brian gleim march 23rd, 2006 ast 591 instructor: rolf jansen
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“The interaction of a giant planet with a disc with MHD turbulence II: The interaction of the planet with the disc” Papaloizou & Nelson 2003, MNRAS 339 (4), 993. Brian Gleim March 23rd, 2006 AST 591 Instructor: Rolf Jansen. Introduction. - PowerPoint PPT PresentationTRANSCRIPT
““The interaction of a giant planet with The interaction of a giant planet with a disc with MHD turbulence II:a disc with MHD turbulence II:
The interaction of the planet with the The interaction of the planet with the disc”disc”
Papaloizou & Nelson 2003, MNRAS 339 (4), 993Papaloizou & Nelson 2003, MNRAS 339 (4), 993
Brian GleimBrian GleimMarch 23rd, 2006March 23rd, 2006
AST 591 AST 591 Instructor: Rolf JansenInstructor: Rolf Jansen
IntroductionIntroduction Discovery of giant planets close to Discovery of giant planets close to
their star has led to the idea that their star has led to the idea that they migrated inwards due to they migrated inwards due to gravitational interaction with the gravitational interaction with the gaseous discgaseous disc
Causes of MigrationCauses of Migration Standard picture involves torques Standard picture involves torques
between a laminar viscous disc and a between a laminar viscous disc and a Jovian protoplanet exciting spiral Jovian protoplanet exciting spiral waves, producing an inward migrationwaves, producing an inward migration
Massive protoplanet can open an Massive protoplanet can open an annular gap in discannular gap in disc
Form of gap & gas accretion rate: Form of gap & gas accretion rate: function of visc., planet mass, heightfunction of visc., planet mass, height
Causes of MigrationCauses of Migration Protoplanet orbits in gap, interacts Protoplanet orbits in gap, interacts
with outer discwith outer disc Leads to inward migration ~10Leads to inward migration ~1055 yr yr Balbus & Hawley (1991): angular Balbus & Hawley (1991): angular
momentum transport, inward momentum transport, inward migration also originates from migration also originates from magnetorotational instability (MRI)magnetorotational instability (MRI)
Paper I: Turbulent DiscsPaper I: Turbulent Discs Focused on turbulent disc models prior Focused on turbulent disc models prior
to introducing a perturbing protoplanetto introducing a perturbing protoplanet Cylindrical disc models; no vertical Cylindrical disc models; no vertical
stratificationstratification Assume disc is adequately ionized for Assume disc is adequately ionized for
ideal MHD conditions; consider models ideal MHD conditions; consider models with no net magnetic fluxwith no net magnetic flux
Now on to planet-disc interaction...Now on to planet-disc interaction...
Planet-Disc ModelPlanet-Disc Model From paper I: H/r From paper I: H/r
= 0.1= 0.1 Stress Parameter Stress Parameter
= 5x10 = 5x10-3-3
Stellar Mass = Stellar Mass = 1 M1 Msolarsolar
Planet Mass must Planet Mass must be >3 Jupiter be >3 Jupiter masses: consider 5 masses: consider 5 MMJupiterJupiter
Thinner discs and Thinner discs and less massive less massive planets are more planets are more desirable: H/r = desirable: H/r = 0.05 /1 M0.05 /1 MJupiterJupiter
Both are Both are computationally computationally impossible nowimpossible now
Initial Model SetupInitial Model Setup
Protoplanet ModelProtoplanet Model Modeled as Hill Modeled as Hill
sphere @ r = 2.2sphere @ r = 2.2 Roche lobe Roche lobe
atmosphere around atmosphere around planet before gap planet before gap construction construction completecomplete
Not accretion Not accretion directly onto planetdirectly onto planet
Protoplanet ModelProtoplanet Model Nelson et al. (2000): Nelson et al. (2000):
matter accretes matter accretes from atmosphere from atmosphere onto planetonto planet
Cannot simulate Cannot simulate that here: effect on that here: effect on mag. field difficultmag. field difficult
Atmosphere gains Atmosphere gains matter, not planetmatter, not planet
Another ProblemAnother Problem Directly imbedding planet into disc Directly imbedding planet into disc
produces no gapproduces no gap N&P carve out small gap @ r = 2.2N&P carve out small gap @ r = 2.2 Justifed because magnetic energy Justifed because magnetic energy
and stress remain sameand stress remain same
Numerical ResultsNumerical Results Continuity Eq. for Continuity Eq. for
disc surface density:disc surface density:
Equation of Motion:Equation of Motion:
Indentical to Viscous Indentical to Viscous Disc TheoryDisc Theory
Time Evolution of ModelTime Evolution of Model Simulation ran for Simulation ran for
100 planetary orbits100 planetary orbits Initial gap Initial gap
deepeneddeepened Accretion onto Accretion onto
central parts central parts produced produced something like something like central cavitycentral cavity
Time Evolution of ModelTime Evolution of Model Magnetic Energy Magnetic Energy
value maintained value maintained throughout throughout simulationsimulation
Protoplanetary Protoplanetary perturbations do perturbations do not have strong not have strong globalglobal effect on effect on the dynamo the dynamo
Time Evolution of ModelTime Evolution of Model However, planet However, planet
effects turbulence effects turbulence locallylocally
Planet creates an Planet creates an ordered field ordered field where material where material passes through passes through spiral shocksspiral shocks
Protoplanet in Disc GapProtoplanet in Disc Gap
Magnetic Field in Disc GapMagnetic Field in Disc Gap
Stress Parameter vs. TimeStress Parameter vs. Time Magnetic stress is Magnetic stress is
same as without same as without the planetthe planet
Total stress peaks Total stress peaks due to spiral due to spiral waves launched waves launched by protoplanetby protoplanet
Stress vs. RadiusStress vs. Radius Total stress and Total stress and
magnetic magnetic component component become large become large around planetaround planet
Further out, value Further out, value is similar to disc is similar to disc w/o planetw/o planet
Angular Momentum FluxAngular Momentum Flux High Reynolds High Reynolds
stress immediately stress immediately outside gapoutside gap
High Magnetic High Magnetic stress at large radiistress at large radii
Magnetic stress is Magnetic stress is non-zero through non-zero through gap, transferring L gap, transferring L without tidal torquewithout tidal torque
Angular Momentum FluxAngular Momentum Flux Flux Profile at later Flux Profile at later
time:time: Same Same
characteristics: characteristics: stable pattern of stable pattern of behavior has been behavior has been established quicklyestablished quickly
Inward migration Inward migration results ~10results ~1044 orbits orbits
Turbulent vs. Viscous DiscTurbulent vs. Viscous Disc Spiral waves ‘sharper’ in viscous Spiral waves ‘sharper’ in viscous
discdisc
Turbulent vs. Viscous DiscTurbulent vs. Viscous Disc Little circular flow around protoplanetLittle circular flow around protoplanet
Turbulence could effect accretion rateTurbulence could effect accretion rate
Turbulent vs. Viscous DiscTurbulent vs. Viscous Disc Turbulent disc Turbulent disc
appears to have appears to have smaller stress smaller stress parameter parameter
Could be artifact Could be artifact of simulation OR of simulation OR magnetic magnetic communication communication across the gapacross the gap
ConclusionsConclusions Demonstrated many of phenomena Demonstrated many of phenomena
seen in laminar viscous discseen in laminar viscous disc Planet launched spiral waves that Planet launched spiral waves that
transport angular momentumtransport angular momentum Turbulent disc has smaller Turbulent disc has smaller
– Mag. fields transport L across the gapMag. fields transport L across the gap Magnetic breaking around planetMagnetic breaking around planet
– MightMight slow mass accretion rate slow mass accretion rate
ReferencesReferences ““The interaction of a giant planet with a disc with The interaction of a giant planet with a disc with
MHD turbulence II:MHD turbulence II:The interaction of the planet with the disc”The interaction of the planet with the disc”Papaloizou & Nelson 2003, MNRAS 339 (4), 993-1005Papaloizou & Nelson 2003, MNRAS 339 (4), 993-1005
““The interaction of a giant planet with a disc with The interaction of a giant planet with a disc with MHD turbulence I:MHD turbulence I:The initial turbulent disc models”The initial turbulent disc models”Papaloizou & Nelson 2003a, MNRAS 339, 923Papaloizou & Nelson 2003a, MNRAS 339, 923
Images from:Images from:– http://astron.berkeley.edu/~gmarcy/http://astron.berkeley.edu/~gmarcy/
0398marcybox4.html0398marcybox4.html– http://www.sns.ias.edu/~dejan/CCS/work/SciArt/http://www.sns.ias.edu/~dejan/CCS/work/SciArt/