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.)