SIMBAD references

We have photometrically monitored ∼3600 young, low-mass stars in four 45'x45' fields in the outer Orion Nebula cluster, surrounding but not including the Trapezium region. The 281 periodic variables we find do not produce the expected bimodal distribution of rotation periods. There is no unambiguous correlation of period with I_C-K_s, H-K_s_, and U-V color excesses or more indirect disk indicators; the slowest rotators are not necessarily the disk candidates, and the disk candidates are not necessarily the slow rotators, regardless of how one defines a disk candidate. To the extent that the small numbers allow, the disk candidates represent a constant fraction of the total sample to P=15 days, beyond which there are no disk candidates, inconsistent with the hypothesis that the more slowly rotating stars are more likely to have disks. We find an intriguing relationship between specific angular momentum (j) and some excesses, namely, H-K_s excesses and the strongest U-V excesses; whereas stars are found with j values ranging over ∼10⁶-10⁸ km².s^–1, disk candidates with these excesses are restricted to 10^6.5 km².s^–1<j<10^7.5 km².s^–1. A similar relationship is not found for the I_C-K_s disk candidates, or in the less excessive U-V candidates. There is no clear correlation between signal amplitude and period or logj. Other investigators have found differences in period distributions for stars more and less massive than 0.25 M_☉; we find ambiguous evidence for differences in distributions of P and no difference in those of logj on either side of this boundary, although for stars more massive than ∼0.6 M_☉, values appear to cluster around j=10⁷ km².s^–1. When comparing the logj distribution derived here with those for other clusters, we find that it is consistent with a population of stars draining angular momentum into disks. We conclude that disk locking may be operating, but it is not the complete solution to the problem of angular momentum distributions in young stars. We find weak (1.5-2 σ) evidence for a change in stellar structure, spot coverage, and/or disk characteristics for stars redder than V-I_C∼2.5 (type ∼M3, ∼0.25 M_☉). We find that at least ∼10% of the stars have identical light curves (shape and phase) between the two seasons of our observations, suggesting that the lifetime of the photospheric disturbance causing periodic modulations in these stars is at least a year.