Formation of Low Mass Stars, Disks, and Bipolar Outflows

Details Formation of Low Mass Stars, Disks, and Bipolar Outflows Formation of Low Mass Stars, Disks, and Bipolar Outflows

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jena.confq..28m&link_type=abstract

"JENAM-2007, "Our non-stable Universe", held 20-25 August 2007 in Yerevan, Armenia. Abstract book, p. 28-28"

Computer Science

Scientific paper

We are studied the super fine structure of the Orion-KL active region of H2O maser emission at V_LSR = 7.65 km/s in polarized emission with an angular resolution 0.15 mas or 0.07 AU, epoch 1998-1999. The star formation is accompanied by a structure that consists of bright compact source - ejector, high-collimated bipolar outflow and torus-disk, divided into proto-planetary rings. Brightness temperature of the ejector is T_b ≈ 10^17 K, degree of linear polarization is m ≲ 50%. The ring rotation corresponds to hard disk. Rotation period is equal 170 yr. Precession of axis (T≈10 yr) is determined helix structure of outflow. Variation of the polarized plane in the profile is equal dX/dV = - 23 o/km/s, that is much higher than Faraday's rotation in the HII region in front of the molecular cloud. The “rotation” is effect of different polarized orientation of bipolar ejector.

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