A Photometric Study of Stars in the MBM 12 Association

Abstract

We have monitored four fields containing nine previously identified members of the MBM 12 association to search for photometric variability and periodicity in these pre-main sequence stars. Seven of the nine are found to be variable and definite periodicity (of 1.2, 2.6 and 6.2 days) is found for three of them, including the classical T Tauri star LkH-alpha 264. Two other members are possibly periodic but each requires confirmation. In addition, a "field" star that is associated with the X-ray source RX J0255.9+2005 was discovered to be a variable with a period of 4.2 days. Our results indicate that the photometric variability characteristics of the known MBM 12 association members are typical of what is found in ~few My old stellar groups such as IC 348, supporting arguments for a similar age. In particular, there is a mix of periodic and non-periodic variables with typical amplitudes (in Cousins I) of 0.1-0.5 mag, in addition to a small number of larger amplitude variables. The periods, as a group, are somewhat shorter than in IC 348 but when allowance is made for the known dependence of period on mass in pre-main sequence stars the difference may not be significant. Our data confirm and illustrate the value of photometric monitoring as a tool for identifying likely association members and for studying rotation in extremely young stellar groups.