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-