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Possibility of Detecting Moons of Pulsar Planets Through Time-of-Arrival Analysis | Karen M. Lewis
; Penny D. Sackett
; Rosemary A. Mardling
; | Date: |
28 May 2008 | Abstract: | 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 - 3n_b) and (2n_p - n_b
), where n_p and n_b 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 equal to the fraction sin I[9(M_p M_m)/16(M_p +
M_m)^2] [r/R]^5 of the system crossing time R/c, where M_p and M_m are the 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 B1620-26 b, 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 the moon had a separation of
about one fiftieth of that of the orbit of the planet around the pulsar, and a
mass ratio to the planet of ~5% or larger. | Source: | arXiv, 0805.4263 | Services: | Forum | Review | PDF | Favorites |
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