2014A&A...570A..88S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST20:50:36

2014A&A...570A..88S - Astronomy and Astrophysics, volume 570A, 88-88 (2014/10-1)

Weak magnetic fields in central stars of planetary nebulae?

STEFFEN M., HUBRIG S., TODT H., SCHOELLER M., HAMANN W.-R., SANDIN C. and SCHOENBERNER D.

Abstract (from CDS):

It is not yet clear whether magnetic fields play an essential role in shaping planetary nebulae (PNe), or whether stellar rotation alone and/or a close binary companion, stellar or substellar, can account for the variety of the observed nebular morphologies. In a quest for empirical evidence verifying or disproving the role of magnetic fields in shaping planetary nebulae, we follow up on previous attempts to measure the magnetic field in a representative sample of PN central stars. We obtained low-resolution polarimetric spectra with FORS2 installed on the Antu telescope of the VLT for a sample of 12 bright central stars of PNe with different morphologies, including two round nebulae, seven elliptical nebulae, and three bipolar nebulae. Two targets are Wolf-Rayet type central stars. For the majority of the observed central stars, we do not find any significant evidence for the existence of surface magnetic fields. However, our measurements may indicate the presence of weak mean longitudinal magnetic fields of the order of 100Gauss in the central star of the young elliptical planetary nebula IC418 as well as in the Wolf-Rayet type central star of the bipolar nebula Hen2-113 and the weak emission line central star of the elliptical nebula Hen2-131. A clear detection of a 250G mean longitudinal field is achieved for the A-type companion of the central star of NGC1514. Some of the central stars show a moderate night-to-night spectrum variability, which may be the signature of a variable stellar wind and/or rotational modulation due to magnetic features. Since our analysis indicates only weak fields, if any, in a few targets of our sample, we conclude that strong magnetic fields of the order of kG are not widespread among PNe central stars. Nevertheless, simple estimates based on a theoretical model of magnetized wind bubbles suggest that even weak magnetic fields below the current detection limit of the order of 100G may well be sufficient to contribute to the shaping of the surrounding nebulae throughout their evolution. Our current sample is too small to draw conclusions about a correlation between nebular morphology and the presence of stellar magnetic fields.

Abstract Copyright:

Journal keyword(s): planetary nebulae: general - stars: magnetic field - stars: AGB and post-AGB - binaries: close - techniques: polarimetric

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 246 PN 00 47 03.3420803259 -11 52 18.975106178 10.15 11.52 11.76 12.18   PG1159 452 0
2 NGC 1360 PN 03 33 14.6471964691 -25 52 17.981057073   10.95 11.16     sdO 269 0
3 NGC 1514 PN 04 09 16.9857297577 +30 46 33.469936956   10.01 9.48     sdO+A0/3III 315 2
4 IC 418 PN 05 27 28.2060343141 -12 41 50.282659007   9.78 13.0     O7fp 1001 2
5 NGC 2346 PN 07 09 22.5216571385 -00 48 23.611157830   11.76 11.58     A5V 552 0
6 NGC 2392 PN 07 29 10.7669120392 +20 54 42.478515772     9.68     O6f 698 1
7 CD-56 2932 PN 09 43 25.61980 -57 16 55.6095   11.85 11.17 11.21   A2II 114 0
8 PN HbDs 1 PN 09 52 44.5227859639 -46 16 47.455337619 11.11 12.28 12.50 12.66   O(H)3Vz 73 0
9 NGC 3132 PN 10 07 01.7655812249 -40 26 11.138949314   10.14 10.01     A2V 371 1
10 CPD-51 6744 PN 14 18 08.8856504204 -52 10 39.518062758   12.39 11.98     [WC] 146 0
11 WRAY 15-1269 PN 14 59 53.4814028450 -54 18 07.524725528 12.12 12.17 11.64 11.63   [WC11] 228 0
12 HD 138403 PN 15 37 11.2073858949 -71 54 52.885863880   10.24 10.47 11.01   O8(f)ep 254 0
13 HD 148937 SB* 16 33 52.3867163783 -48 06 40.476619334 6.49 7.12 6.71 7.61   O6f?p 355 4

    Equat.    Gal    SGal    Ecl

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2020.07.11-20:50:37

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