Pre-main sequence binaries.

Details Pre-main sequence binaries. Pre-main sequence binaries.

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esoc...33..447z&link_type=abstract

ESO Workshop on Low Mass Star Formation and Pre-Main Sequence Objects, p. 447 - 469

Astronomy and Astrophysics

Astrophysics

38

Pre-Main-Sequence Stars: Binaries, Pre-Main-Sequence Stars: Stellar Evolution, Pre-Main-Sequence Stars: Circumstellar Disks, Star Formation: Close Binaries

Scientific paper

The astrophysics of pre-main sequence (PMS) binaries is discussed. Recent observational results on visual, speckle, lunar occultation and spectroscopic PMS binaries are summarized. Several suggestions for new observations are made: to image the known visual PMS binaries with NIR arrays (to separate the NIR excess of the components); to measure the 10 μm excess of each component (to probe for separate circumstellar disks); to detect UV boundary layer emission from the individual components (as a tracer of the mass accretion rates); to search for aligned double jets from the components (to probe for coplanar disks). On the theory side, numerical calculations of the collapse of an elongated filament, rotating end over end, are proposed as a promising mechanism for the formation of wide binaries. The origin of close binaries remains a more daunting challenge. Any formation process must be capable of creating pairs of roughly equal mass and high orbital eccentricity.

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