The general three-body problem studies the mutual interaction of three masses by determining their motion under the gravitational force using the Newton’s laws of motion and Newton’s law of gravitation. It is established that the closed form solution does not exist for the general three body problem. Further research introduced study of Circular Restricted Three-body problem. In this case one of the bodies is considered to have infinitesimal mass whose motion in circular orbits is influenced by the gravitational force of two massive primaries and the infinitesimal mass does not affect the motion of primaries. Lagrange proposed particular solution for this problem by considering a rotating frame such that the center of mass of the two primaries is taken as origin, the line joining the primary masses is x-axis, y-axis is taken perpendicular to x-axis in the plane of motion of primaries and z-axis is perpendicular to both x-axis and y-axis. The particular solution took the form of both collinear and non-collinear solutions. Associated with these solutions are the five points known as equilibrium points. Equilibrium points are the points where the forces acting on the body with infinitesimal mass in a rotating system are balanced hence there is no motion relative to the rotating system. Small particles like meteors, cosmic dust are considered as body with infinitesimal mass then their motion is influenced by the light pressure due to radiation emitted by the two primaries, hence along with the gravitational force another force due to light pressure was considered which paved way to the study of photogravitational three-body problem. In photogravitational circular restricted three body problem, the Infinitesimal mass experiences apart from the gravitational attractive force Fg, a repulsive force due to light pressure Fp, from both the primaries. In this paper, we present some valuable and interesting findings which have relevant real world applications. We prove the existence of out of plane equilibrium points for the Photo-Gravitational Circular Restricted three-body Problem and establish that they lie on a circle in a plane perpendicular to the plane of motion of primaries. It is also proved that for the equal values of radiation parameters which are less than 1, the triangles formed on either side of x-axis, by the line joining 1-μ and L4 or L5 having length r1, line joining μ and L4 or L5 having length r2 and the line joining the two primaries which are at unit distance is an isosceles triangle instead of being an equilateral triangle which was established by Lagrange in case of the non-photo-gravitational circular restricted three–body problem by formulating and solving the mathematical model of the photogravitational circular restricted three body problem.

1.
Y. A.
Chernikov
,
The Photogravitational Restricted Three-Body Problem
(
sovast
,
1970
),
176
.
2.
S.N.
Hasan
.: (Cosmic research,
1995
) pp
146
151
3.
A. L.
Kunitsyn
,
On The Stability Of Triangular Libration Points Of The Photogravitational Restricted Circular Three-Body Problem
(
Celestial Mechanics and DynamicalAstronomy
,
1978
).
4.
A. L.
Kunitsyn
,
On The Collinear Libration Points In The Photo-Gravitational Three-Body Problem
(
Celestial Mechanics and Dynamical Astronomy
,
1985
).
5.
C. W.
MeCracken
and
W. M.
Alexander
,:
1968
, in:
W. N.
Hess
and
G.D.
(eds),
Introduction to Space Science
,
2nd Edition
,
Gordon and Breach Science Publ
.,
New York
, Chap. 11, p.
447
.
6.
A. A.
Perezhogin
,
Stability of the sixth and seventh libration points in the photogravitational restricted circular three-body problem
. (
Soviet Astronomy Letters
,
1976
)
174
.
7.
J. H.
Poynting
,
The pressure of light.
(
The Inquirer,
1903
), pp
195
196
.
8.
V. V.
,
The restricted three-body problem, including radiation pressure
(
Astron. Zh,
1950
), pp
250
56
.
9.
V. V.
,
The space photogravitational restricted three-body problem
(
Astron. Zh,
1953
), pp.
265
273
.
10.
O.
Ragos
and
C.
Zagouras
,
The Zero Velocity Surfaces in the Photogravitational Restricted Three-Body Problem
. (
Earth, Moon, and Planets
,
1988
).
11.
O.
Ragos
and
C.
Zagouras
,
Periodic solutions about the `out of plane’ equilibrium points in the photogravitational restricted three-body problem
, (
Celestial Mechanics
,
1988
) pp.
135
154
.
12.
O.
Ragos
,
C.G.
Zagouras
, &
E.
Perdios
,
Periodic motion around stable collinear equilibrium   point in the photogravitational restricted problem of three bodies
, (
Astrophys Space Sci
,
1991
), pp.
313
336
.
13.
Ragos
,
O.
&
Zagouras
,
C.
:
1991
Celestial Mech. Dynam. Astr
50
,
325
.
14.
O.
Ragos
,
C.G.
Zagouras
,
On the existence of the “out of plane” equilibrium points in the photogravitational restricted three-body problem
, (
Astrophysics and space science
,
1993
).
15.
H. P.
Robertson
,
H. N.
Russell
,
Dynamical Effects of Radiation in the Solar System
, (
Monthly Notices of the Royal Astronomical Society
,
1937
), Pages
423
437
.
16.
D.W.
Schuerman
,
, (
Astrophys Space Sci
,
1972
) pp.
351
358
17.
D. W.
Schuerman
,
The restricted three-body problem including radiation pressure
, (
The Astrophysical Journal
,
1980
), pp.
337
342
.
18.
Simons
et al,
Celestial Mech.
35
,
145
.
19.
I.
Todoran
,
The photogravitational restricted three-body problem
. (
Astrophys Space Sci,
1994
), pp.
237
243
.
20.
S. P.
Wyatt
and
F. L.
Whipple
,
The Poynting-Robertson effect on meteor orbits,
(
Astrophys
,
1950
), pp.
134
141
.
This content is only available via PDF.