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. (http://www.sciencemag.org/cgi/content/full/295/5552/76)

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)

Note

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

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