Gravitational Waves from Accreting Neutron Stars undergoing Common-Envelope Inspiral

Abstract

The common envelope phase is a likely formation channel for close binary systems containing compact objects. Neutron stars in common envelopes accrete at a fraction of the Bondi-Hoyle-Lyttleton accretion rate, since the stellar envelope is inhomogeneous, but may still be able to accrete at hyper-critical rates (though not enough to become black holes). We show that common envelope systems consisting of a neutron star with a massive primary may be gravitational wave sources detectable in the Advanced LIGO band as far away as the Magellanic Clouds. To characterize their evolution, we perform orbital integrations using 1D models of $12M_{\odot }$ and $20M_{\odot }$ primaries, considering the effects of density gradient on the accretion onto the NS and spin evolution. From the range of possible accretion rates relevant to common envelope evolution, we find that these systems may be louder gravitational wave sources than low-mass X-ray binaries like Sco X-1, which are currently the target of directed searches for continuous GWs. We also find that their strain amplitude signal may allow for novel constraints on the orbital separation and inspiral timescale in common envelopes when combined with pre-common envelope electromagnetic observations.

20 pages, 9 figures, accepted to ApJ

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• The maximum accreted mass of recycled pulsars
• Optimizing the third generation of gravitational-wave observatories for Galactic astrophysics
• Gravitational Radiation from Close Binaries with Time-Varying Masses
• The Role of Strong Gravity and the Nuclear Equation of State on Neutron-Star Common-Envelope Accretion
• Gravitational Waves from Supernova Mass Loss and Natal Kicks in Close Binaries
• Constraints on r-modes and mountains on millisecond neutron stars in binary systems