Computer Science
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sptz.prop30434b&link_type=abstract
Spitzer Proposal ID #30434
Computer Science
Scientific paper
We have discovered, through optical radial velocity measurements, the first confirmed close white dwarf + brown dwarf binary. Since the system is double-lined, we are able to determine the companion's mass as 0.055+/-0.005Msun, placing it firmly in the substellar regime. The orbital period is 115 minutes, and no mass transfer is taking place. Therefore, the brown dwarf must have survived a previous common envelope phase of evolution, during which it was engulfed by the red giant precursor's envelope. The discovery of this system raises the possibility that lower mass substellar objects, including giant planets, may also survive the red giant phase to become close companions to white dwarfs. Indeed, they may accrete a significant amount of mass during this phase. A small excess K band flux above that expected from the white dwarf is found in 2MASS photometry, enabling us to place a tentative upper limit on the brown dwarf's spectral type as mid-L. We request Spitzer IRAC photometry of the binary to more accurately determine the brown dwarf's spectral type (to one subclass), and to measure precise fluxes and an effective temperature. These data will be used to understand how this unique binary has been created: has the brown dwarf accreted a significant amount of matter during the common envelope phase? Was it originally a lower mass brown dwarf or even a giant planet? If yes, this has implications for the fate of all planets and brown dwarfs in the post main-sequence phase of evolution.
Brinkworth Carolyn
Burleigh Matt
Dobbie Paul
Hoard Donald
Maxted Pierre
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