Orbital non-fermi-liquid behavior in cubic ruthenates

Physical Review Letters

Volumn 100, Issue 9, 2008, Pages

  Laad, M S ^a   Bradaric I ^a,b   Kusmartsev, F V ^a  

^a LOUGHBOROUGH UNIVERSITY   (United Kingdom)

^b UNIVERSITY OF BELGRADE   (Serbia)

Author keywords

[No Author keywords available]

Indexed keywords

COULOMB INTERACTIONS; ELECTRIC CONDUCTIVITY; PARAMAGNETIC MATERIALS; RAMAN SPECTROSCOPY;

DYNAMICAL MEAN-FIELD THEORY; RAMAN LINE SHAPES;

FERMI LEVEL;

EID: 40849120787     PISSN: 00319007     EISSN: 10797114     Source Type: Journal    
DOI: 10.1103/PhysRevLett.100.096402     Document Type: Article

References (26)

1. P.W. Anderson, in The Theory of High-Tc Superconductivity in the Cuprates (Princeton University, Princeton, NJ, 1998).
2. P. Coleman, J. Phys. Condens. Matter JCOMEL 0953-8984 8, 9985 (1996). 10.1088/0953-8984/8/48/020
3. T. Chien, Phys. Rev. Lett. 67, 2088 (1991). PRLTAO 0031-9007 10.1103/PhysRevLett.67.2088
4. T. Rosenbaum, Phys. Rev. B PRBMDO 0163-1829 57, R13997 (1998). 10.1103/PhysRevB.57.R13997
5. E. Abrahams, Phys. Rev. B PRBMDO 0163-1829 68, 094502 (2003). 10.1103/PhysRevB.68.094502
6. C.M. Varma, Phys. Rev. Lett. 63, 1996 (1989). PRLTAO 0031-9007 10.1103/PhysRevLett.63.1996
7. P. Kostic, Phys. Rev. Lett. 81, 2498 (1998). PRLTAO 0031-9007 10.1103/PhysRevLett.81.2498
8. L. Klein, Phys. Rev. B PRBMDO 0163-1829 60, 1448 (1999); 10.1103/PhysRevB.60.1448
9. Y.S. Lee, Phys. Rev. B PRBMDO 0163-1829 66, 041104 (2002). 10.1103/PhysRevB.66.041104
10. D. Kirillov, Phys. Rev. B PRBMDO 0163-1829 51, 12825 (1995). 10.1103/PhysRevB.51.12825
11. We have fitted the Raman intensity of the electronic background to the form C.ω up to 3000cm-1; see Fig. 1. The data were taken at 5.4 K by triple scanning spectrometer where all types of contributions with different polarizations have been included. In our view this observed background is associated with low-energy orbital excitations. At the energy higher than 3000cm-1 the magnetic excitations may already take over the orbital ones. Therefore, this part of the spectrum has been excluded in our fits.
12. G. Cao, Phys. Rev. B PRBMDO 0163-1829 56, 321 (1997); 10.1103/PhysRevB.56.321
13. S.C. Gausepohl, Phys. Rev. B PRBMDO 0163-1829 54, 8996 (1996). 10.1103/PhysRevB.54.8996
14. G.M. Zhang, Phys. Rev. B PRBMDO 0163-1829 49, 7759 (1994). 10.1103/PhysRevB.49.7759
15. Q. Si, Phys. Rev. B PRBMDO 0163-1829 46, 1261 (1992). 10.1103/PhysRevB.46.1261
16. K.D. Schotte, Phys. Rev. 182, 479 (1969); PHRVAO 0031-899X 10.1103/PhysRev.182.479
17. A. Luther, Phys. Rev. B PRBMDO 0163-1829 19, 320 (1979). 10.1103/PhysRevB.19.320
18. P.W. Anderson, Phys. Rev. B PRBMDO 0163-1829 55, 11785 (1997); 10.1103/PhysRevB.55.11785
19. P.W. Anderson Phys. Rev. Lett. 67, 2092 (1991). PRLTAO 0031-9007 10.1103/PhysRevLett.67.2092
20. Hyeong-Do Kim, Phys. Rev. Lett. 93, 126404 (2004); PRLTAO 0031-9007 10.1103/PhysRevLett.93.126404
21. P.S. Cornaglia and A. Georges, Phys. Rev. B PRBMDO 0163-1829 75, 115112 (2007). 10.1103/PhysRevB.75.115112
22. B.S. Shastry, Phys. Rev. Lett. 65, 1068 (1990). PRLTAO 0031-9007 10.1103/PhysRevLett.65.1068
23. C.M. Varma, Phys. Rev. Lett. 79, 1535 (1997). PRLTAO 0031-9007 10.1103/PhysRevLett.79.1535
24. A. Khurana, Phys. Rev. Lett. 64, 1990 (1990). PRLTAO 0031-9007 10.1103/PhysRevLett.64.1990
25. E. Müller-Hartmann, Z. Phys. B ZPCMDN 0722-3277 76, 211 (1989); 10.1007/BF01312686
26. For experimental details, see A.P. MacKenzie, Phys. Rev. B PRBMDO 0163-1829 58, R13318 (1998). 10.1103/PhysRevB.58.R13318