# 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.