Kinematics of the structure of the active region in Orion-KL |
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| Authors: | Email author" target="_blank">L?I?MatveyenkoEmail author V?A?Demichev S?S?Sivakon’ |
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| Institution: | 1.Space Research Institute,Russian Academy of Sciences,Moscow,Russia |
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| Abstract: | 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. |
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