Possibility of Detection of Exomoons with Inclined Orbits Orbiting Pulsar Planets Using the Time-of-Arrival Analysis
Dublin Core
Title
Possibility of Detection of Exomoons with Inclined Orbits Orbiting Pulsar Planets Using the Time-of-Arrival Analysis
Description
The perturbation caused by planet-moon binarity on the time-of-arrival
(TOA) signal of a pulsar with an orbiting planet is derived for the case of the
orbit of the planet-moon system inclined of an angle α with respect to
the plane of the orbit of the planet-moon barycenter around the pulsar.
We also consider both the orbits of the moon and the planet-moon barycenter as circular.
The signal consists of three sinusoids with frequency, respectively, of (2np−3nb), (2np−nb), and (2np−3nb), where np and nb are, respectively, 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 sinI[9(Mp/Mm)/16(Mp+Mm)2][r/R]5(5 sin2α/3−2sinα/3−2 cos2α/9) of the system crossing time R/c, where Mp and Mm are, respectively, the mass of the planet and the mass of the 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.
(TOA) signal of a pulsar with an orbiting planet is derived for the case of the
orbit of the planet-moon system inclined of an angle α with respect to
the plane of the orbit of the planet-moon barycenter around the pulsar.
We also consider both the orbits of the moon and the planet-moon barycenter as circular.
The signal consists of three sinusoids with frequency, respectively, of (2np−3nb), (2np−nb), and (2np−3nb), where np and nb are, respectively, 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 sinI[9(Mp/Mm)/16(Mp+Mm)2][r/R]5(5 sin2α/3−2sinα/3−2 cos2α/9) of the system crossing time R/c, where Mp and Mm are, respectively, the mass of the planet and the mass of the 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.
Creator
Antonio Pasqua
Khudhair A. Assaf
Publisher
Advances in Astronomy
Date
2014
Rights
Copyright © 2014 Antonio Pasqua and Khudhair A. Assaf.
Language
en
Type
Research Article
Identifier
https://doi.org/10.1155/2014/450864
Collection
Citation
Antonio Pasqua and Khudhair A. Assaf, “Possibility of Detection of Exomoons with Inclined Orbits Orbiting Pulsar Planets Using the Time-of-Arrival Analysis,” Open Access Journal Archives, accessed June 3, 2023, http://oajour.info/items/show/886.