2020ApJ...903....5L

While young stellar objects sometimes undergo bursts of accretion, these bursts usually occur sporadically, making them challenging to study observationally and to explain theoretically. We build a schematic description of cyclical bursts of the young stellar object EC 53 (also known as V371 Ser) using near-IR and submillimeter monitoring obtained over six cycles, each lasting ≃530 days. EC 53 brightens over 0.12 yr by 0.3 mag at 850 µm, by 2 mag at 3.35 µm, and by 1.5 mag at near-IR wavelengths, to a maximum luminosity consistent with an accretion rate of ∼8 x 10^–6 M_☉ yr^–1. The emission then decays with an e-folding timescale of ~0.74yr until the accretion rate is ∼1 x 10^–6 M_☉ yr^–1. The next eruption then occurs, likely triggered by the buildup of a ∼5 x 10^–6 M_☉ mass in the inner disk, enough for it to become unstable and drain onto the star. Just before outburst, when the disk is almost replenished, the near-IR colors become redder, indicating an increase in the geometrical height of the disk by this mass buildup. The reddening disappears soon after the initial burst, as much of the mass is drained from the disk. We quantify physical parameters related to the accretion process in EC 53 by assuming an α-disk formulation, constrained by the observed disk properties and accretion rate. While we can only speculate about the possible trigger for these faithful eruptions, we hope that our quantified schematic will motivate theorists to test the hypothesized mechanisms that could cause the cyclical buildup and draining of mass in the inner disk.