CN Zeeman measurements in star formation regions

By E. Falgarone, T. Troland, R. Crutcher, G. Paubert. 2008

147 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Inefficient star formation through turbulence, magnetic fields and feedback (2015, background): “Falgarone et al. (2008) find an average Alfvén Mach number of about MA = 1.5 in 14 different starforming regions in the Milky Way.”
THE INTERPLAY OF MAGNETIC FIELDS, FRAGMENTATION, AND IONIZATION FEEDBACK IN HIGH-MASS STAR FORMATION (2010, background): “If the magnetic field strengths inferred by Falgarone et al. (2008) are typical throughout high-mass clumps, and not just in their high-density cores, magnetic braking and reduction of fragmentation may be even stronger than reported here.”
Turbulent molecular clouds (2012, background): “They include Zeeman measurements that sample B‖ in diffuse (mostly atomic) clouds in HI from Heiles & Troland (2005), in low-mass dense cores and molecular clouds in OH and in star-forming regions from CN (Crutcher 1999, Falgarone et al. 2008).”
OUTFLOW FEEDBACK REGULATED MASSIVE STAR FORMATION IN PARSEC-SCALE CLUSTER-FORMING CLUMPS (2009, background): “Our adopted degree of magnetization is in the range inferred by Falgarone et al. (2008).”
The Critical Density and the Effective Excitation Density of Commonly Observed Molecular Dense Gas Tracers (2015, background): “…Plume et al. 1997, Jijina et al. 1999, Savage et al. 2002, Pirogov et al. 2003, Purcell et al. 2006, Blair et al. 2008, Rosolowsky et al. 2008, Falgarone et al. 2008, Hily-Blant et al. 2010, Barnes et al. 2011, Dunham et al. 2011, Ginsburg et al. 2011, Reiter et al. 2011, Adande et al. 2012,…”
Collapse, outflows and fragmentation of massive, turbulent and magnetized prestellar barotropic cores (2011, background): “…et al. 2010), the influence of the magnetic field is not extensively explored yet because only few studies have been performed (e.g. Banerjee & Pudritz 2007) in spite of the measurement which suggest that it reaches substantial values (Crutcher 1999, Falgarone et al. 2008, Girart et al. 2009).”
RADIATION MAGNETOHYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR COLLAPSE: PROTOSTELLAR CORE FORMATION (2012, background): “…transport angular momentum very efficiently and modify the structure of the accretion flow significantly, and observations suggest that molecular clouds are considerably magnetized (Heiles & Crutcher 2005; Girart et al. 2006; Falgarone et al. 2008; Troland & Crutcher 2008; Crutcher et al. 2009).”
COLLAPSE OF MASSIVE MAGNETIZED DENSE CORES USING RADIATION MAGNETOHYDRODYNAMICS: EARLY FRAGMENTATION INHIBITION (2011, background): “In this Letter, we explore three magnetization degrees: μ = 130 corresponding to a weak initial magnetic field, and μ = 5 and μ = 2 which are close to the observed values (e.g., Falgarone et al. 2008).”
DISPERSION OF MAGNETIC FIELDS IN MOLECULAR CLOUDS. II. (2008, background): “…of measuring the strength of (generally the line of sight component of) magnetic fields (Heiles 1997; Crutcher et al. 1999; Brogan & Troland 2001; Falgarone et al. 2008), its weakness in the interstellar medium limits the types of environments and number of regions where detections can…”
On the universality of interstellar filaments: theory meets simulations and observations (2015, background): “Falgarone et al. (2008) find an average Alfvén Mach number of about MA = 1.5 in 14 different star-forming regions in the Milky Way.”
TADPOL: A 1.3 mm SURVEY OF DUST POLARIZATION IN STAR-FORMING CORES AND REGIONS (2013, background): “These measurements are consistent with previous single-dish CN Zeeman measurements, which estimate the line-of-sight magnetic field strength to be 0.36 and 0.71mG for MM1 and MM2, respectively (Crutcher 1999; Falgarone et al. 2008).”
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).”
THE STAR FORMATION RATE OF SUPERSONIC MAGNETOHYDRODYNAMIC TURBULENCE (2009, methodology): “The compilation of OH and CN Zeeman measurements by Troland & Crutcher (2008) and Falgarone et al. (2008) give an average value of β = 0.39, independent of density (the value is the same in the two samples, even if the mean gas density of the CN cores is approximately two orders of magnitude larger…”