Beyond the Textbook:Beyond the Textbook:Why Planetary Nebula are the Why Planetary Nebula are the

Most Exciting Problem in Most Exciting Problem in Astrophysics.Astrophysics.

Adam FrankAdam FrankUniversity of RochesterUniversity of Rochester

A Cast of ManyA Cast of Many

Eric Blackman (UR), Orsola De Marco, Bruce BalickEric Blackman (UR), Orsola De Marco, Bruce Balick

Sean Matt (UV)Sean Matt (UV)

Jason Nordhaus (UR), T. Dennis (UR)Jason Nordhaus (UR), T. Dennis (UR)

AstroBEAR AMR MHDAstroBEAR AMR MHD

Andrew Cunningham (UR)Andrew Cunningham (UR)

Kris Yirak (UR)Kris Yirak (UR)

The StoryThe Story

PNe are penultimate evolutionary stage PNe are penultimate evolutionary stage of low/intermediate mass stars. of low/intermediate mass stars.

Some view field as mostly “done.”Some view field as mostly “done.” New observational/theoretical studies New observational/theoretical studies

show both PNe and late stages of stellar show both PNe and late stages of stellar evolution NOT UNDERSTOOD.evolution NOT UNDERSTOOD.

New models invoke processes at New models invoke processes at frontiers of modern astrophysics frontiers of modern astrophysics (magnetic fields, jets, accretion disk)(magnetic fields, jets, accretion disk)

Strong Lab Astro connectionStrong Lab Astro connection

Stellar and PNe Evolution: Stellar and PNe Evolution: The Textbook PictureThe Textbook Picture

• AGB -> pPNe-> PNe -> WD

• ‘Proven” evolutionary Tracks

•Locus of evolution vs. temporal sequence.

PNe Shapes; Solution circa 1992:PNe Shapes; Solution circa 1992: Planetary Nebula as Wind Blown BubblesPlanetary Nebula as Wind Blown Bubbles

White dwarf fast wind White dwarf fast wind sweeps up Red Giant sweeps up Red Giant slow wind.slow wind.

Dense shell of Dense shell of snowplowed gas snowplowed gas becomes nebulabecomes nebula

Bipolar PNe

Planetary Nebulae: Modern ViewPlanetary Nebulae: Modern ViewNarrow Waist Bipolar OutflowsNarrow Waist Bipolar Outflows

Point symmetry

Aspherical Bubbles?Aspherical Bubbles?Generalized Wind ModelGeneralized Wind Model

Imagine slow wind Imagine slow wind emerges with a emerges with a doughnut shape.doughnut shape.

““Inertial Confinement”Inertial Confinement” Fast wind escapes Fast wind escapes

through doughnut through doughnut holes.holes.

Shaping Starts Early!Shaping Starts Early!Aspherical proto-Planetary NebulaeAspherical proto-Planetary Nebulae

Multi-Polar OutflowsMulti-Polar Outflows“Young PNe”“Young PNe”

• T* ~ 30000 K

• Ionization fronts just Beginning to break out.

• “Starfish” phase

Momentum Excess in pPNeMomentum Excess in pPNeBujarrabal et al 2001Bujarrabal et al 2001

Outflow shaping begins during proto-PNe stageOutflow shaping begins during proto-PNe stage– Acceleration time short (< 100 y?)Acceleration time short (< 100 y?)

pPNe show pronounced momentum excess!pPNe show pronounced momentum excess!– Radiation driving Radiation driving can notcan not account for outflows account for outflows

namename MassMassMMsolsol

P = MVP = MV(gm cm s(gm cm s--

11))

EE(erg)(erg)

P/(L/c)P/(L/c)

CRL 618CRL 618 .65.65 2.1 102.1 103939 1.8 101.8 104545 1.8 101.8 1044

CRL 2688CRL 2688 .69.69 2.2 102.2 103939 1.7 101.7 104545 2.2 102.2 1044

M2-56M2-56 .01.01 3.0 103.0 103737 2.0 102.0 104444 3.3 103.3 1033

Frosty Frosty LeoLeo

.36.36 8.0 108.0 103838 4.5 104.5 104444 7.0 107.0 1044

)//( cLP

Need a New ParadigmNeed a New Paradigm

MHDMHD Binary StarsBinary Stars

Why MHD for PNe?Why MHD for PNe?

Hydrodynamic Models can Hydrodynamic Models can not recover morphologies.not recover morphologies.– (Garcia-Segura, Lopez etc)(Garcia-Segura, Lopez etc)

!! !! Fields observed in PNe Fields observed in PNe !!!!– Nebular gas (B ~ mG)Nebular gas (B ~ mG)

(Miranda et al 2001, Herpin 2004)(Miranda et al 2001, Herpin 2004)

– Central star (B ~ kG)Central star (B ~ kG) (Jordan et al 2004)(Jordan et al 2004)

Central stars -> hard X-raysCentral stars -> hard X-rays (Kastner et al, Chu et al)(Kastner et al, Chu et al)

PN masers (Miranda et al)

PN X-rays ( Chu et al)

MHD and Outflows:MHD and Outflows:Magneto-Rotational Launching (MRL)Magneto-Rotational Launching (MRL)

* GRAND CHALLENGE PROBLEM* GRAND CHALLENGE PROBLEM– MRL -> MRL -> EVERY COLLIMATED OUTFLOW ENVIRONMENT!EVERY COLLIMATED OUTFLOW ENVIRONMENT!

YSOs, AGN, micro-Quasars: GRBs, SNeYSOs, AGN, micro-Quasars: GRBs, SNe

Many forms of theory Many forms of theory (Blandford & Payne 1985, Shu et al (Blandford & Payne 1985, Shu et al 1994)1994)

– Theory/Simulation – “Fling” (BTheory/Simulation – “Fling” (Bpp) vs. “Spring” (B) vs. “Spring” (B))

Theory of Theory of jet launching and collimationjet launching and collimation

Mature Paradigm – Ex. HH jet rotation -> Mature Paradigm – Ex. HH jet rotation -> disk footpoints disk footpoints (Cabrit et al 2006)(Cabrit et al 2006)

MRL BasicsMRL Basics

Magneto-centrifugal Models“Fling” (Tsinganos et al)

Magnetic Tower Models“Spring” (Kato et al)

Disk-Star Models(Ferreria et al)

Binary Stars:Binary Stars:Common Common Envelope Envelope EvolutionEvolution

Two (+) evolutionary channels

1. Mass transfer binary

2. Merger ->Rapidly spinning object

3 Secondary break-up Disk around primary

Binary Stars Disk & Binary Stars Disk & JetsJets

Link to other Link to other Astro systems!Astro systems!

Disks+JetsDisks+Jets– Young StarsYoung Stars– AGNAGN

Binary+Jets+DiskBinary+Jets+Diskss– CVsCVs– Micro-quasarsMicro-quasars

Our Proposal Part 1Our Proposal Part 1

2 Flavors of MHD Launching2 Flavors of MHD Launching Explosive or ContiniousExplosive or Continious

The Tool:The Tool:AstroBEAR AMR CodeAstroBEAR AMR Code

• “Block” AMR

• Choice of solvers/integrators

• Parallel – load balance

• Multi-physics modules:

Ionization and H2Chemistry

heat conduction

*self-gravity

*rad trans (diff limit)

MHD Flux conservation via CT

Cunningham, Frank, Varniere & Mitran 2007*Cunningham, Frank, Varniere & Mitran 2007*

Radiative Outflows in Radiative Outflows in Heterogeneous MediaHeterogeneous MediaCunningham, Frank, Varniere & Mitran 2007*Cunningham, Frank, Varniere & Mitran 2007*

MRL Model 1: FlingMRL Model 1: FlingBlackman, Frank & Welch 01Blackman, Frank & Welch 01

Both Star and Disk create MRL outflowsBoth Star and Disk create MRL outflows

– Disk forms via disruption of companion Disk forms via disruption of companion (Soker, Livio, Reyes-Ruiz & Lopez)(Soker, Livio, Reyes-Ruiz & Lopez)

– Star and Accretion Disk each produce Star and Accretion Disk each produce wind (need binary).wind (need binary).

– Explain multi-polar flowsExplain multi-polar flows

– Scaling Argument fulfills power Scaling Argument fulfills power requirementsrequirements

sergRBBdVELw /103532 Energy requirement of Bujarrabal et al 2001Energy requirement of Bujarrabal et al 2001

MRL Model 1: MRL Model 1: Nested Wind SimulationsNested Wind SimulationsDennis, Yirak & Frank 2007* (AstroBEAR AMR MHD Dennis, Yirak & Frank 2007* (AstroBEAR AMR MHD Code)Code)

Slow Inner Wind Fast Inner Wind

MRL Model 1: MRL Model 1: FlingFling Detailed Disk ModelsDetailed Disk Models

Calculate “Full” MRL Disk SolutionsCalculate “Full” MRL Disk Solutions– Frank & Blackman 2004Frank & Blackman 2004

ii) Disk Around Companion ii) Disk Around Companion i)i) Disk Around Primary Disk Around Primary (companion disrupted)(companion disrupted)

Garica-Arrendondo & Frank 04Frank & Blackman 04

MRL Model 2: SpringMRL Model 2: SpringBlackman, Frank, Thomas & Van Horn Blackman, Frank, Thomas & Van Horn 2001 2001 NatureNature

Use model (Kawaler) Use model (Kawaler) Single Star (!)Single Star (!) – – Derive Derive (r) profile(r) profile

– Assume MS rotation profileAssume MS rotation profile– Evolve via rEvolve via r22 conservation on cylinders conservation on cylinders

Use calibrated dynamo to calculate Use calibrated dynamo to calculate fieldfield22

When AGB “atmosphere” peels off, When AGB “atmosphere” peels off, dynamo field (B = Bdynamo field (B = B) “unwinds” ) “unwinds”

Outflow generated with E ~ EOutflow generated with E ~ EpPNepPNe ((Bujarrabal)Bujarrabal)

MRL Model 2: SpringMRL Model 2: Spring Magnetized Rotating CoresMagnetized Rotating Cores

Matt, Frank & Blackman 2004, 2006Matt, Frank & Blackman 2004, 2006

Attempt to simplify and Attempt to simplify and simulate problem.simulate problem.

Initial conditions:Initial conditions: – Massive, magnetized ball, Massive, magnetized ball,

initiate rotation t = 0.initiate rotation t = 0.– axis aligned with dipole or axis aligned with dipole or

monopolemonopole– no inflow/outflowno inflow/outflow– Initially stagnant hydrostatic Initially stagnant hydrostatic

envelope Menvelope Mbb >> M >> Mee

RESULTS: – small scales

• -> B

• Bpressure drives outflow

• Bp lines opened

RESULTS : Field Geometry and Morphology

Dipole Field Split Monopole FieldSmall Scale

Large Scale

RESULTS: Acceleration and Energetics

•Polar shell exceeds local escape speed after 6 trot

• Polar and equatorial shells KE dominated,

• Polar interior Poynting Flux dominated. (GRBs)

SNe/GRB Magnetic ModelsSNe/GRB Magnetic ModelsWheeler et al 2007Wheeler et al 2007

pPNe as Explosions: pPNe as Explosions: CRL 618 CRL 618

CRL 618: pPNCRL 618: pPN– ““pure” Shock pure” Shock

excitationexcitation– No photo-ionizationNo photo-ionization

Multiple “lobes”Multiple “lobes”– Jets or BulletsJets or Bullets

Hint: “Rings” via Hint: “Rings” via vortex shedding.vortex shedding.

pPN as ExplositionspPN as ExplositionsBullets vs. Jets: Bullets vs. Jets: (Dennis, Frank & Balick 2007)(Dennis, Frank & Balick 2007)

• Run 2 and 3D sims of single jet or bullet.

• Compare emission maps

• Compare PV diagrams

• Bullets vortex shedding events match CRL 618 better

• Bullet PV diagram better fit as well.

MRL Models and MRL Models and Evolved StarsEvolved Stars

ConclusionConclusion MRL works for both pPNe and MRL works for both pPNe and

PNePNe Rich morphological potentialRich morphological potential

Tie Star(s) to NebulaTie Star(s) to Nebula

Magnetic Tower Models Magnetic Tower Models need Magnetic Fieldsneed Magnetic Fields

Our proposal: Part IIOur proposal: Part II

Questions:Questions: How do we get magnetic How do we get magnetic

fields in an AGB star?fields in an AGB star?

Dynamo ProblemsDynamo ProblemsCompare ECompare Erotrot with E with Emagmag

• EErotrot << E << Emagmag • Don’t have Lmag needed at end of AGB• Need source of differential rotation - binary

• Dynamos turn into B•Dynamo cycle should operate throughout AGB• Need Lmag at end of AGB

Binaries and Dynamos: CE Binaries and Dynamos: CE EvolutionEvolutionNordhaus & Blackman 2006Nordhaus & Blackman 2006Nordhaus, Blackman & Frank 2006Nordhaus, Blackman & Frank 2006

Calculate fraction of the orbital energy released by the companion and used for envelope ejection .

• Secondary produces drag luminosity. Balance via change in gravitational energy companion.

• Calculate end states, (r)• Use mean field dynamo equations to calculate AGB fields

Dynamos in AGB StarsDynamos in AGB StarsNordhaus, Blackman & Frank 2006Nordhaus, Blackman & Frank 2006

No companion Case

1. Dynamo dies after t < 50 years

2. Can maintain with convective reseeding but only with special conditions.

Dynamos in AGB StarsDynamos in AGB StarsNordhaus, Blackman & Frank 2006Nordhaus, Blackman & Frank 2006

With Companion Case

1. CE evolution stirs inner regions.

2. re-supplied.

3. Magnetic or Thermal Outflow.

Direct Envelope Ejection

Outflow is predominately equatorial.

Dynamo Driven Ejection

Outflow is aligned around the rotationaxis and is magnetically collimated.

Disk Driven Ejection

Shred SecondaryOutflow is aligned with rotation axis.

Varniere, Quillen & Frank 2005

Disks and pAGB starsDisks and pAGB starsNordhaus et al 2007Nordhaus et al 2007

““Transitional Disks” Transitional Disks” with inner holes with inner holes common in YSOs common in YSOs – Origin: Planets, Origin: Planets,

evaporationevaporation SEDs yield properiesSEDs yield properies Disks in pAGB stars Disks in pAGB stars

also appear common also appear common – >25% van Winkle et >25% van Winkle et

alal pAGB stars SEDs pAGB stars SEDs

also show holes. also show holes. D’Alessio et al 2005HD179821

Dynamo Models and Dynamo Models and Binary StarsBinary Stars

ConclusionConclusion Single stars dynamos can’t workSingle stars dynamos can’t work

Binary star dynamos can Binary star dynamos can generate needed fields to power generate needed fields to power

explosive outflowsexplosive outflows

Conclusions Conclusions

Magneto-rotational models promising for Magneto-rotational models promising for PNe/pPNe.PNe/pPNe.

physics applicable to variety of objects physics applicable to variety of objects (GRB/SNe, YSOs)(GRB/SNe, YSOs)

Binary Stars must play critical role.Binary Stars must play critical role. Accretion disks also likely to be presentAccretion disks also likely to be present