The Challenges of the LastThe Challenges of the LastDecade of Observations of Decade of Observations of

PNePNe

Gdansk June, 2005Gdansk June, 2005Gdansk June, 2005Gdansk June, 2005

Bruce BalickBruce BalickUniversity of WashingtonUniversity of Washington

HST image by Hans Van Winckel, and Martin Cohen

Model by Vincent Icke

The Challenges of the LastThe Challenges of the LastDecade of Observations of Decade of Observations of

PNePNe• • IntroductionIntroduction: In the past decade HST, : In the past decade HST, Spitzer, and many other new tools have Spitzer, and many other new tools have opened new ranges of spectral coverage opened new ranges of spectral coverage and, at the same time, pushed the and, at the same time, pushed the imaging observations to the milliarcsec imaging observations to the milliarcsec domain. domain.

• • IntroductionIntroduction: In the past decade HST, : In the past decade HST, Spitzer, and many other new tools have Spitzer, and many other new tools have opened new ranges of spectral coverage opened new ranges of spectral coverage and, at the same time, pushed the and, at the same time, pushed the imaging observations to the milliarcsec imaging observations to the milliarcsec domain. domain.

Gdansk June, 2005Gdansk June, 2005Gdansk June, 2005Gdansk June, 2005

• • ConclusionConclusion: The endpoint of stellar : The endpoint of stellar evolution is the startpoint for uncovering evolution is the startpoint for uncovering significant new insights into late stages of significant new insights into late stages of stellar evolution.stellar evolution.

• • ConclusionConclusion: The endpoint of stellar : The endpoint of stellar evolution is the startpoint for uncovering evolution is the startpoint for uncovering significant new insights into late stages of significant new insights into late stages of stellar evolution.stellar evolution.

• • DataData: Observational progress has been : Observational progress has been dizzying. dizzying. • • DataData: Observational progress has been : Observational progress has been dizzying. dizzying. • • Most theoreticians are just starting to Most theoreticians are just starting to recover. recover. • • Most theoreticians are just starting to Most theoreticians are just starting to recover. recover.

H-R Diagram, 1 MsunH-R Diagram, 1 Msun

1 solar mass, no rotation1 solar mass, no rotation

Sackman, Boothroyd & Kraemer 1993 Astrophysical Journal 417 473

Inter-pulse Period = 105 y

Ascending the “AGB”; preparing to eject a protoPNAscending the “AGB”; preparing to eject a protoPN

Betelgeuse - Betelgeuse -

RoundPNe

from Isotropic

WindsKwok, Purton,

& Fitzgerald 1978; Dyson, Pik’elner…

RoundPNe

from Isotropic

WindsKwok, Purton,

& Fitzgerald 1978; Dyson, Pik’elner…

Challenge: If winds are Challenge: If winds are Isotropic then why aren’t Isotropic then why aren’t all PNe round?all PNe round?

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• <20% are round. The other symmetries of PNe fall into clear ymmetries of PNe fall into clear patterns and categories.patterns and categories.• do almost all dying do almost all dying

AGB/post AGB AGB/post AGB stars stars build collimators? build collimators? • How?How?

Challenge. What Challenge. What paradigm?paradigm?

• GISW models were generally successful in explaining the large-scale features of most PNe.

HST upended our HST upended our complacencycomplacency

Gdansk June, 2005Gdansk June, 2005Gdansk June, 2005Gdansk June, 2005

Cat’s EyeCat’s EyeNGC 6543NGC 65431” seeing1” seeing[N II][N II][O III][O III]

The devil is in the The devil is in the details…details…

JetsJets

FLIERsFLIERs

Paradigm lost?Paradigm lost?

Challenge: Why are many outflows stunningly

collimated, esp pPNe?

Challenge: Why are many outflows stunningly

collimated, esp pPNe?

• • where there’s collimation, there must where there’s collimation, there must be collimatorsbe collimators• • where there’s collimation, there must where there’s collimation, there must be collimatorsbe collimators

Kwok, Hrivnak, Su et al

He 3-401He 3-401

QuickTime™ and aTIFF (Uncompressed) decompressor

are needed to see this picture.

He 3-1475He 3-1475

He 2-90He 2-90 CRL 618CRL 618

Challenge: The disks are too thin!

Challenge: The disks are too thin!

Q: Challenge: How do dying stars make disks without accretion? A: Mass-transfer binaries?

Q: Challenge: Can accretion do it alone? What’s the collimator? A: At best, a thick disk.

Challenge: Too Many Axes, Not Enough

Disks

Challenge: Too Many Axes, Not Enough

Disks

Sahai & Trauger 1998

CRL 2688CRL 2688

redshiftedredshiftedblueshiftedblueshifted

Red = H2 2.12 mBlue = scattered starlightContours = 12 CO

Red = H2 2.12 mBlue = scattered starlightContours = 12 CO

Kastner et al 2001

Cox et al 2002

7 pairs!7 pairs!7 pairs!7 pairs!

Challenge: CO studies of Challenge: CO studies of outflowsoutflows

show HUGE momentum show HUGE momentum excess!excess!

• • Bujarrabal, Alcolea, and their collaborators: Bujarrabal, Alcolea, and their collaborators: radiation-driven winds aren’t a radiation-driven winds aren’t a complete answercomplete answer

• • Bujarrabal, Alcolea, and their collaborators: Bujarrabal, Alcolea, and their collaborators: radiation-driven winds aren’t a radiation-driven winds aren’t a complete answercomplete answer

nameMass

Msol

P = MV(gm cm s-1)

E(erg) P/(L/c)

CRL 618 .65 2.1 1039 1.8 1045 1.8 104

CRL 2688 .69 2.2 1039 1.7 1045 2.2 104

M2-56 .01 3.0 1037 2.0 1044 3.3 103

Frosty Leo .36 8.0 1038 4.5 1044 7.0 104

> gravitational powering by close binaries?> gravitational powering by close binaries?

NGC 6543

BD+30˚3639

NGC 7009

Ellipticals with Attitude:

soft X rays fill the bubble

Ellipticals with Attitude:

soft X rays fill the bubble

Challenge: Changing Wind Challenge: Changing Wind Mode?Mode?

NGC 6543

Corradi et al 2004

OH 231.8+4.2Alcolea et al. (2001) A&A 373,932OH 231.8+4.2Alcolea et al. (2001) A&A 373,932

Challenge: “Hubble Challenge: “Hubble Flows”Flows”

Result: ages ≈ 5700 yr Result: ages ≈ 5700 yr

Corradi et al 2002Corradi et al 2002

He2–104He2–104

Menzel 3 Santander et al 2004

Menzel 3 Santander et al 2004

275 km s-1

Bottom line: all major components have nearly the same expansion ages.

Bottom line: all major components have nearly the same expansion ages.

Challenge: Challenge: Steady Winds or Steady Winds or Eruptions?Eruptions?

Physics of “Hubble” Physics of “Hubble” outflows:outflows:• • sudden ejection + sudden ejection + ballistic flow?ballistic flow?• • self similar? (adiabatic?)self similar? (adiabatic?)• • magnetic “event” (see magnetic “event” (see Frank talk)Frank talk)

• • What processes orchestrate the What processes orchestrate the spectacular grand finale at the spectacular grand finale at the

AGB tip?AGB tip?• • Whither all that outflow Whither all that outflow momentum?momentum?

Magnetized Wind Collimation ModelMagnetized Wind Collimation Model

QuickTime™ and aTIFF (LZW) decompressor

are needed to see this picture.

Isodensity surfacesIsodensity surfaces

IRAS 17106-3046IRAS 17106-3046Kwok et al. 2000Kwok et al. 2000

IRAS 17106-3046IRAS 17106-3046Kwok et al. 2000Kwok et al. 2000

CarinaeCarinaeMorse et al. 1998Morse et al. 1998

CarinaeCarinaeMorse et al. 1998Morse et al. 1998

Steady magnetized windSteady magnetized wind carrying dipolar field.carrying dipolar field.

Stellar rotationStellar rotation• • flings equatorial fields andflings equatorial fields and creates a (passive) diskcreates a (passive) disk• • winds polar fields and winds polar fields and traps high-latitude windstraps high-latitude windsSteady state solution;Steady state solution; can’t make Hubble flowcan’t make Hubble flow

Magnetic “bomb” next.Magnetic “bomb” next.

Grand Challenge: Grand Challenge: What creates and What creates and shapes PNe?shapes PNe?

Astronomy: How do stars create high-order symmetries in a brief event?

• • Internal?Internal? Thermonuclear pulse?Thermonuclear pulse? Symmetry imposed by emerging Symmetry imposed by emerging BB fields? fields?

• • External?External? Sudden CE phase or tidal onset?Sudden CE phase or tidal onset?

• • What generates plural What generates plural symmetry axes?symmetry axes?

Astronomy: How do stars create high-order symmetries in a brief event?

• • Internal?Internal? Thermonuclear pulse?Thermonuclear pulse? Symmetry imposed by emerging Symmetry imposed by emerging BB fields? fields?

• • External?External? Sudden CE phase or tidal onset?Sudden CE phase or tidal onset?

• • What generates plural What generates plural symmetry axes?symmetry axes?

ApplauseApplause

M2-9: 40 years of mischief

M2-9: 40 years of mischief

M2–9 HST motion pictureM2–9 HST motion picture

QuickTime™ and aGIF decompressorare needed to see this picture.

Common Envelope Collimator?Common Envelope Collimator?

Colors: OutflowVelocity Field

Wire Frame:IsodensitySurface

Colors: OutflowVelocity Field

Wire Frame:IsodensitySurface

F. Garcia, A.Frank, N. Soker, B. Balick, in progressF. Garcia, A.Frank, N. Soker, B. Balick, in progress

Magnetic fields, sudden Ionization &

heating, steady winds

Magnetic fields, sudden Ionization &

heating, steady winds

Early MHD SimulationEarly MHD Simulation

Model V, Garcia-Segura et alModel V, Garcia-Segura et al

1999 Astrophys J, 517, 7671999 Astrophys J, 517, 767

Mz 3 ImageHeuristicModel

Mz 3 ImageHeuristicModel

If we assume: Mcore = 0.5 Msun

Vesc = 1000 km/sMEgg ≈ 0.062 Msun (Bujarrabal et al. 2001)

REgg ≈ 104 AU

Some “al” #’s:Then: Rcore ≈ 0.2 Rsun

Bcore ≈ 105 GaussKEcore ≈ 1046 ergTspin-down ≈ 100 years

Thompson, Hines, & Sahai (1997)

??

Magnetic “Bomb”: sudden emergence of surface B

fieldsFrank, Matt & Balick (in progress)

Magnetic “Bomb”: sudden emergence of surface B

fieldsFrank, Matt & Balick (in progress)

“Discovery of Magnetic Fields in CPNs”Jordan, Werner, O’Toole, ASP Conf Ser (LANL Prerprints)

ESO-VLT1 + FORS1

H+HeIIH+HeII H+HeIIH+HeII

H+HeIIH+HeIIHeII 4686HeII 4686

NGC 1360stellar circularpolarizationand modelsfor 2832G(-1343, 1708,2832, 194 G;4 obs/42 days)

LS1362Abell 36?EGB 5?

Whither the fields?Whither the fields?

“Dynamos in AGB stars as the origin of magnetic fields shaping planetary nebulae”E.G. Blackman, A. Frank, J.A. Markiel, J.H. Thomas, H.M. van HornNature, 409, 485-487 (25 January 2001)

Wherefore the fields?Wherefore the fields?… we show that an asymptotic-giant-branch (AGB) star can indeed generate a strong magnetic field, having as its origin a dynamo at the interface between the rapidly rotating core and the more slowly rotating envelope of the star. The fields are strong enough to shape the bipolar outflows that produce the observed bipolar planetary nebulae.

“A fossil origin for the magnetic field in A-stars and white dwarfs”J. Braithwaite and H.C. SpruitNature, 431, 819-821 (14 October 2004)

Numerical simulations of the shape of the magnetic field lines in a magnetic star.

Field lines protruding through the surface of the star (red)are held together and stabilized by the twisted ring inside the star (blue).

This magnetic field configuration drifts slowly outward(over a period of hundreds of millions of years) under the influence of the finite electrical resistivity of the star, then distorts into the shape of the seam on a tennis ball.

Wherefore the fields?Wherefore the fields?