We present numerical results concerning the distances of the large trans-Neptunian objects (TNOs) Eris, 2005 FY9, 2003 EL61, Sedna, Orcus, Quaoar, Varuna, and 2002 AW197, computed by the so-called "global polytropic model". This model (Geroyannis 1993 [P1]; Geroyannis and Valvi 1993 [P2]) is based on the assumption of hydrostatic equilibrium for the solar system and its structure is described by the well-known Lane-Emden differential equation. A polytropic sphere of particular polytropic index n and radius R1 represents the central component S1 (in our case, the Sun) of a resultant polytropic configuration, of which further components are the polytropic spherical shells S2, S3, ..., defined by the pairs of radii (R1,R2), (R2,R3), ..., respectively. R1, R2, R3, ..., are the roots of the real part Re(theta(R)) of the complex Lane-Emden function theta(R), defined in the so-called "complex-plane strategy" (Geroyannis 1988). In this method, the complex Lane-Emden differential equation is solved numerically in the complex plane. Each polytropic shell can be considered as an appropriate place for a "planet" to be "born" and "live". This scenario has been studied numerically for the case of the planets of the solar system (P1, P2). In the present paper, we extend our computations far beyond Neptune, in order to include in our study the TNOs named above. REFERENCES: Geroyannis, V. S. 1988, Ap. J., 327, 273. Geroyannis, V. S. 1993, Earth, Moon, and Planets, 61, 131 [P1]. Geroyannis, V. S., and Valvi, F. N. 1993, Earth, Moon, and Planets, 63, 15 [P2].