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V-type asteroids are bodies whose surfaces are constituted of basalt. In the Main Asteroid elt, most of these asteroids are assumed to come from the basaltic crust of asteroid (4) Vesta. This idea is mainly supported by (i) the fact that almost all the known V-type asteroids are un the same region of the belt as (4) Vesta, i. e., the inner belt (semi-major axis 2.1 < a <2.5 AU), (ii) the existence of a dynamical asteroid family associated to (4) Vesta, and (iii) the observational evidence of at least one large craterization event on Vesta´s surface. One V-type asteroid that is difficult to fit in this scenario is (1459) Magnya, located in the outer asteroid belt, i.e., too far away from (4) Vesta as to have a real possibility of coming from it. The recent discovery of the first V-type asteroid in the middle belt (2.5 < a < 2.8 AU), (21238) 1995 WV7 [Binzel et al., Bull. Am. Astron. Soc. 38, 627, 2006; Hammergren et al., ArXiv e-print, astro-ph/0609420, 2006], located at ~2.54 AU, raises the question of whether it came from (4) Vesta or not. In this paper, we present spectroscopic observations indicating the existence of another V-type asteroid at ~2.53 AU, (40521) 1999 RL95, and we investigate the possibility that these two asteroids evolved from the Vesta family to their present orbits by a semi-major axis drift due to Yarkovsky effect. The main problem with this scenario is that the asteroids need to cross the 3/1 mean motion resonance with Jupiter, which is highly unstable. Combining N-body numerical simulations of the orbital evolution, that include the Yarkovsky effect, with Monte Carlo models, we compute the probability that an asteroid of a given diameter D evolves from the Vesta family and crosses over the 3/1 resonance, reaching a stable orbit in the middle belt. Our results indicate that an asteroid like (21238) 1995 WV7 has a low probability (~1%) of having evolved through this mechanism due to its large size (D ~ 5 km), because the Yarkovsky effect is not sufficiently efficient for such large asteroids. However, the mechanism might explain the orbits of smaller bodies like (40521) 1999 RL95 (D ~ 3 km) with 70-100% probability, provided that we assume that the Vesta family formed > 3.5 Gy ago. We estimate the debiased population of V-type asteroids that might exist in the same region as (21238) and (40521) (2.5 < a <2.62 AU) and conclude that about 10 to 30% of the V-type bodies with D > 1 km may come from the Vesta family by crossing over the 3/1 resonance. The remaining 70-90% must have a different origin.