Magnetic field-gas density relation and observational implications revisited

• We revisit the relation between magnetic-field strength (B) and gas density (ρ) for contracting interstellar clouds and fragments (or, cores), which is central in observationally determining the dynamical importance of magnetic fields in cloud evolution and star formation. Recently, it has been claimed that a relation B ∝ ρ2/3 is statistically preferred over B ∝ ρ1/2 in molecular clouds, when magnetic-field detections and non-detections from Zeeman observations are combined. This finding has unique observational implications on cloud and core geometry: the relation B ∝ ρ2/3 can only be realized under spherical contraction. However, no indication of spherical geometry can be found for the objects used in the original statistical analysis of the B-ρ relation. We trace the origin of the inconsistency to simplifying assumptions in the statistical model used to arrive at the B ∝ ρ2/3 conclusion and to an underestimate of observational uncertainties in the determination of cloud and core densities. We show that, when these restrictive assumptions are relaxed, B ∝ ρ1/2 is the preferred relation for the (self-gravitating) molecular-cloud data, as theoretically predicted four decades ago.

Ämnesord

NATURVETENSKAP  -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)

NATURAL SCIENCES  -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)

Nyckelord

stars: formation

ISM: clouds

ISM: magnetic fields

diffusion

methods: statistical

MHD

Astrophysics - Astrophysics of Galaxies

Publikations- och innehållstyp

art (ämneskategori)

ref (ämneskategori)