Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:0805.4263)
· References in the article
· Citations to the Article (5) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (7)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Possibility of Detecting Moons of Pulsar Planets through Time-of-Arrival Analysis
Authors:
Lewis, Karen M.; Sackett, Penny D.; Mardling, Rosemary A.
Affiliation:
AA(School of Mathematical Sciences, Monash University, Clayton, Victoria 3800, Australia; , .), AB(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo Observatory, Cotter Road, Weston, ACT 2611, Australia; .), AC(School of Mathematical Sciences, Monash University, Clayton, Victoria 3800, Australia; , .)
Publication:
The Astrophysical Journal, Volume 685, Issue 2, pp. L153-L156. (ApJL Homepage)
Publication Date:
10/2008
Origin:
UCP
ApJ Keywords:
Stars: Planetary Systems, Stars: Pulsars: General, Stars: Pulsars: Individual: Alphanumeric: PSR B1620-26, Stars: Oscillations
DOI:
10.1086/592743
Bibliographic Code:
2008ApJ...685L.153L

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 (2np-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 sinI[9(MpMm)/16(Mp+Mm)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.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints