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• W3102640871 endingPage "182" @default.
• W3102640871 startingPage "137" @default.
• W3102640871 abstract "The diffuse interstellar H I is the matrix within which many molecular clouds reside and the medium that soaks up the energy injected by sources such as supernovae and stellar winds. This energy stimulates turbulence in the H I, which cascades up the turbulent wavenumber spectrum. The spectral wavelengths extend all the way down to scales most easily quoted in Astronomical Units. H I and molecular clouds enjoy a synergistic relationship, with turbulent energy, angular momentum, magnetic fields, and matter flowing across the boundaries in both directions. The molecular clouds form stars, which in turn act as energy sources to round the circle and make star formation a feedback process. Fortunately for us who study magnetic fields, the neutral medium isn’t really neutral and, as a consequence, flux freezing applies. In diffuse H I the minimum free electron fraction is, at minimum, equal to that of heavy elements that have ionization potential less than that of H I ( > ∼ 10−4) because even in the dark reaches of space there are plenty of starlight photons available to keep any such element ionized. As a crude approximation we can model a piece of the interstellar gas as a giant inductor, for which the timescale τ for decay of a current (and its associated magnetic field) is the inductance divided by the resistance; this, in turn, goes as τ ∝ L/η, where L is the length scale and η the resistivity. Even with the low fractional ionization, L dominates and timescales for decay are always long in diffuse H I. In dense molecular clouds starlight is excluded and the free electrons come from cosmic-ray ionization of H; the fractional ionization is small enough that slow leakage of frozen magnetic flux allows the clouds to gradually evolve. With flux freezing, the magnetic field becomes one of the four most important forces on the diffuse gas. The others are gas pressure, cosmic-ray pressure, and gravity. Gravity dominates on the largest scales, e.g. by keeping the gas pulled down as part of the Galactic plane; it also dominates during star formation, of course. On all other scales the gas responds only to the three pressure forces. The gas and cosmic rays are connected by the field, so they form a coupled system. The field is a – perhaps the – major player. One determines the field strength in the diffuse interstellar gas in several ways. Each method has its own idiosyncrasies and provides values that are biased either up or down. Beck et al. (2003) is required reading to understand these biases. Synchrotron emissivity provides a volume average of 〈B〉, where 1.9 < ∼ x < ∼ 3.9 depending on whether one assumes the electron cosmic-ray spectrum or energy equipartition (Beck, 2001). Comparing pulsar rotation and dispersion measures" @default.
• W3102640871 created "2020-11-23" @default.
• W3102640871 creator A5015624173 @default.
• W3102640871 creator A5030787078 @default.
• W3102640871 date "2005-10-01" @default.
• W3102640871 modified "2023-09-27" @default.
• W3102640871 title "Magnetic Fields in Diffuse HI and Molecular Clouds" @default.
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• W3102640871 doi "https://doi.org/10.1007/11369875_7" @default.
• W3102640871 hasPublicationYear "2005" @default.
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