transfer ◽  
High Tc Superconductors ◽  
High Tc ◽  
The Magnetic Field

The efficiency of high pressure technique for the evidence of the Josephson nature of the intergranular contacts in metal ceramics has been demonstrated. With this technique it has been found that the abnormal hysteresis in fields of the order of tens kOe was not connected with the short-circuited contacts between the granules. The reason for the hysteresis lies in the ambiguity of the magnetization of the granules versus the change in the magnetic field direction. The critical current stability of the Josephson conteacts to high magnetic fields is due to both the inhomogeneity of the contacts and the existence of Abrikosov vortices within the superconducting electrode links.

scholarly journals MHD simulations of jet formation - protostellar jets & applications to AGN jets

2010 ◽  
Vol 6 (S275) ◽  
pp. 383-391 ◽  
Author(s):  
Christian Fendt ◽  
Bhargav Vaidya ◽  
Oliver Porth ◽  
Somayeh Sheikh Nezami
Keyword(s):  
Magnetic Field ◽  
Time Lag ◽  
Field Configuration ◽  
Pressure Effects ◽  
Time Interval ◽  
Jet Formation ◽  
Central Dipole ◽  
Mhd Simulations ◽  
Protostellar Jets ◽  
Jet Collimation

AbstractJet formation MHD simulations are presented considering a variety of model setups. The first approach investigates the interrelation between the disk magnetisation profile and jet collimation. Our results suggest (and quantify) that outflows launched from a very concentrated region at the inner disk tend to be weakly collimated. In the second approach, jet formation is investigated from a magnetic field configuration consisting of a stellar dipole superposed by a strong disk field. We find that the central dipole considerably de-collimates the disk wind. In addition, reconnection flares are launched in the interaction region of disk and stellar magnetic field, subsequently changing the outflow mass flux by factors of two. The time interval between flare ejection is about 1000 Keplerian periods - surprisingly similar to the observed time lag between jet knots. The third approach considers radiative pressure effects on jet collimation - an environment which is interesting mainly for outflows from massive young stars (but also for relativistic jets). Finally we present relativistic MHD simulations of jet formation from accretion disks extenting the previous non-relativistic approaches.

Magnetic field and pressure effects on magnetism of bond-frustrated ZnCr2S4

2013 ◽  
Vol 339 ◽  
pp. 81-83 ◽  
Author(s):  
Y.M. Xie ◽  
Z.R. Yang ◽  
Z.T. Zhang ◽  
C. Shen ◽  
L. Li ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Pressure Effects
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