Query : 2008A&A...488..619V

2008A&A...488..619V - Astronomy and Astrophysics, volume 488, 619-622 (2008/9-3)

The magnetic field of the proto-planetary nebula candidate IRAS 19296+2227.


Abstract (from CDS):

Magnetic fields are thought to be one of the possible mechanisms responsible for shaping the generally spherical outflow of evolved stars into often aspherical planetary nebulae. However, direct measurements of magnetic fields during the transition to the planetary nebula phase are rare. The aim of this project is to expand the number of magnetic field measurements of stars in the (proto-)planetary nebula phase and find if the magnetic field strength is sufficient to affect the stellar outflow.We used Very Long Baseline Array observations to measure the circular polarization due to the Zeeman splitting of 22GHz H2O masers in the envelope of the proto-planetary nebula candidate star IRAS 19296+2227 and the planetary nebula K3-35.A strong magnetic field of B||=-135±28 is detected in the H2O maser region of the proto-planetary nebula candidate IRAS 19296+2227. The H2O masers of K3-35 are too weak to detect circular polarization although we do present the measurements of weak linear polarization in those masers.The field measured in the masers of IRAS 19296+2227 is dynamically important and, if it is representative of the large scale field, is an important factor in driving the stellar mass loss and shaping the stellar outflow.

Abstract Copyright:

Journal keyword(s): masers - stars: magnetic fields - polarization - stars: circumstellar matter - stars: late-type

Simbad objects: 5

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Number of rows : 5
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
1 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 4003 3
2 OH 031.0+00.0 OH* 18 47 41.13768 -01 45 11.4048           O-rich 143 1
3 QSO B1848+283 QSO 18 50 27.5898721080 +28 25 13.155071160   17.1 17 17.16   ~ 82 1
4 PN K 3-35 PN 19 27 43.9749997920 +21 30 02.907990216           O-rich 148 0
5 OH 057.5+01.8B C* 19 31 45.5807303448 +22 33 42.841426356           C 25 0

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