Magnetic Field versus Gas Density, in Different Physical Conditions

Details Magnetic Field versus Gas Density, in Different Physical Conditions Magnetic Field versus Gas Density, in Different Physical Conditions

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ap%26ss.234....1v&link_type=abstract

Astrophysics and Space Science, Volume 234, Issue 1, pp.1-10

Astronomy and Astrophysics

Astrophysics

12

Magnetic Fields, Molecular Clouds

Scientific paper

A search is made here for possible variations in the behavior of magnetic field valuesB at various gas density valuesn, when comparing low density gas versus high density gas, and when comparing compressed gas versus quiescent gas.
(a)
For thequiescent microturbulent interstellar gas (e.g., clouds, interclumps — see TableI), the statistical relationB ~n k yieldsk = 0.46 ± 0.07 forhigh gas densityn > 100 cm-3, andk = 0.17 ± 0.03 forlow gas densityn < 100 cm-3 (see Figure 1).
(b)
For thecompressed macroturbulent interstellar gas (e.g., masers, expanding shells — see Table II), the statistical relationB ~n K yieldsK = 0.61 ± 0.09 forhigh gas densityn > 100 cm-3, andK = 0.37 ± 0.2 forlow gas densityn < 100 cm-3 (see Figure 2).
(c)
The separation betweenlow density gas andhigh density gas is statistically significant. The 2 different physical behaviors (below and above the break at 100 cm-3) are confirmed statistically (about 2 to 4 sigma away for the quiescent gas alone; about 3 to 6 sigma away for the combined quiescent plus compressed gas).
(d)
The separation betweencompressed gas andquiescent gas is not statistically significant now (see Figure 3). Atn > 100 cm-3, a comparison of quiescent gas versus compressed gas shows no statistically significant differences in behavior (they are only about 1 sigma away). Atn < 100 cm-3, a comparison of quiescent versus compressed gas also shows no statistically significant differences in behavior (less than 1 sigma away).
(e)
A relation between the densityn and the galactic-wide Star Formation Rate (SFR) can be made for galactic magnetic fields, i.e.: (SFR) ~n n . For galactic-wide parameters using quiescent, low densityn < 100 cm-3, and the known relationshipsB ~n k/j withk = 0.17,B ~ (SFR) j withj = 0.13, then one gets here a lawSFR ~n k/j with an exponentk/j = 1.3. This is in rough accord with known data for the Milky Way and for NGC6946.

Affiliated with

Also associated with

No associations

Rating

Magnetic Field versus Gas Density, in Different Physical Conditions does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Magnetic Field versus Gas Density, in Different Physical Conditions, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magnetic Field versus Gas Density, in Different Physical Conditions will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1257499