Magnetic Orientations and Energetics in Interstellar Clumps within Small Clouds

Details Magnetic Orientations and Energetics in Interstellar Clumps within Small Clouds Magnetic Orientations and Energetics in Interstellar Clumps within Small Clouds

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...530..806v&link_type=abstract

The Astrophysical Journal, Volume 530, Issue 2, pp. 806-816.

Astronomy and Astrophysics

Astronomy

18

Infrared: Ism, Ism: Clouds, Ism: Globules, Magnetic Fields, Techniques: Polarimetric

Scientific paper

We present new observations of dust-continuum emission and associated magnetic fields made at 760 μm in the extreme-infrared (EIR, a.k.a. submillimeter wavelengths) of a total of 19 protostellar clumps inside 17 interstellar cloudlets (0049+56, L1551:IRS5, N2071:IR, N2264, OH 0739, IRC 10216, IRAS 1629, GGD 27, IRAS 18316, G30.79, G35.2:N, IR 20126, M20188, GL 2591, W75:N, 21391+58, LkHα 234). Our clumps, with gas density (~1x108 cm-3) and linear size (~0.09 pc; 18,000 AU) have a median linear polarization near 0.8%. Our typical clump extends to about one-half of the small cloud (``cloudlet''). For our clumps we find that ~c, with c=-1.4+/-0.2. For six of our nine smallest clumps, we find that the clump's magnetic field is roughly parallel to the elongation of the cloudlet in which the clump is embedded. For most simple resolved clumps near the Sun, a clump's gravitational energy is roughly equal to its turbulent (nonthermal kinetic) energy, while other energy components (magnetic, thermal, external pressure) are smaller. If there is exact equilibrium between turbulence and gravity, then we have the indices q=1+0.5c, where the gaseous line nonthermal dispersion σturb~Rq, with the radius R=0.5.

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