Magnetic braking saturates: evidence from the orbital period distribution of low-mass detached eclipsing binaries from ZTF

We constrain the orbital period (P-orb) distribution of low-mass detached main-sequence eclipsing binaries (EBs) with light-curves from the Zwicky Transient Facility (ZTF), which provides a well-understood selection function and sensitivity to faint stars. At short periods (P-orb less than or similar to 2 d), binaries are predicted to evolve significantly due to magnetic braking (MB), which shrinks orbits and ultimately brings detached binaries into contact. The period distribution is thus a sensitive probe of MB. We find that the intrinsic period distribution of low-mass (0.1 less than or similar to M-1/M-circle dot < 0.9) binaries is basically flat (dN/dP(orb) proportional to P-orb(0))) from P-orb = 10 d down to the contact limit. This is strongly inconsistent with predictions of classical MB models based on the Skumanich relation, which are widely used in binary evolution calculations and predict dN/dP(orb) proportional to P-orb(7/3) at short periods. The observed distributions are best reproduced by models in which the magnetic field saturates at short periods with a MB torque that scales roughly as ((J) over dot) proportional to P-orb(-1), as opposed to ((J) over dot) proportional to P-orb(-3) in the standard Skumanich law. We also find no significant difference between the period distributions of binaries containing fully and partially convective stars. Our results confirm that a saturated MB law, which was previously found to describe the spin-down of rapidly rotating isolated M dwarfs, also operates in tidally locked binaries. We advocate using saturated MB models in binary evolution calculations. Our work supports previous suggestions that MB in cataclysmic variables (CVs) is much weaker than assumed in the standard evolutionary model, unless mass transfer leads to significant additional angular momentum loss in CVs.

Automated summary

We use light-curves from the ZTF to constrain the orbital period distribution of low-mass detached main-sequence eclipsing binaries. Our findings suggest that the intrinsic period distribution of these binaries is inconsistent with classical magnetic braking models, and supports the idea of a saturated magnetic field at short periods. We also find that the period distribution is not significantly affected by the convective properties of the stars in the binaries.