Effect of radiation on the stability of equilibrium points in the binary stellar systems: RW-Monocerotis, Krüger 60

Abstract

We have studied the stability of location of various equilibrium points of a passive micron size particle in the field of radiating binary stellar system within the framework of circular restricted three body problem. Influence of radial radiation pressure and Poynting-Robertson drag (PRdrag) on the equilibrium points and their stability in the binary stellar systems RW-Monocerotis and Krüger-60 has been studied. It is shown that both collinear and off axis equilibrium points are linearly unstable for increasing value of β 1 (ratio of radiation to gravitational force of the massive component) in presence of PR-drag for the binary systems. Further we find that out of plane equilibrium points (L i , i = 6, 7) may exists for range of values of β 1 > 1 for these binary systems in the presence of PR-drag. Our linear stability analysis shows that the motion near the equilibrium points L 6,7 of the binary systems is unstable both in the absence and presence of PR-drag.

On out of plane equilibrium points in photo-gravitational restricted three-body problem

“…Further, β i corresponds to the ratio of force due to radiation and the gravitational force of the i-th binary component (cf. Das et al 2008b) from the i-th binary component. It is important to note that for solar dust particles less than a μm comprising spherical silicate BPCA, carbon BPCA, silicate compact, asteroidal dust, young and cometary dust grains, β may vary in the range ∼ 10 −2 -5.0 (cf.…”

“…Besides the classical coplanar equilibrium points (cf. Das et al 2008b), it is possible to have out of plane equilibrium points exclusively due to radiation from binary components. Such points do not have any classical analogue.…”

“…Since then several authors (cf. Chernikov 1970;Perezhogin 1976;Scheurman 1980;Simmons et al 1985;Ragos & Zagouras 1988;Murray 1994;Ragos et al 1995;Roman 2001;Kunitsyn & Chudayeva 2003;Kushvah & Ishwar 2004;Das et al 2008a) extended the work to understand various issues related to the dynamics of a particle around radiating primaries. However, majority of these works involve the use of independent quantities q 1 = 1 − β 1 and q 2 = 1 − β 2 , where β i corresponds to the ratio of radiation pressure force to the gravitational force of i-th binary component.…”

Linear stability of equilibrium points in the generalized photogravitational Chermnykh’s problem

“…The stability of triangle libration points in generalized restricted circular three-body problem has been studied by Beletsky and Rodnikov (2008). Das et al (2008) examined the stability of location of various equilibrium points of a passive micron size particle in the field of radiating binary stellar system within the framework of circular restricted three body problem.…”

Effect of three-body interaction on the number and location of equilibrium points of the restricted three-body problem

“…Such models are the photogravitational CR3BP where the primaries are considered to be radiation sources (e.g. Schuerman 1980;Simmons et al 1985;Ragos and Zagouras 1993;Das et al 2008) or the CR3BP which takes into account the oblateness of the primaries (e.g. Sharma and Subba Rao 1975;Oberti and Vienne 2003;Arredondo et al 2012;Douskos et al 2012) as well as combination of them (e.g.…”