Current and secular accretion rates of EX Hydrae

We report an observed accretion rate of Ṁ₁ = (3.86 ± 0.60) × 10⁻¹¹ M_⊙ yr⁻¹ for the white dwarf in the short-period, intermediate polar EX Hya. This result is based upon the accretion-induced 4π-averaged energy flux from 2.45 μm to 100 keV and the corresponding luminosity at the Gaia distance of 56.77 pc. Our result is in perfect agreement with the theoretical mass transfer rate from the secondary star induced by gravitational radiation (GR) and the spin-up of the white dwarf, − Ṁ₂ = (3.90 ± 0.35) × 10⁻¹¹ M_⊙ yr⁻¹; 24% of it is caused by the spin-up. The agreement indicates that mass transfer is conservative. The measured Ṁ₁ obviates the need for angular momentum loss (AML) by any process other than GR. We complemented this result with an estimate of the mean secular mass transfer rate over ∼10⁷ yr by interpreting the non-equilibrium radius of the secondary star in EX Hya based on published evolutionary calculations. This suggests a time-averaged mass transfer rate enhanced over GR by a factor f_GR ≳ 2. Combined with the present-day lack of such an excess, we suggest that an enhanced secular AML is due to an intermittently active process, such as the proposed frictional motion of the binary in the remnants of nova outbursts. We argue that EX Hya, despite its weakly magnetic nature, has evolved in a very similar way to non-magnetic CVs. We speculate that the discontinuous nature of an enhanced secular AML may similarly apply to the latter.

Full Table 1 is available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/687/A273