Magnetic fields in Planetary and Proto Planetary. Nebulae. Laurence Sabin (IAC ,SPAIN / Manchester,UK) . A.A. Zijlstra (Manchester,UK) and J.S. Greaves (St Andrews,UK) . 3 Shaping Models. ✸ Wind-Wind interaction . BUT need of initial axisymmetrical structure.
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Laurence Sabin(IAC ,SPAIN / Manchester,UK)
A.A. Zijlstra (Manchester,UK) and J.S. Greaves (St Andrews,UK)
I) Detection of global magnetic fields.
II) Characteristics of the field in 4 bipolar objects
III) Relation with the physical properties of the targets.
IV) What is the role of B in the shaping of Post-AGBs and PNe?
Small : 4 objects
Unique : NO other known data
“Death” of SCUBA
Hot central star (1.5-2.5 x 10^ 5 K)
Magnetic Field distribution:
- Does not cover all the nebula
- Organized (1 main direction)
- Consistent (small variation of polarization degree & no change in geometry)
Bfield in the SE-NW direction = equatorial plane
Well defined toroidal magnetic field.
mp:(11.2 ± 2.2) %, ma: (26.5 ± 5.7) °
Credit: W. B. Latter et al., HST, NICMOS
Submm size: ~ 40 x 36 arcsec²
B distribution :
Toroidal magnetic field.
NE: mp=8.9±0.9 % SW: mp=7.6±1.3 %
2,2m ESO.Courtesy: R. Corradi & A. Zijlstra
~ 1.7 x 1 arcmin²
mp: (11.4 ±1.6) % ma: (32.7± 4.6)°
B localized and aligned at the radio core position : Not Toroidal
HST data. Credit: R. Sahai, J. Trauger
Submm size: ~ 60 x 45 arcsec²
Composite: Visible+ IR
HST data. Credit: R. Sahai, J. Trauger, R. Thompson
POLOIDAL & TOROIDAL magnetic fields
mp: 1.4% - 3.2 % - 8.8%
**** Re-seeding process (J. Nordhaus, APN4)
Sabin L. , Zijlstra A.A, and Greaves J.S, 2007, MNRAS, Vol 376-378
Greaves J.S., 2002 , A&A, Vol 392, p L1-L4