1 / 9

Kinematics of Microstructures in Planetary Nebulae: Binary Star Influences and Maser Emissions

This study explores the intricate kinematics of microstructures within planetary nebulae, focusing on phenomena such as precessing outflows and collimated ejections from binary central stars. Detailed analyses were conducted on NGC 6884, highlighting characteristics like point-symmetric spiral structures, multiphased outflows, and the role of water maser emissions. Observations from HST reveal a link between binary systems and the dynamics of ejected materials, with implications for understanding the evolution of symbiotic stars and the relationship between stellar interactions and nebular kinematics.

thyra
Download Presentation

Kinematics of Microstructures in Planetary Nebulae: Binary Star Influences and Maser Emissions

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. INTERNAL KINEMATICS OF MICROSTRUCTURES AND IMPLICATIONS Luis F. Miranda IAA-CSIC G. Anglada, R. Cesaroni, I. de Gregorio, J.F. Gómez, Y. Gómez, M.A. Guerrero, J.M. Torrelles, R. Vázquez • Precessing outflows • Collimated ejections from binary central stars • Water maser emission in planetary nebulae

  2. NGC 6884 • Multi-component planetary nebula • Ellipsoidal shell • Point-symmetric spiral structures • Two bipolar knots The properties of the point-symmetric spirals agree that the spiral are precessing bipolar outflows Vexp ~ 55 kms-1 Precession period ~ 475 yr (D ~ 1.9 kpc, Palen et al. 2002) R=[NII] , G=H , B=[OIII] HST Miranda, Guerrero, Torrelles 1999

  3. Hu2-1 and IC4846 IC4846 HHST Hu2-1 [NII]HST Binary central stars N The systemic velocity of the bipolar ejections does not coincide with the systemic velocity of the nebula Difference ~ 8 - 10 kms-1 Interpretation in terms of a binary star The velocity difference is related to the orbital velocity E 2" N E Vsys(jets) -Vsys(shell) = Vorb cos i  cos  2" Orbital parameters Orbital separation < 30 AU Orbital period < 100 yr Related to symbiotic stars?

  4. Water maser emission from red giants to planetary nebulae Typical emission from the (spherical) envelope of red giants and AGB stars (e.g. Elitzur 1992; Habing 1996; Engels 2002)  W43A AGB star with a precessing bipolar jet (Imai et al. 2002)  Detected in proto-planetary nebulae • IRAS 19296+2227 (Marvel & Boboltz 1998,1999) • IRAS 16342-3814 (Likkel & Morris 1988, Morris et al. 2003) • More cases  Detected in extremely young planetary nebulae • K3-35 (Miranda et al. 2001) • IRAS 17347-3139 (de Gregorio et al. 2003)

  5. K3-35 Bipolar planetary nebula (optical size ~ 10") with an equatorial torus [OI] [NII] [OI] Strong [NII] and [OIII] emission lines HeII 4686  Teff > 60000 K [NII] [SIII] HeI H [SII] Miranda et al. 2003 H HeII [OIII]

  6. K3-35 • Water maser emission in a torus (r  85 AU [d = 5 kpc]) and at the tips of precessing collimated outflows ( 5000 AU from the center) • The jets are probably involved in the excitation of the distant water masers • The 1665 MHz line presents high levels of circular polarization (50%)  magnetized torus (Miranda et al. 2001)

  7. K3-35 New VLA observations reveal changes in the water maser spots  Changes in region C  No water maser at the tips of the jets (3 = 7 mJy) The time difference between the two epochs (2.5 yr) is too long to make a clear identification of the same water maser spots  Proper motions (?)  Destruction of the 1999 maser shell and creation of a new (2002) maser shell (?) + Miranda et al. 2001 ( September 1999)  de Gregorio et al. 2003 (May 2002) 1.3cm continuum emission peak (de Gregorio et al. 2003)

  8. IRAS 17347-3139 N • HST (K-band) (Bobrowsky et al. 1999) • Bipolar nebula 2" x 0.7" , PA -40º • Water maser emission detected with the Robledo 70 m antenna (Madrid) (de Gregorio et al. 2003, Survey for water maser emission in PNe) E 1" The radio continuun emission (1.3 cm-6 cm) indicates a partially optically thick ionized nebula (de Gregorio et al. 2003) Teff > 26000 °K ; Ne 106 cm-3 (D  0.8 kpc) Br and NeII nebular emission lines (Garcia-Lario, 2003, private communication)

  9. IRAS 17347-3139 VLA observations 2002 +0.6 +1.3 • 13 water maser spots tracing an ellipse  0.25"0.12" (PA  62°) • If circular ring  axis tilted  60° w.r.t. the observer • The kinematics suggests rotating and expanding motions in the ring • The 1.3cm continuum emission peak () does not coincide with the center of the ellipse • Inhomogenities in the (unresolved) ionized nebula + large beam? • Binary star? -0.7 0.0 +2 +2.6 -2.7 +3.3 +3.9 -3.3 -2.0 -1.3 -4.0 1" (De Gregorio et al. 2003)

More Related