The Turbulent Interstellar Medium

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arXiv:astro-ph/0605088v1 3 May 2006Theturbulentinterstellarmedium

A.Burkert

UniversityObservatoryMunich,Scheinerstr.1,D-81679Munich,Germany

1Introduction

Steady-statemulti-phasemodelshavedominatedourpictureoftheinterstellar

medium(ISM)intheMilkyWayforalongtime.Accordingtotheearlymodel

ofFieldetal.(1969)andsubsequentmodificationstheISMrepresentsan

ensembleoftwostablegasphasesthatareinthermalpressureequilibriumwithameanpressureofn×T≈1000Kcm−3.Coldmolecularcloudswith

meandensitiesofn≈100cm−3andtemperaturesT≈10Kareembedded

inawarm,diffuseandpartlyionizedintercloudcomponentwithdensityn≈

0.1cm−3andtemperaturesoforder104K.Thegascloudscontainalarge

fractionofthetotalmassandmoveasstable,densespheroidalobjectsinthe

widespreadintercloudmediumwhichontheotherhandhasthedominant

volumefillingfactor.Starformationwouldeventuallyheatanddispersethe

massiveclouds.Newgenerationsofsmallcloudsformfromtheintercloud

mediumbycoolinginstabilities(Field1965)andsubsequentlygrowbyrandom

inelasticcloud-cloudcollisions(e.g.Elmegreen1989).Alreadyin1977McKee

&Ostrikernoticedthatthetwo-phasemodelcouldnotbevalidassupernova

explosionsshouldleadtoathird,hotandtenuousgasphase.Howeverthey

stillfocussedontheimportanceofthermalpressureequilibriumandasteady

statedescriptionasthemainphysicalconstrainttoevaluatethestateofthe

variousgasphases.

Thissituationhaschangeddrasticallyinthelastdecade.High-resolutionob-

servationse.g.withtheInfraredAstronomicalSatellite(IRAS)andmorere-

centlywiththeSpitzersatelliterevealacomplexkinematicalstateandspatial

structureoftheinterstellargas.TheISMappearstobefarfromhydrostatic

equilibriumandturbulent.Infact,itisthekineticturbulentpressure,not

thermalpressure,thatprobablydominatesthegasdynamicsandthatchar-

acteristizesitsdensitystructureandthedynamicsofthevariousgasphases.

Turbulencecouplesstructuresonverydifferentscales.Molecularcloudsmight

justrepresentthehigh-densitytailofthishierarchy,formingincollidinggas

flowsthatleadtotransientlocalcompressionsthatsubsequentlycool.We

willdiscussbelowthatthecomplexinternalstructureofmolecularclouds

thatdeterminestheirevolutionandtheircondensationintostarsandstellar

clustersisalsoaresultofturbulence,generatedbyvarioushydrodynamical

instabilitiesduringtheprocessofmolecularcloudformation.

WithturbulencebecomingthedominantsourceofstructureintheISM,the-

oreticalmodelslosttheirsimplicityandequilibriumdescriptionshadtobe

replacedbydynamicalmodelswherelargeandsmallscalesaresimultane-

ouslyconsidered.Wearejuststartingtoexploreandunderstandthisrichand

enormouslycomplexnewfieldofastrophysics.InthisshortreviewIcanonly

focusonafewinterestingtopicsandunsolvedquestions.Anexcellentand

comprehensivereviewofourcurrentunderstandingispresentedbyElmegreen

&Scalo(2004)andScalo&Elmegreen(2004).Reviewsthatfocusespecially

onnumericalsimulationsofISMturbulencearee.g.V´azquez-Semadenietal.

(2000)andBallesteros-Paredesetal.(2006).Asummaryofourunderstanding

ofstarformationinturbulentcloudsisgivenbyMacLow&Klessen(2004).

2

Fig.1.Characteristicvelocitydispersionσofasampleofdiskgalaxiesasfunctionoftheiraveragesurfacestarformationrateinunitsof(M⊙yr−1kpc−2)(Dibetal.2006).σisalmostindependentofthestarformationratefortypicalvaluesfoundinslowlyevolvingdiskgalaxiesliketheMilkyWay.Itrisessteeplyinstarburstregionswithhighstarformationrates.

2TurbulenceinthediffuseISM

ItisnowawellestablishedfactthattheISMingalacticdisksisdominatedby

irregularandoftensupersonicgasmotions(Larson1981;Scalo1987;Dickey

&Lockman1990).InmostspiralgalaxiesHIemissionlinesexceedthevalues,

expectedfromthermalbroadening,indicatingturbulentvelocitydispersionsσ

oforder10km/s.Thevelocitydispersioningalacticdisksingeneraldecreases

outwardsfromσ≈12-15km/sintheinnerregionstoσ≈4-6km/sin

theouterparts.Figure1showsthecharacteristicvelocitydispersionfora

sampleofgalaxiesasfunctionoftheirsurfaceaveragedstarformationrate

(Dibetal.2006).Notethatself-regulatedstarformationratesthataretypical

forMilkyWay-typediskgalaxiesleadtovelocitydispersionsoforderσ≈

6-8kms−1,independentofthestarformationrate.ThediffuseISMacts

likeathermostate.Thesituationchangesdrasticallyinsituationswherestar

formationisgettingoutofcontrol,leadingtostarburststhatlastashorttime,

oforder108yrs.Asshowninfigure1,thetransitionintothestarburstregime

ismarkedbyasteepincreaseofthevelocitydispersion.

32.1DrivingturbulenceinthediffuseISM

Severalphysicalprocesses,actingondifferentscalesandinjectingdifferent

amountsofkineticenergycontributetothedrivingofISMturbulence.How-

ever,despitealargeamountofnumericalworkinthisfield,thedominanten-

ergeticsourcesandthephysicalprocessesthatconvertthekineticenergyinto

turbulencearenotwellunderstood.Starsareobviouscandidates.Large-scale

expandinggasflowscoulde.g.begeneratedbyhigh-pressureHIIregions,re-