Multiplicity of Young Brown Dwarfs in Cha I
- Autor(en)
- Viki Joergens, Eike Guenther, Ralph Neuhäuser, Fernando Comerón, Nuria Huélamo, João Alves, Wolfgang Brandner
- Abstrakt
How frequent are brown dwarf binaries? Do brown dwarfs have planets? Are
current theoretical pre-main-sequence evolutionary tracks valid down to
the substellar regime? - Any detection of a companion to a brown dwarf
takes us one step forward towards answering these basic questions of
star formation. We report here on a search for spectroscopic and visual
companions to young brown dwarfs in the Cha I star forming cloud. Based
on spectra taken with UVES at the VLT, we found significant radial
velocity (RV) variations for five bona-fide and candidate brown dwarfs
in Cha I. They can be caused by either a (substellar or planetary)
companion or stellar activity. A companion causing the detected RV
variations would have about a few Jupiter masses. We are planning
further UVES observations in order to explore the nature of the detected
RV variations. We also found that the RV dispersion is only ˜2
km/s indicating that there is probably no run-away brown dwarf among
them. Additionally a search for companions by direct imaging with the
HST and SOFI (NTT) has yielded to the detection of a few companion
candidates in larger orbits.
- Organisation(en)
- Institut für Astrophysik
- Externe Organisation(en)
- European Southern Observatory (Germany), Max-Planck-Institut für extraterrestrische Physik, Thüringer Landessternwarte Tautenburg
- Seiten
- 127
- DOI
- https://doi.org/10.1007/10856518_16
- Publikationsdatum
- 2002
- ÖFOS 2012
- 103004 Astrophysik
- Link zum Portal
- https://ucris.univie.ac.at/portal/de/publications/multiplicity-of-young-brown-dwarfs-in-cha-i(20c03527-2252-437e-bcc4-0cdfd8b1f44a).html