Compact protoplanetary disks around the stars of a young binary system

Details Compact protoplanetary disks around the stars of a young binary system Compact protoplanetary disks around the stars of a young binary system

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998natur.395..355r&link_type=abstract

Nature, Volume 395, Issue 6700, pp. 355-357 (1998).

Astronomy and Astrophysics

Astronomy

128

Scientific paper

Planet formation is believed to occur in the disks of gas and dust that surround young solar-type stars. Most stars, however, form in multiple systems, where the presence of a close companion could affect the structure of the disk and perhaps interfere with planet formation. It has been difficult to investigate this because of the resolution needed. Here we report interferometric observations (at a wavelength of 7mm) of the core of the star-forming region L1551. We have achieved a linear resolution of seven astronomical units (less than the diameter of Jupiter's orbit). The core of L1551 contains two distinct disks, with a separation of 45AU these appear to be associated with a binary system. Both disks are spatially resolved, with semi-major axes of about 10AU, which is about a factor of ten smaller than disks around isolated stars. The disk masses are of order 0.05 solar masses, which could be enough to form planetary systems like our own.

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