Observations of Young Clusters . III . NGC 2264 and the Orion Flanking Fields

Chandra observations of solar-like pre-main sequence (PMS) stars in the Orion Flanking Fields (age ∼1 Myr) and NGC 2264 (∼3 Myr) are compared with the results of the COUP survey of similar objects in the ONC (∼0.5 Myr). The correlations between log L x and mass found for PMS stars on convective tracks in these clusters are consistent with the relationships found for the ONC, indicating little change in the median values of either log L x or log L x /L bol during the first ∼3-5 Myr of evolution down convective tracks. The fraction of stars with extreme values of L x , more than 10 times higher than the average for a given L bol or with log L x /L bol greater than the canonical saturation value of −2.9, is however larger by a factor of two in the younger ONC when compared with the Orion FF and NGC 2264. PMS stars in NGC 2264 on radiative tracks have L x /L bol values that are systematically lower by a factor of ∼10 times than those found for stars of similar – 2 – mass on convective tracks. The dramatic decrease in flux from convective to radiative phases of PMS evolution is likely related to major structural changes which influence the efficiency of magnetic field generation and thus the level of magnetic activity. As in the ONC, we find that stars with measured periods have, on average, higher X-ray luminosities. However, there is a wide range in L x and L x /L bol for both periodic and non-periodic stars of similar mass. Among stars with measured periods, the level of X-ray emission does not correlate with the rotation rate. For this data set, we find no statistically significant correlation between X-ray flux and (a) the presence or absence of circumstellar accretion disks, or (b) disk accretion rates as assessed from ultraviolet excesses.