Influence of Rashba spin-orbit coupling on the Kondo effect

An Anderson model for a magnetic impurity in a two-dimensional electron gas with bulk Rashba spin-orbit interaction is solved using the numerical renormalization group under two different experimental scenarios. For a fixed Fermi energy, the Kondo temperature TK varies weakly with Rashba coupling [l...

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Veröffentlicht in:Physical review. B 2016-02, Vol.93 (7), Article 075148
Hauptverfasser: Wong, Arturo, Ulloa, Sergio E., Sandler, Nancy, Ingersent, Kevin
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Sprache:eng
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Zusammenfassung:An Anderson model for a magnetic impurity in a two-dimensional electron gas with bulk Rashba spin-orbit interaction is solved using the numerical renormalization group under two different experimental scenarios. For a fixed Fermi energy, the Kondo temperature TK varies weakly with Rashba coupling [lambda]R, as reported previously. If instead the band filling is low and held constant, increasing [lambda]R can drive the system into a helical regime with exponential enhancement of TK. Under either scenario, thermodynamic properties at low temperatures T exhibit the same dependencies on T/TK as are found for [lambda]R=0. Unlike the conventional Kondo effect, however, the impurity exhibits static spin correlations with conduction electrons of nonzero orbital angular momentum about the impurity site. We also consider a magnetic field that Zeeman splits the conduction band but not the impurity level, an effective picture that arises under a proposed route to access the helical regime in a driven system. The impurity contribution to the system's ground-state angular momentum is found to be a universal function of the ratio of the Zeeman energy to a temperature scale that is not TK (as would be the case in a magnetic field that couples directly to the impurity spin), but rather is proportional to T sub()Kdivided by the impurity hybridization width. This universal scaling is explained via a perturbative treatment of field-induced changes in the electronic density of states.
ISSN:2469-9950
2469-9969
DOI:10.1103/PhysRevB.93.075148