Pith. sign in

REVIEW 3 cited by

Tidal evolution of eccentric orbits in massive binary systems; a study of resonance locking

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv astro-ph/9909073 v1 pith:IY5M4ZGF submitted 1999-09-03 astro-ph

M.G. Witte , G.J. Savonije (University of Amsterdam) This is my paper · ORCID
classification astro-ph
keywords orbitaltidalevolutionresonancelockingbinarystarcalculations
verification ladder T0 review T1 audit T2 compute T3 formal
0 comments
read the original abstract

We study the tidal evolution of a binary system consisting of a 1.4 Msun compact object in elliptic orbit about a 10 Msun uniformly rotating main sequence star for various values of the initial orbital parameters. We apply our previously published results of 2D non-adiabatic calculations of the non-radial g- and r-mode oscillations of the uniformly rotating MS star, and include the effects of resonant excitation of these modes in the tidal evolution calculations. A high orbital eccentricity enhances the effectiveness of the tidal interaction because of the large number of harmonic components of the tidal potential and the reduced orbital separation near periastron. By including the evolution of the MS star, especially of its rotation rate, many resonance crossings occur with enhanced tidal interaction. We analyse the phenomenon of resonance locking whereby a particular tidal harmonic is kept resonant with a stellar oscillation mode. Resonance locking of prograde g-modes appears an effective mechanism for orbital circularization of eccentric orbits. We consider the orbital evolution of the binary pulsar PSR J0045-7319 and conclude that resonance locking could explain the observed short orbital decay time of this system if the B-star spins in the direction counter to the orbital motion.

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Empirical Constraints on Tidal Dissipation in Exoplanet Host Stars

    astro-ph.EP 2025-01 conditional novelty 8.0 of 10

    The slope of the hot Jupiter decay-time distribution implies the stellar tidal quality factor scales as Q'* proportional to P^alpha with alpha between -4.33 and -2, favoring resonance locking.

  2. Prospects of Constraining Equilibrium Tides in Low-Mass Binary Stars

    astro-ph.SR 2025-07 conditional novelty 6.0 of 10

    Equilibrium tide strength Q cannot be inferred to order-of-magnitude precision from individual binary systems because of degeneracies with initial conditions.

  3. Testing tidal theory using Gaia binaries: the red giant branch

    astro-ph.SR 2025-01 conditional novelty 6.0 of 10

    F-mode tidal models reproduce late red-giant circularization but under-predict early red-giant circularization by about a factor of two, extending the main-sequence tidal discrepancy to the early red giant branch.

Pith tools