Comparative study of superconducting and normal-state anisotropy in Fe1+yTe0.6Se0.4 superconductors with controlled amounts of interstitial excess Fe
Source abstract
Abstract
We report a systematic study of the superconducting (SC) and normal-state anisotropy of ${\mathrm{Fe}}1+y{\mathrm{Te}}0.6{\mathrm{Se}}0.4$ single crystals with controlled amounts of excess Fe ($y$ = 0, 0.07, and 0.14). The SC state anisotropy ${\ensuremath{\gamma}}H$ was obtained by measuring the upper critical fields under high magnetic fields over 50 T for both $H\ensuremath{\parallel}ab$ and $H\ensuremath{\parallel}c$. On the other hand, the normal state anisotropy ${\ensuremath{\gamma}}_{\ensuremath{\rho}}$ was obtained by measuring the resistivity with current flowing in the $ab$ plane (${\ensuremath{\rho}}ab$) and along the $c$ axis (${\ensuremath{\rho}}c$). To precisely measure ${\ensuremath{\rho}}ab$ and ${\ensuremath{\rho}}c$ in the same part of a specimen avoiding the variation dependent on pieces or parts, we adopt a new method using a microfabricated bridge with an additional neck part along the $c$ axis. The ${\ensuremath{\gamma}}H$ decreases from a value dependent on the amount of excess Fe at ${T}_{\mathrm{c}}$ to a common value $\ensuremath{\sim}1$ at 2 K. The different ${\ensuremath{\gamma}}H$ at ${T}_{\mathrm{c}}$ ($\ensuremath{\sim}1.5$ for $y$ = 0, and 2.5 for $y$ = 0.14) suggests that the anisotropy of effective mass ${m}c*/{m}ab*$ increases from $\ensuremath{\sim}2.25$ ($y$ = 0) to 6.25 ($y$ = 0.14) with the excess Fe. The almost isotropic ${\ensuremath{\gamma}}H$ at low temperatures is due to the strong spin paramagnetic effect at $H\ensuremath{\parallel}ab$. By contrast, the ${\ensuremath{\gamma}}_{\ensuremath{\rho}}$ shows a much larger value of $\ensuremath{\sim}17$ ($y$ = 0) to $\ensuremath{\sim}50$ ($y$ = 0.14) at the temperature just above ${T}_{\mathrm{c}}$. Combined the results of ${\ensuremath{\gamma}}H$ and ${\ensuremath{\gamma}}_{\ensuremath{\rho}}$ near ${T}_{\mathrm{c}}$, we found out that the discrepant anisotropies between the SC and normal states originates from a large anisotropy of scattering time ${\ensuremath{\tau}}ab/{\ensuremath{\tau}}c\phantom{\rule{4pt}{0ex}}\ensuremath{\sim}$ 7.8. The ${\ensuremath{\tau}}ab/{\ensuremath{\tau}}c$ is found to be independent of the excess Fe.
Source: openalex_inverted_index · Quality: baseline
Research context
OpenAlex topics: Iron-based superconductors research · Physics of Superconductivity and Magnetism · Rare-earth and actinide compounds
SciVX discovery tags are terminology-based. OpenAlex topics are source-provided classifications.
References (68)
Show source-provided references
1. 10.1038/nmat249110.1038/nmat2491 ↗
2. 10.1021/ja907345x10.1021/ja907345x ↗
3. 10.1038/nmat346410.1038/nmat3464 ↗
4. 10.1038/nmat415510.1038/nmat4155 ↗
5. 10.1038/nphys353010.1038/nphys3530 ↗
6. 10.1103/PhysRevLett.116.07700210.1103/PhysRevLett.116.077002 ↗
7. 10.1038/nmat364810.1038/nmat3648 ↗
8. 10.1038/nmat415310.1038/nmat4153 ↗
9. 10.1038/nmat449210.1038/nmat4492 ↗
10. 10.1038/ncomms1084010.1038/ncomms10840 ↗
11. 10.1038/ncomms1218210.1038/ncomms12182 ↗
12. 10.1073/pnas.141347711110.1073/pnas.1413477111 ↗
13. 10.1038/nphys221610.1038/nphys2216 ↗
14. 10.1126/science.aan459610.1126/science.aan4596 ↗
15. 10.1038/s41567-018-0280-z10.1038/s41567-018-0280-z ↗
16. 10.1126/science.aao179710.1126/science.aao1797 ↗
17. 10.1038/s41563-019-0397-110.1038/s41563-019-0397-1 ↗
18. 10.1038/ncomms233710.1038/ncomms2337 ↗
19. 10.1088/0034-4885/74/12/12450110.1088/0034-4885/74/12/124501 ↗
20. 10.1016/j.mattod.2017.09.00610.1016/j.mattod.2017.09.006 ↗
21. M. Tinkham · 1996
22. 10.1063/1.492648610.1063/1.4926486 ↗
23. 10.1103/PhysRevB.79.09450710.1103/PhysRevB.79.094507 ↗
24. 10.1063/1.308145510.1063/1.3081455 ↗
25. 10.1038/nature0767610.1038/nature07676 ↗
26. 10.1134/S002136400914010010.1134/S0021364009140100 ↗
27. 10.1103/PhysRevB.85.18452510.1103/PhysRevB.85.184525 ↗
28. 10.1038/ncomms349910.1038/ncomms3499 ↗
29. 10.1103/PhysRevB.87.10450610.1103/PhysRevB.87.104506 ↗
30. 10.1103/PhysRevB.83.17450610.1103/PhysRevB.83.174506 ↗
31. 10.1063/1.343547210.1063/1.3435472 ↗
32. 10.1143/JPSJ.78.06370210.1143/JPSJ.78.063702 ↗
33. 10.1038/nmat279510.1038/nmat2795 ↗
34. 10.1088/1367-2630/ab3d7510.1088/1367-2630/ab3d75 ↗
35. 10.1103/PhysRevB.93.05452210.1103/PhysRevB.93.054522 ↗
36. 10.1103/PhysRevB.80.17450910.1103/PhysRevB.80.174509 ↗
37. 10.1103/PhysRevB.81.02050910.1103/PhysRevB.81.020509 ↗
38. 10.1103/PhysRevB.81.18451110.1103/PhysRevB.81.184511 ↗
39. 10.1103/PhysRevB.81.22452010.1103/PhysRevB.81.224520 ↗
40. 10.1143/JPSJ.79.08471110.1143/JPSJ.79.084711 ↗
41. 10.1088/0953-2048/26/1/01501510.1088/0953-2048/26/1/015015 ↗
42. 10.1038/srep0458510.1038/srep04585 ↗
43. 10.7566/JPSJ.82.09370510.7566/JPSJ.82.093705 ↗
44. 10.7566/JPSJ.82.11500210.7566/JPSJ.82.115002 ↗
45. 10.1088/1361-6668/ab30c210.1088/1361-6668/ab30c2 ↗
46. 10.1143/JPSJ.77.04370510.1143/JPSJ.77.043705 ↗
47. 10.1103/PhysRevB.101.13451610.1103/PhysRevB.101.134516 ↗
48. 10.1109/TASC.2016.251558510.1109/TASC.2016.2515585 ↗
49. 10.7567/JJAP.56.04310110.7567/JJAP.56.043101 ↗
50. 10.1103/PhysRevB.80.14050710.1103/PhysRevB.80.140507 ↗
51. 10.1126/science.118739910.1126/science.1187399 ↗
52. 10.1016/j.physc.2011.05.01110.1016/j.physc.2011.05.011 ↗
53. 10.1103/PhysRevB.89.14451210.1103/PhysRevB.89.144512 ↗
54. 10.1038/srep3229010.1038/srep32290 ↗
55. 10.1088/1367-2630/11/7/07500710.1088/1367-2630/11/7/075007 ↗
56. 10.1103/PhysRev.147.28810.1103/PhysRev.147.288 ↗
57. 10.1103/PhysRevLett.124.10700110.1103/PhysRevLett.124.107001 ↗
58. 10.7567/APEX.6.04310110.7567/APEX.6.043101 ↗
59. 10.1103/PhysRevB.81.09451810.1103/PhysRevB.81.094518 ↗
60. 10.1103/PhysRevB.91.16510910.1103/PhysRevB.91.165109 ↗
61. 10.1103/PhysRevB.97.11515210.1103/PhysRevB.97.115152 ↗
62. 10.1088/0034-4885/75/11/11450210.1088/0034-4885/75/11/114502 ↗
63. 10.1126/sciadv.160237210.1126/sciadv.1602372 ↗
64. 10.1088/0034-4885/74/12/12450510.1088/0034-4885/74/12/124505 ↗
65. 10.1103/PhysRevLett.95.09700510.1103/PhysRevLett.95.097005 ↗
66. 10.1103/PhysRevB.84.18051410.1103/PhysRevB.84.180514 ↗
67. 10.1103/PhysRevB.79.01250610.1103/PhysRevB.79.012506 ↗
68. 10.1103/PhysRevLett.108.10700210.1103/PhysRevLett.108.107002 ↗