  In this paper we study the location and stability of the collinear Lagrangian
points for the RTBP for the case in which one of the primary bodies is
radiating and the other is oblate. We consider the effect of Poynting-Roberson
drag and investigate how the location and stability of the Lagrangian points
change with changes in the radiation parameter $\beta$ and oblateness $a$. We
apply our results to ten exoplanet systems -- CoRoT-2~b, TOI-1278~b,
HAT-P-20~b, Kepler-75~b, WASP- 89~b, TIC 172900988~b, NGTS 9~b, LP 714 - 47~b,
WASP- 162~b and XO- 3~b, data of which has been taken from NASA exoplanet
archives, with the aim of finding locations in these exoplanet systems where
one can detect asteroids, primodial material or seeds where planet formation
can take place. We find that the location of the collinear Lagrangian points
changes with variation in radiation pressure and oblateness. Further, for all
the ten planetary systems, studied in this paper, the Lagrangian points are
unstable and can be locations where we expect to find minor planets, asteroids
or debris. The unstability of the the Lagrangian points can be a possible cause
of relocation and migration of planetesimals.
