1 / 15

The morphology and kinematics of planetary nebulae: a tribute to Hugo Schwarz

The morphology and kinematics of planetary nebulae: a tribute to Hugo Schwarz. Romano L.M. Corradi Isaac Newton Group of Telescopes. My story with Hugo, and our story with PNe, started on 1991 at ESO Chile…. Catalogue of CCD narrowband images of PNe and morphological classification

ollie
Download Presentation

The morphology and kinematics of planetary nebulae: a tribute to Hugo Schwarz

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The morphology and kinematics of planetary nebulae: a tribute to Hugo Schwarz Romano L.M. Corradi Isaac Newton Group of Telescopes

  2. My story with Hugo, and our story with PNe, started on 1991 at ESO Chile… • Catalogue of CCD narrowband images of PNe and morphological classification • Studies of the kinematic properties of bipolar PNe • Search and study of nebulae around symbiotic stars

  3. 1) Catalogue of CCD images of PNe… The first extensive CCD surveys had appeared: Jewitt et al 1986 ApJ 302, 727 44 PNe (“haloes”) Chu et al. 1987 ApJS 64, 529 ~100 PNe (multiple-shells) Balick 1987 AJ 94, 671 51 PNe and a morphological sequence (round elliptical  butterfly ) linked with the Generalised Interacting Stellar Winds theory Schwarz, Corradi & Melnick 1992 A&AS 96, 23 255 PNe

  4. 1) Catalogue of CCD images of PNe… The first extensive CCD morphological studies had appeared: Jewitt et al 1986 ApJ 302, 727 44 PNe (haloes) Chu et al. 1987 ApJS 64, 529 ~100 PNe (multiple-shells) Balick 1987 AJ 94, 671 51 PNe and a morphological sequence (round elliptical  butterfly ) linked with the Generalised Interacting Stellar Winds theory Schwarz, Corradi & Melnick 1992 A&AS 96, 23 255 PNe

  5. 1) … its morphological classification… Schwarz, Corradi & Stanghellini 1992 IAU Symp. 155, p. 214

  6. 1) .. and the study of the statistical properties of the morphological classes of PNe Stanghellini, Corradi & Schwarz 1993 A&A 276, 463 Schwarz & Corradi 1995 APN1 Corradi & Schwarz 1995 A&A 293, 871 • Bipolar PNe belong to a younger Galactic stellar population than elliptical and round PNe, i.e. have more massive progenitors: • smaller scale height on the Galactic plane; • more ordered Galactic kinematics; • hotter central stars; • He and N overabundances; • … Corradi APN2 discusses why the characteristic above is not necessarily a decisive constraint for the physical mechanisms shaping collimated PNe

  7. NGC 6537 2) Studies of the kinematics of bipolar PNe Schwarz & Corradi 1992 A&A 265, L37 Corradi & Schwarz 1993 A&A 268, 714; … 269, 462; … 273, 247; …278, 247 Aspin et al. 1993 A&A 278, 255 Schwarz et al. 1997 A&A 319, 267 Schwarz & Corradi 1992 A&A 265, L37 Corradi & Schwarz 1993 A&A 268, 714; … 269, 462; … 273, 247; …278, 247 Aspin et al. 1993 A&A 278, 255 Schwarz et al. 1997 A&A 319, 267 Streamlines are radial and gas is expanding in a ballistic way: self-similar expansion in a Hubble-like flow (V ∝ r). Shaping occurs in the early evolution, and an asymptotic shape (self-similar regime) is quickly reachedCorradi APN3

  8. 2) Point-symmetry  Precession? Schwarz 1993, in 2nd ESO/CTIO Workshop on “Mass loss on the AGB and beyond”, La Serena, Chile, 21-24 Jan 1992. Edited by H.E. Schwarz, ESO 1993

  9. 2) A special case and a beauty: M 2-9 Today’s Astronomy Picture of the Day!

  10. 2) … the dusty dentist’s mirrors of M 2-9… Schwarz et al. 1997 A&A 319, 267 Nature and expansion parallax of its dusty outermost knots VN = Vexp+ Vexpsin i VS = Vexp- Vexpsin i

  11. 2) … and its “light house” Monitoring since the end of the 80’s, mainly at ESO first and then at the Nordic Optical Telescope when Hugo moved to La Palma on 1995

  12. For the same longitude, the “illuminating” beam excites N2 and S2 about 2 yr later than N1 and S1, which corresponds to a travelling speed of ~5000 km/s  particle beam=jet? Doyle et al. 2000 AJ 119, 339 Corradi et al. in preparation Prot=90-130 yr 2) … and its “light house” N2 N1 S1 S2

  13. 3) Symbiotic stars can do it R Aqr nebula known since 1921 (Lampland 1923 PAAS 4, 319), but the concept that a large fraction of symbiotic Miras have (collimated) nebulae very similar to PNe, which illustrate the potential importance of binary interactions for the shaping of PNe, started growing from the moment that Hugo discovered the Southern Crab and other symbiotic nebulae. Schwarz Aspin & Lutz 1989 ApJ 344 L29 Corradi et al. 2001 ApJ 553 221

  14. V417 Cen BI Cru AS 201 V1016 Cyg CH Cyg HM Sge Schwarz 1991 A&A 243, 469 van Winckel et al. 1994 A&A 285, 241 Schwarz & Corradi 1992 A&A 265, L37 Corradi & Schwarz 1993 A&A 715, 725 Corradi et al. 1999 A&A 348, 978

More Related