Kinematics of the structure of the active region in Orion-KL


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The kinematics of the superfine structure of the active star-forming region in the dense molecular cloud Orion-KL has been investigated in the Н2О maser emission for the period 1998–2003. It has been established that the surrounding gas inflows onto the disk and is transferred in a spiral trajectory to the center. An excess angular momentum as it is accumulated is carried away by a bipolar outflow; a highvelocity central flow surrounded by low-velocity components is formed. The outer low-velocity component observed at the detection limit has a diameter Ø3 ≈ 4.5 AU, further out, Ø2 ≈ 0.5 AU and Ø1 ≈ 0.24 AU. The gas transfer velocity increases exponentially as the center is approached. The maser emission from the central flow is decisive. A rise in the velocity leads to a flow discontinuity and a reduction in the amount of inflowingmaterial and, accordingly, the emission level. The emission in the period under consideration was reduced exponentially for ~6 months, whereupon its restoration began.

Sobre autores

L. Matveyenko

Space Research Institute

Autor responsável pela correspondência
Email: lmatveenko@gmail.com
Rússia, ul. Profsoyuznaya 84/32, Moscow, 117997

V. Demichev

Space Research Institute

Email: lmatveenko@gmail.com
Rússia, ul. Profsoyuznaya 84/32, Moscow, 117997

S. Sivakon’

Space Research Institute

Email: lmatveenko@gmail.com
Rússia, ul. Profsoyuznaya 84/32, Moscow, 117997

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