turbulence in protoplanetary disks: observaons and theoryturbulence in protoplanetary disks:...

TurbulenceinProtoplanetaryDisks:Observa7onsandTheory

JakeSimon(CUBoulder/SwRI)A.MeredithHughes(Wesleyan)

ParameterSpace 1)  Radius2)  Height3)  Time

MoreDirectWaystoMeasureTurbulence

Accretion rate measurements

UV continuum excess Gullbring et al. (1998)

Rovibrational lines

Transonic turbulence to fit CO band head Carr et al. (2004)

Millimeter observations

Fitting models to low-res CO spectra Dutrey et al. (1998)

LessDirectWaystoMeasureTurbulence

Narrow Rings

Pinte et al. (2016), Okuzumi et al. (2016)

Dust traps / vortices

van der Marel et al. (2013)

Settling - SED

Mulders et al. (2012)

Settling - Imaging

Guilloteau et al. (2016)

Also:Polariza7on(Hulletal.submiQed)Chemistry/ioniza7on(Cleevesetal.2015)

R =100 AU

Flaherty… Simon et al. (2015), ApJ HD 163296

Local simulation at 100 AU

Theory

CO CO Flaherty… Simon et al.

(2017), ApJ HD 163296

DCO+

Flaherty… Simon et al. (2018),

accepted, TW Hya CO CO

Magnetic field lines

Stronger field

βz = 2P/Bz2

β0 = 2P/B02

Weak turbulence

Ques7ons:

•  Whatisthenextstepinobserva7ons?Thisisaques7onforbothobserversandtheorists!– Howelsemightweconstrainturbulence?– Howcanwemakeendsmeetinradius/height/7me?

– Howdoesturbulencefeedintoyourtheoryofplanetforma7onandaffectobserva7onaltracers?

•  Whataretheimplica7onsifturbulenceislowin(some/most)outerdisks?– Aretherealterna7vestoMRIthatareconsistent?– Doeslowturbulencecauseirrevocableproblems?

Whatdoesittaketodox?Rosenfeldetal.(2013)

Δv=110m/s,θ=0.5”,140minutesonsource(~3hourstotal)

Todoublethespectralresolu7on(sameSNR):3hx2=6hours

Todoubletheangularresolu7on(sameSNR):3hx16=48hoursTodoubletheSNR:3hx4=12hours

Note:Nantennashasalmostdoubledsincethen,whichhelpsalot(all7mesdownby~4x).

Also,beQerweathermakesabigdifferenceaboveBand6.(3rdvs.6thoc7lechanges7mesbyalmost4xatBand7)

Butremember…thisisoneofthebiggest/brightestknowndisks…