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Correlation of PN morphology and nebular parameters

Correlation of PN morphology and nebular parameters. Arturo Manchado Instituto de Astrofísica de Canarias. Colaborators. Eva Villaver STSCI Letizia Stanghellini STSCI Martín Guerrero Instituto de Astrofísica de Andalucía. PNe morphology vs. stellar evolution.

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Correlation of PN morphology and nebular parameters

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  1. Correlation of PN morphology and nebular parameters Arturo Manchado Instituto de Astrofísica de Canarias

  2. Colaborators Eva Villaver STSCI Letizia Stanghellini STSCI Martín Guerrero Instituto de Astrofísica de Andalucía

  3. PNe morphology vs. stellar evolution An AGB star can lose up to 80% of its mass Round Interacting wind model: The PN is formed by the interaction of a low density fast wind with a high density slow wind (e.g Kwok, Purton & Fitzgerald 1978, ApJ 219, 17) First observational evidence hot bubble in NGC 7009 Guerrero, Gruendl, Chu 2002, A&A 387, L1 Elliptical Interacting wind model with an ecuatorial density enhancement Frank, Balick, Icke, Mellema 1993, ApJ 404, L25 Mellema 1995, "Asymmetrical PN", ed. Harpaz, p. 229

  4. Jets & ansae Frank, A., Balick, B., Livio, M. 1996ApJ, 471, L53 Bipolar Binaries, commom envelope phase, substellar interaction (Soker, 1997, ApJSS, 112, 487) Magnetic fields  García-Segura et al. 1999 ApJ, 517, 767 Pointsymmetric García-Segura, G. & López, J.A. 2000ApJ, 544, 336 Muliple Shell PNe Villaver , Manchado, García-Segura, 2002 ApJ, 581, 1204 Steffen, M.; Schönberner, D. 2000A&A, 357, 180

  5. Interaction with the Insterstellar Medium Villaver, García-Segura, Manchado,2003 ApJ, 585, L49 20 km/s causes asymmetry due to interaction with the IM Morphology of PPNe Ueta , Meixner, Bobrowsky 2000AJ, 528, 861 sole - round, elliptical duplex - bipolar Review on Shapes and Saphing of Planetary Nebulae Balick, Frank 2002, Annu. Rev. Astron. Astrophys. 40, 439

  6. On theMorphology • Extended halosCurtis, H.D. 1918, Pub. Lick Obs. 13, 57 • "binebulous" and circular nebulaGreig , W. E., 1972,A&A 18, 70 • 108 of non-stellar PNebipolar, round, disk-like, and annularZuckerman, B., & Aller, L. H. 1986, ApJ 301, 772 • Round, elliptical and butterflyBalick , B. 1987, AJ 94, 671 • 41 Multiple shellsChu, Y. -H., Jacoby, G. H., & Arendt, R. 1987, ApJS 64, 529 • 250 PNe; stellar (S), elliptical (E), bipolar (B), pointsymmetric (P), and irregular (I)Schwarz, H. E., Corradi, R. L. M., & Melnik J.1992 A&AS 96, 23 • 243 PNe; round(R), bipolar(B), elliptical(E),quadrupolar(Q), pointsymmetric (P) Manchado, A., Guerrero, M.A., Stanghellini, L., & Serra-Ricart, M. 1996, The IAC Morphological Catalog of Northern Galactic PN, ed. IAC http://www.iac.es/nebula/nebula.html • 101 PNe Górny, S.K., Schwarz, H.E., Corradi, R.L.M., Winckel, H. van, 1999, A&AS 136, 145

  7. On the Morphology 50 MSPN,Corradi, Schoenberner, Steffen, Perinotto 2003, Mon. Not. R. Astron. Soc. 340, 417 35% show asymmetry 50 PNs with low-ionization structures (LISs), Goncalves, Corradi, Mampaso 2001, AJ 547, 302 56 PNs Large Magellanic CloudStanghellini, Blades, Osmern Barlow, Liu, 1999AJ, 510,687 Shaw, Stanghellini, Mutchler, Balick, Blades, 2001, 548, 727

  8. On the structural classification • Projection effects • Pottasch, S.R.1984Planetary Nebulae, ed. Reidel • Evolutionary scheme: early, middle, late; round, elliptical, butterflyBalick , B.1987, AJ 94, 671 • 50 % of PNe are Multiple Shell Planetary Nebulae • Chu, Y. -H., Jacoby, G. H., & Arendt, R. 1987, ApJS 64, 529 • Central star mass distribution different for bipolar and elliptical. • Elliptical are younger and more luminous than MPSN • Stanghellini, L., Corradi, R. L. M, & Schwarz, H. E,1993 A&A 279, 521

  9. Classification scheme Balick , B. 1987, AJ 94, 671

  10. Corradi, R. L. M, & Schwarz, H. E. 1995, A&A 293, 871 (250 PNe) • Elliptical z = 320 M < 1.1 M • Bipolar z = 130 M > 1.5 M • Overabundance helium, nitrogen and neon • Giant dimensions • Górny, S.K., Stasinska, G., & Tylenda, R. 1997, A&A 318, 256 (125 PNe) • Bipolar: higher mass, smaller z, higher N/O • Pointsymmetric a separate class • Elliptical z = 680 Mean Central Star mass 0.61 M • Bipolar z = 360 Mean Central Star mass 0.68 M • Pointsymmetric z = 800 Mean Central Star mass 0.59 M • Shaw,R.A, Stanghellini,L.,Mutchler,M.,Balick,B.,Blades,J.C. 2000, ApJ, 548, 727 (29 PNe) • Elliptical 17 % • Round 29 % • Bipolar 51 % • Pointsymmetric 3 %

  11. Stanghellini, Manchado, Villaver, Guerrero 2002, AJ 576, 285 Different mass ranges for Round, Elliptical and Bipolar PNs • Soker 2002, A&A 386, 885 Spherical PN low metalicity 70% are further away from the galactic center than the sun is from the galactic center.

  12. Górny, S.K., Stasinska, G., & Tylenda, R. 1997, A&A 318, 256

  13. On the statistics • Sample selection • Complete sample (255 PNe) • All PNe larger than 4 arcseconds in Acker´s catalog (1992). • All northern PNe (d > -11) • Ha , [N II], [O III] images • 213 PNe from: • Manchado, A., Guerrero, M.A., Stanghellini, L., & Serra-Ricart, M.1996, The IAC Morphological Catalog of Northern Galactic PN ed. IAC • 20PNe from Balick , B.1987, AJ 94, 671 • 22PNe from Schwarz, H. E., Corradi, R. L. M., & Melnik J.1992, A&AS 96, 23

  14. Database • Statistical distances: • Cahn, J.H., Kaler, J.B., Stanghellini, L. 1992, A&AS 94, 399 • NASA Astrophysics Data System • http://adsabs.harvard.edu/

  15. Chemical abundances • Emission lines: • Kaler, J.B., Shaw, R.A., Browning, L. 1997, PASP 109, 289 • Guerrero, M.A. 1995, PhD Thesis • Plasma diagnostic + ionic chemical abundances • nebular analysis package in IRAF/STSDAS (Shaw et al.1998) • Helium abundances • collisional effects Clegg (1987)

  16. Abell 39

  17. Abell 50

  18. NGC 2438

  19. Abell 72

  20. NGC 1501

  21. IC 1295

  22. NGC 6853

  23. He 2-429

  24. NGC 650

  25. K 4-55

  26. He 2-437

  27. M 3-28

  28. On the projection effects Round classification <D>= 10 and 27.5 arcsec a/b < 1 +0.06 Projected ellipsoid (c:1:1) Observed ellipse x= (c2(sin(i)2)+(cos(i))2) x a/b i inclination angle

  29. On the projection effects

  30. On the projection effects 1.2< c <1.5 P  7.3 % N(elliptical)=149 11 elliptical seen as round N(round)=63 17 % of round could be elliptical 40 % of MSPN are asymmetrical

  31. d < 6.5 Kpc

  32. Morphological classes whole sample E=58 %,R=25 %, B=17 % Taking into account projection effect E=63 %, R=20 %, B=17 % d < 6.5 Kpc E=62 %, R=26 %, B=12 % Taking into account projection effect E=66 %, R=22 %, B=12 %

  33. d < 6 Kpc

  34. Round, Bipolar, Elliptical

  35. <R>=638 <E>=276 <E+P>=259 <B>=56 <B+P>=135

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