Geometrical Misalignment of the Disks in the HH 24 MMS Protobinary System

Details Geometrical Misalignment of the Disks in the HH 24 MMS Protobinary System Geometrical Misalignment of the Disks in the HH 24 MMS Protobinary System

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.6222k&link_type=abstract

American Astronomical Society, AAS Meeting #211, #62.22; Bulletin of the American Astronomical Society, Vol. 39, p.851

Astronomy and Astrophysics

Astronomy

Scientific paper

The HH 24 MMS protostellar system was observed in the 6.9 mm continuum with a high angular resolution (0.5 arcsec) using the Very Large Array. The spectral energy distribution suggests that the 6.9 mm flux of HH 24 MMS is almost entirely from dust. Our high-resolution image shows a small-scale structure that can be interpreted as two disks partially overlapped. The separation between them, sources 1 and 2, is about 0.9 arcsec or 360 AU. Both sources seems to be highly elongated. The 6.9 mm image and the spectrum suggest that HH 24 MMS may be a protostellar binary system. Total mass including the accretion disks and the inner protostellar envelope is about 1.4 Msun. Disk masses of sources 1 and 2 are 0.6 and 0.3 M&sun; respectively. The difference in the position angle of the two disks is about 45 degrees, which means that HH 24 MMS is a highly misaligned protobinary system. Theories of binary formation suggest that fragmentation of star-forming clumps can be induced either by rotation or by turbulence. The misalignment of the HH 24 MMS system suggests that turbulent fragmentation may be the formation mechanism relevant to wide binaries.

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