Bethe Ansatz for the Bloch Particle in Magnetic Field

1995 ◽  
pp. 399-416
Author(s):  
P. B. Wiegmann ◽  
A. V. Zabrodin
Keyword(s):  
Magnetic Field ◽  
Bethe Ansatz

Bethe-ansatz for the Bloch electron in magnetic field

1994 ◽  
Vol 72 (12) ◽  
pp. 1890-1893 ◽  
Author(s):  
P. B. Wiegmann ◽  
A. V. Zabrodin
Keyword(s):  
Magnetic Field ◽  
Bethe Ansatz ◽  
Bloch Electron

scholarly journals QUANTUM GROUP AND MAGNETIC TRANSLATIONS: BETHE ANSATZ SOLUTION FOR THE HARPER’S EQUATION

1994 ◽  
Vol 08 (05) ◽  
pp. 311-318 ◽  
Author(s):  
P.B. WIEGMANN ◽  
A.V. ZABRODIN
Keyword(s):  
Magnetic Field ◽  
Quantum Group ◽  
Bethe Ansatz ◽  
Critical Value ◽  
Bloch Function ◽  
Present Solution ◽  
Bethe Ansatz Solution ◽  
Bloch Electrons ◽  
Natural Relation

We present the Bethe ansatz solution for the problem of Bloch electrons in magnetic field described by the Harper’s equation [Formula: see text] We made explicit a natural relation between magnetic translations and the quantum group Uq(sl2) and express the midband spectrum and the Bloch function in terms of solutions of the Bethe ansatz equations. In this letter we present solution for the critical value λ=1.

scholarly journals Explicit Solutions of the Bethe Ansatz Equations for Bloch Electrons in a Magnetic Field

1994 ◽  
Vol 73 (8) ◽  
pp. 1134-1137 ◽  
Author(s):  
Yasuhiro Hatsugai ◽  
Mahito Kohmoto ◽  
Yong-Shi Wu
Keyword(s):  
Magnetic Field ◽  
Bethe Ansatz ◽  
Explicit Solutions ◽  
Bloch Electrons

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.

Calculated Coronal Magnetic Fields and Their Comparison with the Coronal Structures as Observed during Five Solar Eclipses

1994 ◽  
Vol 144 ◽  
pp. 559-564
Author(s):  
P. Ambrož ◽  
J. Sýkora
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Coronal Magnetic Field ◽  
Coronal Magnetic Fields ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractWe were successful in observing the solar corona during five solar eclipses (1973-1991). For the eclipse days the coronal magnetic field was calculated by extrapolation from the photosphere. Comparison of the observed and calculated coronal structures is carried out and some peculiarities of this comparison, related to the different phases of the solar cycle, are presented.

Faint Hα Emission in the Corona and Its Relation to the Prominences

1994 ◽  
Vol 144 ◽  
pp. 339-342
Author(s):  
V. N. Dermendjiev ◽  
Z. Mouradian ◽  
J.- L. Leroy ◽  
P. Duchlev
Keyword(s):  
Magnetic Field ◽  
Solar Corona ◽  
Essential Role ◽  
Hα Emission

AbstractThe relation between episodically observed in the solar corona faint Hαemission structures and the long lived prominences was studied. Particular consideration was given for cases in which the corresponding prominences had undergone DB process. An MHD interpretation of the phenomenon “emissions froides” (cool emission) is proposed in which an essential role plays the prominence supporting magnetic field.

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