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| Paper: |
Disk-Rotation Connection: Very Low Mass Stars and Brown Dwarfs |
| Volume: |
448, 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun |
| Page: |
721 |
| Authors: |
Rodriguez-Ledesma, M. V.; Mundt, R.; Eislöffel, J. |
| Abstract: |
At present, how young pre-main sequence (PMS) objects effectively lose angular momentum is still not fully understood. Nevertheless, irrespective of an specific model, there is a general consensus that circumstellar accretion disks are somehow responsible for the removal of angular momentum, and therefore accreting stars should on average rotate slower than non-accreting ones. Although, many authors have investigated a rotation-disk connection in low mass pre-main sequence stars, this connection was not investigated as yet in the brown dwarf (BD) regime because of the very few samples available. Our investigation extends well down into the substellar regime, with a total sample of 732 very low mass objects, 81 of which are BDs candidates in the Orion Nebula Cluster (ONC), with measured rotational periods.
We found a rotation-disk correlation in the low and very low mass stars of the sample, in which objects with NIR excess tend to rotate slower than objects without NIR excess. Interestingly, we found no correlation in the substellar regime. A tight correlation between the peak-to-peak (ptp) amplitude of the rotational modulation and the NIR excess was found however for all objects. |
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