TY - JOUR

T1 - Possibility of detecting moons of pulsar planets through time-of-arrival analysis

AU - Lewis, Karen M.

AU - Sackett, Penny D.

AU - Mardling, Rosemary A.

PY - 2008

Y1 - 2008

N2 - The perturbation caused by planet-moon binarity on the time-of-arrival signal of a pulsar with an orbiting planet is derived for the case in which the orbits of the moon and the planet-moon barycenter are both circular and coplanar. The signal consists of two sinusoids with frequency (2n p-3nb) and (2np-nb), where np and nb are the mean motions of the planet and moon around their barycenter, and the planet-moon system around the host, respectively. The amplitude of the signal is the fraction sin I [9(MpMm)/16(Mp + M m)2][r/R]5 of the system crossing time R/c, where Mp and Mm are the masses of the planet and moon, r is their orbital separation, R is the distance between the host pulsar and planet-moon barycenter, I is the inclination of the orbital plane of the planet, and c is the speed of light. The analysis is applied to the case of PSR B1620-26b, a pulsar planet, to constrain the orbital separation and mass of any possible moons. We find that a stable moon orbiting this pulsar planet could be detected, if its mass were >5% of its planet's mass, and if the planet-moon distance were-2% of the planet-pulsar separation.

AB - The perturbation caused by planet-moon binarity on the time-of-arrival signal of a pulsar with an orbiting planet is derived for the case in which the orbits of the moon and the planet-moon barycenter are both circular and coplanar. The signal consists of two sinusoids with frequency (2n p-3nb) and (2np-nb), where np and nb are the mean motions of the planet and moon around their barycenter, and the planet-moon system around the host, respectively. The amplitude of the signal is the fraction sin I [9(MpMm)/16(Mp + M m)2][r/R]5 of the system crossing time R/c, where Mp and Mm are the masses of the planet and moon, r is their orbital separation, R is the distance between the host pulsar and planet-moon barycenter, I is the inclination of the orbital plane of the planet, and c is the speed of light. The analysis is applied to the case of PSR B1620-26b, a pulsar planet, to constrain the orbital separation and mass of any possible moons. We find that a stable moon orbiting this pulsar planet could be detected, if its mass were >5% of its planet's mass, and if the planet-moon distance were-2% of the planet-pulsar separation.

KW - General

KW - Individual (PSR b1620-26)

KW - Oscillations

KW - Planetary systems

KW - Pulsars

KW - Stars

UR - http://www.scopus.com/inward/record.url?scp=67649647525&partnerID=8YFLogxK

U2 - 10.1086/592743

DO - 10.1086/592743

M3 - Article

SN - 0004-637X

VL - 685

SP - L153-L156

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 PART 2

ER -