Die Wechselwirkung Planetarischer Nebel mit dem interstellaren Medium

1
Die Wechselwirkung Planetarischer Nebel mit dem
interstellaren Medium

• Florian Kerber, ST-ECF
• IWAA 2003,
• Sternwarte/Osservatorio astronomico Max Valier,
  Karneid, 4.10.2003

2
The Team

• Thomas Rauch (Univ. Bamberg, Tübingen)
• Hans Müller (Dartmouth College)
• Elise Furlan (Cornell Univ.)
• Fabrizia Guglielmetti (Int. Max-Planck Res.
  School)
• Roberto Mignani (ESO)
• Eva-Maria Pauli (Univ. Bamberg)
• Miguel Roth (Carnegie)
• Andreas Wicenec (ESO)

3
Outline

• Stellar Evolution and PNe
• What is so interesting about old Planetary
  Nebulae ?
• Interaction PN-ISM theoretical considerations
• Interaction PN-ISM observational evidence
• New results PNe as Galactic Citizens

4
The Hertzsprung-Russell Diagram

• Temperature vs Luminosity

5
The HRD II

• Main Sequence
• Red Giant
• Asymptotic Giant
• Thermal Pulses
• Planetary Nebula
• White Dwarf

6
Planetary Nebula

• Thick AGB wind
• Thin stellar wind
• Hot central star
• Ionized PN shell
• Thin plasma 10000 K

7
PN Emission Line Spectrum

• Recombination lines
• H
• He
• Forbidden lines
• C, N, O, S

8
What is so interesting about old PNe ?

• The typical Galactic PN is an old PN
• They drive the chemical evolution of galaxies
• PNe contain matter enriched in metals
• Last observable phase before return to ISM
• Complex physics at the PN-ISM interface
• Measurable quantities
• Comparison with theory/models
• PN can be used as probe of ISM

9
The not-so-central central star

• A59 P 2-3. On a deep exposure, the apparent
  arc shape is seen to be just the brightest
  portion of a nearly spherical nebula. The CSC
  central star candidate discussed here is
  off-center, lying closer to the bright northern
  arc. It is the bluest star observed hence we
  have classified it as possible. (Kwitter et
  al., 1988, AJ, 96, 997)

?
10
Concept of PN-ISM Interaction

• Young PNe
• ne (PN) gtgt ne (ISM) - no significant influence on
  PN
• Middle-aged PNe
• P(ISM) upstream ? P(PN shell) no (v
  vexp)2 ne (PN) c2 ? ncrit ((v
  vexp)/c)2 no
• ne (PN) increases - by 2x (Kerber et al. 2000)
• Asymmetric brightness distribution
• Recombination rate goes up
• Lower degree of excitation (EC drops by 1 or 2)

Borkowski et al. (1990), Soker et al. (1991)
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Observational Evidence for Interaction

• Increased ne (PN) in interaction zone

Inner region Higher Excitation
Interaction zone Lower Excitation
12
Concept of PN-ISM Interaction

• Old PNe
• ne (PN) continues to decrease
• vexp of PN slowed (upstream) ? deformation of PN
• Instabilities (Rayleigh-Taylor)
• severe deformation of PN
• break-up of PN shell
• Influence of the ISMs magnetic field (Soker
  Dgani 1997)
• Expansion of PN shell is stopped no (v
  vexp)2 ne (PN) vexp2 ? nstop (v/vexp)2
  no
• CS moves away from geometric center

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PNe move with respect to the ISM
H?
O III
?
PN G315.908.2 (MeWe 1-4)
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Trying to get a quantitative picture

• 50 PNe observed
• Narrow-band imaging (H?, OIII, NII, OII)
• Long-slit spectroscopy PN
• Plasma diagnostics, density, excitation,
  abundances
• Radial velocity, expansion of PN
• Long-slit spectroscopy Central Star
• H/He-rich, log g, Teff , chemical composition,
  distance
• Radial velocity

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Instability
new
PN G272.801.0 (PMR 1)
PN G236.0-10.6 (HaWe 9)
PN G309.201.3 (SuWt 1)
PN G272.4-05.9 (MeWe 1-1)
PN G296.303.1 (KFR 1)
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Instability in A21
17
Sh 2-174 the PN abandoned by its CS
N II
O III
Tweedy Napiwotzki, 1994, AJ, 108, 978
18
Proper Motion of PNe

• Cudworth (1974, AJ, 79, 1384)
• 51 PNe, 2 epochs 10 yr apart, accuracy 1- 10
  mas/yr
• Hipparcos Aug. 89 - Aug. 93
• Hipparcos 120,000 stars at 1 mas/yr
• Tycho-2 2.5 million stars at 2.5 mas/yr
• GSC II, USNO-B photographic all sky
• ca 50 yr time basis, 109 objects, 21 mag, 5 - 20
  mas/yr
• UCAC ongoing, full sky coverage by mid-2004
• 10 - 16 mag, accuracy 20 -70 mas/yr

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Galactic Kinematics of PNe

• RA, DEC, PM components, distance vrad
• Galactic System X, Y, Z U, V, W with R0 8.5
  kpc
• Galactic Potential (Allen Santillan 1991)
• Analytical, symmetric wrt to Z-axis,
  time-independent, rotation curve
• Population membership thin or thick disk, halo
• Distinct regions in the U-V velocity and Jz-e
  diagram
• Calibration sample MS stars with detailed
  abundance analysis

Pauli et al., 2003, AA, 400, 877
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Galactic Kinematics of PNe

• Jz-e diagram

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Galactic Orbits of interacting PNe

• PN G124.010.7 (EGB 1) - thin disk

?
PM 18 4, -16 4 mas/yr
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Galactic Orbits of interacting PNe

• PN G 111.011.6 (DeHt 5) - thin disk

?
PM -12 4, -18 4 mas/yr
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Galactic Orbits of interacting PNe

• PN G 218.9-10.7 (HDW 5) - thick disk

PM 2 4, -24 4 mas/yr
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Galactic Orbits of interacting PNe

• PN G080.3-10.4 - thin disk

PM -4 4, 16 4 mas/yr
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Galactic Orbits of interacting PNe

• PN G025.340.8 (IC 4593) - thick disk ?

PM -8.7 1.6, 4.1 1.5 mas/yr
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Galactic Orbits of interacting PNe

• PN G158.600.7 (Sh 2-216) - thin disk

?
PM 25 2, -13 2 mas/yr
New PM 31.7 1.0, -12.7 1.0 mas/yr
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Galactic Orbits of interacting PNe

• PN G030.606.2 (Sh 2-68) - thick disk ?

?
N II
O III
PM -19.9 5.5, -49.3 5.5 mas/yr
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Galactic Orbits of interacting PNe

• PN G030.606.2 (Sh 2-68) - thick disk ?

PM -19.9 5.5, -49.3 5.5 mas/yr
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Galactic Orbits of interacting PNe

• PN G345.2-08.8 (Tc 1) - thick disk

PM -1.6 2.2, -11.4 2.2 mas/yr
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Galactic Orbits of interacting PNe

• PN G120.318.3 (Sh 2-174) - thin disk

PM -28 4, 4 6 mas/yr
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Modeling the Interaction

• ISM
• 0.2/cm3
• 52 km/s
• 8000 K
• AGB
• up to 50 ksec
• thermal Pulse
• post-AGB at 58 ksec
• PN

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Summary and Outlook

• Solid observational database for PNe interacting
  with ISM (imaging and spectroscopy)
• PM, Galactic Orbits and population membership
• Analysis of CSs properties
• Input for models, towards quantitative
  understanding of interaction processes
• High resolution spec vrad CS vs PN, velocity
  field
• Distances ...

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The ISMs Magnetic Field

• Instability and stripping of nebulae matter

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Galactic Kinematics of PNe

• U-V velocity diagram

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PN G292.500.9 (NeVe 3-6)
H?
O III