Magnetic fields in molecular clouds

By R. Crutcher. 2007

629 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/4c83c86a1cf65d7568b3b7d732f6228f74b8924b

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In Astronomy and Astrophysics

Citations in the corpus

RADIATION MAGNETOHYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR COLLAPSE: NONIDEAL MAGNETOHYDRODYNAMIC EFFECTS AND EARLY FORMATION OF CIRCUMSTELLAR DISKS (2015, background): “…fields are weak (Bate 1998, 2010, 2011; Saigo et al. 2008; Tomida et al. 2010a), but typically magnetic fields observed in molecular clouds (Crutcher 2012; Li et al. 2014a, and references therein) are strong enough to remove angular momenta efficiently and overcome the centrifugal barrier…”
Cosmic-ray propagation with DRAGON2: I. numerical solver and astrophysical ingredients (2016, methodology): “n downloaded from http://www.nrl.navy.mil/rsd/RORF/ne2001/ { 37 { There are several methods to measure and constrain the intensity and the orientation of this component: Zeeman splitting observations [93], infrared, synchrotron and starlight polarisation studies [94{96], and measurements of the Fara”
Ambipolar diffusion in low-mass star formation - I. General comparison with the ideal magnetohydrodynamic case (2015, background): “S R ] 2 1 O ct 2 01 5 (Crutcher 2012), the generation of violent interchange instabilities at the protostar-disk interface (Li et al. 2014b), the growth of the pseudo-disk (Hennebelle & Fromang 2008), and the distortion of the upper layer of the pseudo-disk due to reconnection and the split…”
AN IMPRINT OF MOLECULAR CLOUD MAGNETIZATION IN THE MORPHOLOGY OF THE DUST POLARIZED EMISSION (2013, background): “The study of the magnetic field in molecular clouds is crucial to understand the physical processes relevant in molecular cloud evolution and star formation (Shu et al. 1987; McKee & Ostriker 2007; Crutcher 2012).”
LOW VIRIAL PARAMETERS IN MOLECULAR CLOUDS: IMPLICATIONS FOR HIGH-MASS STAR FORMATION AND MAGNETIC FIELDS (2013, background): “Crutcher (2012) suggests an approximate density–dependent upper limit B .”
EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, background): “…of young protostars in some instances exhibit large scale magnetic field structure in what has been described to resemble the shape of an hourglass (e.g., Girart et al. 2006), thought to arise from the gravitational collapse of a magnetized molecular cloud (see review by Crutcher 2012).”
TADPOL: A 1.3 mm SURVEY OF DUST POLARIZATION IN STAR-FORMING CORES AND REGIONS (2013, background): “…& Mouschovias 1993; Tassis et al. 2009) or turbulent magnetic reconnection diffusion (Lazarian 2005; Leão et al. 2013) are thought to allow dense cores to become “supercritical” (see Crutcher 2012), at which point gravity overwhelms magnetic support and allows the formation of a central protostar.”
The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows (2015, background): “Local tangled components are of similar strengths, however, in dense molecular clouds fields up to several mG have been measured (see e.g. Crutcher et al. 2010; Crutcher 2012).”
Planck intermediate results: XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds (2015, neutral): “These limitations have been particularly critical when integrating magnetic ﬁelds into the general picture of MC dynamics (Elmegreen & Scalo 2004; Crutcher 2012; Heiles & Haverkorn 2012; Hennebelle & Falgarone 2012).”
Global hierarchical collapse in molecular clouds. Towards a comprehensive scenario (2019, background): “Moreover, magnetic support is also not expected to provide sufficient support, as GMCs are now known to be magnetically supercritical in general (Crutcher 2012), and so their gravitational contraction must proceed dynamically rather than quasistatically.”
PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper (2013, background): “nations, focusing on either ambipolar diffusion, turbulence, or magnetic reconnection to decouple matter from the magnetic ﬁeld and allow the formation of condensations of gas in which stars may form [53]. PRISM observations of the polarization in the far-IR and sub-mm will provide unique clues to u”
Molecular Clouds in the Milky Way (2015, background): “…2012, Kennicutt & Evans 2012, Krumholz 2014); interstellar turbulence (Scalo & Elmegreen 2004, Elmegreen & Scalo 2004); cold, dark clouds (Bergin & Tafalla 2007); nearby galaxies (Fukui & Kawamura 2010); magnetic fields (Crutcher 2012); and the CO-to-H2 conversion factor (Bolatto et al. 2013).”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “Pictures of static clouds supported by magnetic fields are currently out of fashion (McKee & Ostriker 2007), but magnetic fields are almost certain to play a role in some way (for a current review, see Crutcher 2012, this volume).”
Global collapse of molecular clouds as a formation mechanism for the most massive stars (2013, background): “Following previous studies (Pillai et al. 2011), we estimated that the magnetic field strength |B|vir necessary to virialize SDC335 is |B|vir = 300 µG, which is at least three times higher than observations of clouds at similar densities suggest (Crutcher 2012).”
The big problems in star formation: The star formation rate, stellar clustering, and the initial mass function (2014, background): “300 cm−3, rising as n2/3H thereafter, and a gas temperature T ≈ 10 K (Dobbs et al. 2014; Crutcher 2012).”
The 511 keV emission from positron annihilation in the Galaxy (2010, background): “…that in atomic clouds, B is typically a few µG, with a slight tendency to increase with increasing density (Heiles and Troland, 2005; Troland and Heiles, 1986), while in molecular clouds, B increases approximately as the square root of density, from ∼ 10 µG to ∼ 3 000 µG (Crutcher, 1999, 2007).”