gzipped tar file of low- and high-resolution figures (2 x 10 jpg)

Caption: Plots of the cyclic models found from ASAS-3 (blue line) and ASAS-SN (red line) data.

Although the cycles for GJ 285 and GJ 406 were not listed in bold font in the paper's Table 1 to indicate "well defined" cycles because their L-S periods (see Figure sets for Figures 3 and Figures 4) were longer than the separate monitoring periods for ASAS and ASAS-SN (and the magnitude scales of the two data sets were not cross-calibrated so the data could not reliably be combined), one can see that both stars likely do have cycles, of roughly 9.5 years for GJ 285 and ~16 years for GJ 406 (Wolf 359, CN Leo).

Update May 2026: A more complete set of optical photometry on GJ 551/Proxima was analyzed in Wargelin et al. (2024), which included corrections for time dependent contamination by nearly stars caused by Proxima's proper motion. Along with X-ray and near-UV data, the newer work provides firm evidence for a ~7 year cycle.

In contrast, corrections for proper motion/stellar contamination in the light curve for GJ 406/Wolf 359 show that the apparent cycle is an artifact, and that the star's brightness is essentially constant (Wargelin et al., in preparation).

GJ 234	GJ 273	GJ 285	GJ 358
GJ 406	GJ 447	GJ 628	GJ 729
GJ 849	GJ 551/Proxima