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Hurley, Tout & Pols (2002)

San Diego State University

Abstract (paraphrased)

Presents the Binary Star Evolution (BSE) rapid population-synthesis algorithm, the binary companion to the single-star (SSE) formulae of Hurley, Pols & Tout (2000). On top of single-star evolution it adds the physics of interacting binaries: mass transfer and Roche-lobe overflow, common-envelope evolution, gravitational-radiation and magnetic-braking angular-momentum loss, and — central to its use here — tidal circularisation and synchronisation of eccentric, non-corotating orbits. Using the equilibrium-tide (convective damping) and dynamical-tide (radiative damping) prescriptions, the paper quantifies the systematic effect of tidal friction on synthesised binary populations and shows that orbits generally circularise before Roche-lobe overflow.

The tidal-circularisation timescale (Eqs. 28–29, 41, verified against the PDF)

For stars with convective envelopes (equilibrium tide), the circularisation rate is (Eq. 28)

1τcirc=212(kT) ⁣cq2(1+q2)(Ra)8,\frac{1}{\tau_{\rm circ}} = \frac{21}{2}\left(\frac{k}{T}\right)_{\!c}\,q_2\,(1 + q_2)\, \left(\frac{R}{a}\right)^{8},

with q2=m/Mq_2 = m/M the companion-to-primary mass ratio, RR the (primary) stellar radius, aa the semi-major axis, and (k/T)c(k/T)_c the apsidal-motion-constant / damping-timescale factor set by the convective eddy turnover (Eq. 30–31, after Rasio et al. 1996). Hurley et al. write it in the equivalent Rasio form (Eq. 29)

1τcirc=fconvτconvMenvMq2(1+q2)(Ra)8.\frac{1}{\tau_{\rm circ}} = \frac{f_{\rm conv}}{\tau_{\rm conv}}\,\frac{M_{\rm env}}{M}\, q_2\,(1 + q_2)\,\left(\frac{R}{a}\right)^{8}.

For stars with radiative envelopes (dynamical tide, after Zahn 1977) the scaling is steeper in R/aR/a (Eq. 41):

1τcirc=212(GMR3)1/2q2(1+q2)11/6E2(Ra)21/2.\frac{1}{\tau_{\rm circ}} = \frac{21}{2}\left(\frac{GM}{R^{3}}\right)^{1/2} q_2\,(1 + q_2)^{11/6}\,E_2\,\left(\frac{R}{a}\right)^{21/2}.

The key physics for progenax is the very strong (R/a)8(R/a)^8 dependence (convective case): the circularisation rate plummets with separation, so only short-period orbits are tidally circularised within the relevant lifetimes. This is exactly the schematic τcirc(a/R)8/[q(1+q)]\tau_{\rm circ} \sim (a/R_\star)^8 / [q(1+q)] used in the eccentricity chapter — the convective-envelope (equilibrium-tide) form, inverted.

Use in progenax

Notes

progenax uses Hurley+2002 only for the scaling intuition behind tidal circularisation — the (R/a)8(R/a)^8 law that makes circularisation a short-period phenomenon — not as an implemented tidal-evolution integrator. A full BSE-style tidal-evolution treatment (and the stellar-evolution-aware Roche radius needed for evolved-star cutoffs) is a planned startrax coupling. The single-star formulae underlying BSE are Hurley, Pols & Tout (2000).

References
  1. Hurley, J. R., Tout, C. A., & Pols, O. R. (2002). Evolution of binary stars and the effect of tides on binary populations. Monthly Notices of the Royal Astronomical Society, 329, 897–928. 10.1046/j.1365-2966.2002.05038.x