Searching for gravitational waves from known pulsars at once and twice the spin frequency

Abstract

The existence of a superfluid core in the interior of a rotating neutron star may have an influence on its gravitational wave emission. In addition to the usually-assumed pure quadrupole radiation with the gravitational wave frequency at twice the spin frequency, a frequency of rotation itself may also be present in the gravitational wave spectrum. We study the parameters of a general model for such emission, compare it with previously proposed, simpler models, discuss the feasibility of the recovery of the stellar parameters and carry out the Monte Carlo simulations to test the performance of our estimation method.

16 pages, 11 figures, CQG accepted

References in corpus (2)

• Upper limits on gravitational wave emission from 78 radio pulsars
• Fitting Pulsar Wind Tori. II. Error Analysis and Applications

Cited by in corpus (8)

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• Searches for continuous gravitational waves from neutron stars: A twenty-year retrospective
• Parameter choices and ranges for continuous gravitational wave searches for steadily spinning neutron stars
• First results and future prospects for dual-harmonic searches for gravitational waves from spinning neutron stars
• Tracking continuous gravitational waves from a neutron star at once and twice the spin frequency with a hidden Markov model
• A new estimation method for mass of an isolated neutron star using gravitational waves
• Searches for continuous gravitational waves from young supernova remnants in the early third observing run of Advanced LIGO and Virgo
• Determination of mass of an isolated neutron star using continuous gravitational waves with two frequency modes: an effect of a misalignment angle