Rotational Velocities of Individual Components in Very Low Mass Binaries

TL;DR

This study measures rotational velocities of individual components in very low mass binaries, revealing rapid rotation, possible inclination effects, and dynamical interactions that influence their evolution.

Contribution

It provides new measurements of rotational velocities for VLM binary components and explores their implications for binary formation and dynamical evolution.

Findings

Most VLM objects are rapid rotators with vsini > 10 km/s.

Binary components often have significantly different rotational velocities.

Dynamical interactions may cause misalignments and influence binary evolution.

Abstract

We present rotational velocities for individual components of eleven very low mass (VLM) binaries with spectral types between M7 and L7.5. These results are based on observations taken with the near-infrared spectrograph, NIRSPEC, and the Keck II laser guide star adaptive optics (LGS AO) system. We find that the observed sources tend to be rapid rotators (vsini > 10 km/s), consistent with previous seeing-limited measurements of VLM objects. The two sources with the largest vsini, LP 349-25B and HD 130948C, are rotating at ~30% of their break up speed, and are among the most rapidly rotating VLM objects known. Furthermore, five binary systems, all with orbital semi-major axes <3.5 AU, have component vsini values that differ by greater than 3sigma. To bring the binary components with discrepant rotational velocities into agreement would require the rotational axes to be inclined with respect to each other, and that at least one component is inclined with respect to the orbital plane. Alternatively, each component could be rotating at a different rate, even though they have similar spectral types. Both differing rotational velocities and inclinations have implications for binary star formation and evolution. We also investigate possible dynamical evolution in the triple system HD 130948A-BC. The close binary brown dwarfs B and C have significantly different vsini values. We demonstrate that components B and C could have been torqued into misalignment by the primary star, A, via orbital precession. Such a scenario can also be applied to another triple system in our sample, GJ 569A-Bab. Interactions such as these may play an important role in the dynamical evolution of very low mass binaries. Finally, we note that two of the binaries with large differences in component vsini, LP 349-25AB and 2MASS 0746+20AB, are also known radio sources.