The star forming core of Mon R2

Abstract

In this thesis, the nature of the star forming core of the Mon R2 cloud is investigated using new, high spatial resolution observations. The new data include: maps of [superscript 12]CO J=3[right arrow]2, HCN J=4[right arrow]3 and H[subscript 2]CO J[subscript k-1][subscript k+1]= 5 [subscript 1.5][right arrow]4[subscript 1.4] spectra of [superscript 12]CO J=2[right arrow]1 and [superscript 13]CO J=3[right arrow]2 at 12 positions, an infrared M-band spectrum, and finally submillimeter and millimeter continuum maps (450 [mu]m, 800 [mu]m, 1100 [mu]m and 1300 [mu]m).

Based on the spatial distribution of the intensity of the [superscript 12]CO J=3[right arrow]2 transition, we present a qualitative description of the region which consists of complexes and clumps. The complexes surround a central area of lower intensity which corresponds to the compact H II region in the cloud core.

The complexes incorporate 13 smaller intensity peaks (clumps). The CO clumps are not distributed in a bipolar fashion. We propose that the outflow could originate from IRS 3, which has gone through a quiescent phase.

The sum of the magnetic and the gravitational energy (12 x 10[superscript 45]erg) is somewhat smaller than the total kinetic energy of the inner core of the Mon R2 cloud (15 x 10 [superscript 45]erg), and, hence, the core is either in the process of disruption or in dynamical equilibrium. (Abstract shortened by UMI.)