MAGNETIC FIELDS IN INTERSTELLAR CLOUDS FROM ZEEMAN OBSERVATIONS: INFERENCE OF TOTAL FIELD STRENGTHS BY BAYESIAN ANALYSIS

By R. Crutcher, Benjamin Dan Wandelt, C. Heiles, E. Falgarone, T. Troland. 2010

344 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Fluid Flow and Transfer Processes

View Paper: https://www.semanticscholar.org/paper/1c1277d2bdf9e062286e1b99f11ec4c461284122

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Fluid Flow and Transfer Processes

Citations in the corpus

Dense core formation by fragmentation of velocity-coherent filaments in L1517 (2011, background): “Ambipolar diffusion models, for example, seem to predict stronger magnetic fields than observed (Crutcher et al. 2010), and they usually predict contraction times that significantly exceed those inferred from observed core lifetimes and chemical clocks (Lee et al. 1999; Tafalla et al. 2002).”
Physical Processes in the Interstellar Medium (2014, background): “However, they are usually not strong enough to provide sufficient support (Crutcher et al., 1999; Crutcher & Troland, 2000; Bourke et al., 2001; Crutcher et al., 2009a, 2010b).”
The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows (2015, background): “On galactic scales the field is expected to be generated by the mean-field dynamo with field strengths of ∼ 1 − 10µG (see e.g. Beck 2001, 2009; Crutcher et al. 2010).”
On the universality of interstellar filaments: theory meets simulations and observations (2015, background): “The magnetic field strength, the turbulent velocity dispersion and the mean density all follow typical values derived from observations of clouds with the given physical properties (Falgarone et al. 1992; Crutcher et al. 2010).”
Inefficient star formation through turbulence, magnetic fields and feedback (2015, background): “The magnetic field strength, the turbulent velocity dispersion and the mean density all follow typical values derived from observations of clouds with the given physical properties (Falgarone et al. 1992; Crutcher et al. 2010).”
The density variance–Mach number relation in supersonic turbulence – I. Isothermal, magnetized gas (2012, background): “Conversely, the importance of magnetic fields in the star formation process is still inconclusive, despite decades of research (Mouschovias & Ciolek 1999; McKee & Ostriker 2007; Crutcher, Hakobian & Troland 2009; Crutcher et al. 2010; Bertram et al. 2012).”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “While there are still controversies, the data indicate that most clouds (or, more precisely, the parts of clouds with Zeeman measurements) are supercritical or close to critical, but not strongly subcritical (Crutcher et al. 2010).”
ON THE STAR FORMATION EFFICIENCY OF TURBULENT MAGNETIZED CLOUDS (2012, methodology): “For the MHD models, we chose magnetic field strengths consistent with the range observed in clouds of that size and density (see Crutcher 1999; Heiles & Troland 2005; Crutcher et al. 2010).”
PICO: Probe of Inflation and Cosmic Origins (2019, background): “Observations to date suggest that the outer envelopes of clouds can be supported against gravity by magnetic fields and turbulence, but in dense cores gravity tends to dominate, and so these dense structures can collapse to form stars [163].”
Planck intermediate results: XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds (2015, unknown): “Analysis of the Zeeman e ﬀ ect observations presented by Crutcher et al. (2010) shows that in the di ﬀ use ISM sampled by H i lines ( n H < 300 cm − 3 ), the maximum magnetic ﬁeld strength B max does not scale with density.”
THE STAR FORMATION RATE OF TURBULENT MAGNETIZED CLOUDS: COMPARING THEORY, SIMULATIONS, AND OBSERVATIONS (2012, methodology): “Magnetic-field strengths for the MHD simulations were chosen to be consistent with the range observed in clouds (e.g., Crutcher 1999; Crutcher et al. 2010).”
THE INTERPLAY OF MAGNETIC FIELDS, FRAGMENTATION, AND IONIZATION FEEDBACK IN HIGH-MASS STAR FORMATION (2010, methodology): “This strength was chosen to be consistent with an analysis of combined H i , OH, and CN Zeeman measurements that yielded a field strength B ' (10µG) ( n 300 cm−3 )0.68 (2) (Crutcher et al. 2010, in prep; Crutcher 2010).”
Turbulent molecular clouds (2012, unknown): “The non-thermal contributions to the total pressure are due to supersonic turbulence and magnetic fields, in rough equipartition, as shown by measurements of magnetic field intensity (Crutcher et al. 2010, see Section 5) and HI linewidths (Haud & Kalberla 2007).”
A characteristic scale for cold gas (2016, background): “Note that in the ISM, the magnetic field strength appears to be independent of temperature or phase for n≤ 300cm−3 (Crutcher et al., 2010), which is potentially explicable by reconnection diffusion (Lazarian, 2014).”
NON-IDEAL MHD EFFECTS AND MAGNETIC BRAKING CATASTROPHE IN PROTOSTELLAR DISK FORMATION (2011, methodology): “For example, at densities of order nH2 ∼ 103.5 cm−3 (probed by typical OH observations; Crutcher et al. 2010), the pre-condensation field strength of our model core would be only ∼ 3.5µG (if the condensation occurs more or less isotropically under flux-freezing condition, as it should be since the…”
Molecular Clouds in the Milky Way (2015, methodology): “This range is much larger than the sound speed of gas at typical CO cloud temperatures of 10–20 K but is comparable with the Alfvén velocity of 2.5 km s−1 for clouds with a magnetic field strength of 30 μ gauss and mean density of 250 cm−3 (Crutcher 1999, Crutcher et al. 2010).”
EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, background): “Zeeman measurements of molecular clouds give us a “starting value” with line of sight estimates of 0.1-1 mG (Crutcher et al. 2010; Falgarone et al. 2008).”