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MHD related papers

References provided by Chris

Recent papers
  1. Sun & Han (astro-ph/0402180) -- Structure Formation Studies for Turbulent Interstellar Medium
  2. Padoan, Jimenez, Juvela & Nordlund (astro-ph/0311349) -- The Average Field Strength in Molecular Clouds: New Evidence of Super-Alfvenic Turbulence
  3. Chatterjee, Nandy & Choudhuri (astro-ph/0405027) -- Full-Sphere Simulations of a Circulation-Dominated Solar Dynamo: Exploring the Parity Issue
  4. Brandenburg & Subramanian (astro-ph/0405052) -- Astrophysical magnetic fields and nonlinear dynamo theory: a review
  5. Elmegreen & Scalo (astro-ph/0404451) -- Interstellar Turbulence I: Observations and Processes
  6. Scalo & Elmegreen (astro-ph/0404452) -- Interstellar Turbulence II: Implications and Effects
Pure MHD papers
  1. 2003a: Cho & Lazarian -- Generation of Compressible Modes in MHD Turbulence
  2. 2003b: Cho & Lazarian -- Compressible magnetohydrodynamic turbulence: mode coupling, scaling relations, anisotropy, viscosity-damped regime and astrophysical implications
  3. 2003c: Cho & Lazarian -- Basic Properties of Compressible MHD Turbulence: Implications for Molecular Clouds
  4. 1994: Goldreich & Sridhar
  5. 1995: Goldreich & Sridhar
  6. 1997: Goldreich & Sridhar
  7. 2001: Lithwick & Goldreich
  8. 2003: Lithwick & Goldreich
  9. Jason Maron, Goldreich, Cowley, et al.
Chronological list of papers from the star formation standpoint:
1956: Mestel & Spitzer
-- static magnetic fields can support regions up to some mass, but they also slip away slowly (ambipolar diffusion) in the absence of ionizing radiation.
1974: Goldreich & Kwan
-- propose that molecular clouds are collapsing in free fall.
1974: Zuckerman & Palmer [also Zuckerman & Evans]
-- that's impossible because the (average) star formation timescale is a hundred times longer than the free-fall time.
* 1975: Arons & Max
-- Alfven waves damp slowly and so could stall collapse
1975: [Scoville & Solomon]
-- do a survey of molecular clouds in the galaxy.
1980: [Norman & Silk]
-- First model of self-regulated star formation & turbulence -- turbulence regenerated by stars.
1980: [Fleck]
-- Suggests turbulence regenerated by Galactic differential rotation]
1981: Larson
-- suggests that there are tight correlations between the observable properties of molecular clouds, for instance turbulent velocity vs. radius and density vs. radius.
1982: Scalo & Pumphrey
-- Turbulent decay rate estimated in a nonmagnetized model and argued to be not-so-fast.
1983: Zweibel & Josafatsson
-- Decay rates of hydromagnetic waves. They estimate "turbulent" decay in very imbalanced cascades, i.e., one wave at a time, using ion-neutral friction and nonlinear wave damping (so recalled).
1987: Shu, Adams, & Lizano
-- an excellent overview of what was known about star formation up to then.
*1989: McKee
-- "Photoionization-regulated star formation": star formation regenerates turbulence and ambipolar diffusion slows down star formation. [Assumed relatively slow turb. decay.]
1991: Blaauw
-- correlation between stars and clouds allow one to estimate cloud lifetimes [10-25 Myr]
1992: McKee & Zweibel
-- Incorporates magnetic fields into the Virial Theorem for molecular clouds, attempting to deal with static and turbulent field contributions
1992: Falgarone, Puget, & Perault
-- small-scale scaling laws in molecular cloud turbulence
1993: McKee, Zweibel, Goodman, & Heiles (in Protostar & Planets III)
-- a lengthy review of the role of magnetic fields in molecular clouds as of then.
*1995: McKee & Zweibel and Zweibel & McKee
-- model the propagation of Alfven waves in molecular clouds and show that Larson's correlations can be explained this way.
*1996: Gammie & Ostriker
-- a 1D version of my project -- turbulent support against gravity
1996: Vazquez-Semadeni, Passot, & Pouquet
-- decay of nonmagnetized turbulent support against gravity
*1998: Stone, Ostriker & Gammie
-- turbulent decay rate
1999: Padoan & Nordlund
-- superAlfvenic turbulence model for molecular clouds.
*1999: Ostriker, Gammie, & Stone
-- a "2.5-D" version of my problem, i.e., magnetic turbulence support of self-gravitating gas
*1999: MacLow
-- another paper like SOG on decay rates (also with ZEUS)
1999: Zweibel
-- review of magnetic fields in molecular clouds [Phys. Plasmas]
*1999: McKee (astro-ph/9901370)
-- excellent review of his view of molecular clouds, magnetic fields, etc.
#1999: Ballesteros-Paredes, Vazquez-Semadeni, & Scalo
-- "Clouds as turbulent density fluctuations". Argues clouds are not long-lived hydrostatic objects but transient objects.
1999: Ballesteros-Paredes, Hartmann, & Vazquez-Semadeni
-- "turbulent flow-driven molecular cloud formation". Similar idea, applied to the "mystery of the missing post-T-tauri stars".
1999: Palla & Stahler
-- argue that clouds live for tens of millions of years (several free-fall times) according to ages of young stars within them. [See Hartmann 2003 for an opposing view.]
#2000: Elmegreen
-- "Star Formation in a Crossing Time". Argues clouds are not in virial balance at all.
#2001: Hartmann, Balasteros-Paredes, & Bergin
-- "Rapid formation of molecular clouds." Argues that molecular clouds form, form stars, and disperse "rapidly", i.e., a "crossing time", and therefore are not in equilibrium or virial balance.
*2002: Matzner
-- argue that photoionization (H II) regions are very energetic events in the life of a molecular cloud and both invigorate its turbulence and remove mass from it.
2002: Ward-Thompson
-- Science article, decent recent overview of the field. (
2002: Boldyrev, Nordlund, & Padoan:
--Scaling relations in theoretical models of supersonic MHD turbulence
2002: Hartmann
-- "flows, fragmentation, & star formation". Argues that observations of nearby molecular clouds show behavior different from theoretical expectations.
*2003: Kudoh & Basu
-- a 1D version of my project. Larson -- more in-depth recent overview of the field
2003: Vazquez-Semadeni, Ballesteros-Paredes, & Klessen
-- a rather interesting view of star formation.
2003: Hartmann
-- argues Palla & Stahler were wrong about the ages of stars found in molecular clouds, and that clouds are young (transient)
*2003: Hartmann
-- [in Star Formation at High Angular Resolution]; argue that young stars are never held up by magnetic fields and that ambipolar diffusion is irrelevant
*2004: MacLow & Klessen
-- a review of why they don't think magnetic fields are important
#2004: Clark & Bonnell
-- star formation in unbound clouds (no support needed)


* useful preparation for a talk introduction
  The rest of the papers are provided for their historical context. 

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Last Update: 19 Feb 2004