2016A&A...586A..97B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST10:18:15

2016A&A...586A..97B - Astronomy and Astrophysics, volume 586A, 97-97 (2016/2-1)

Detection of ultra-weak magnetic fields in Am stars: β Ursae Majoris and θ Leonis.

BLAZERE A., PETIT P., LIGNIERES F., AURIERE M., BALLOT J., BOEHM T., FOLSOM C.P., GAURAT M., JOUVE L., LOPEZ ARISTE A., NEINER C. and WADE G.A.

Abstract (from CDS):

An extremely weak circularly polarized signature was recently discovered in spectral lines of the chemically peculiar Am star Sirius A. A weak surface magnetic field was proposed to account for the observed polarized signal, but the shape of the phase-averaged signature, dominated by a prominent positive lobe, is not expected in the standard theory of the Zeeman effect. We aim at verifying the presence of weak circularly polarized signatures in two other bright Am stars, β UMa and θ Leo, and investigating the physical origin of Sirius-like polarized signals further. We present here a set of deep spectropolarimetric observations of β UMa and θ Leo, observed with the NARVAL spectropolarimeter. We analyzed all spectra with the least squares deconvolution multiline procedure. To improve the signal-to-noise ratio and detect extremely weak signatures in Stokes V profiles, we co-added all available spectra of each star (around 150 observations each time). Finally, we ran several tests to evaluate whether the detected signatures are consistent with the behavior expected from the Zeeman effect. The line profiles of the two stars display circularly polarized signatures similar in shape and amplitude to the observations previously gathered for Sirius A. Our series of tests brings further evidence of a magnetic origin of the recorded signal. These new detections suggest that very weak magnetic fields may well be present in the photospheres of a significant fraction of intermediate-mass stars. The strongly asymmetric Zeeman signatures measured so far in Am stars (featuring a dominant single-sign lobe) are not expected in the standard theory of the Zeeman effect and may be linked to sharp vertical gradients in photospheric velocities and magnetic field strengths.

Abstract Copyright:

Journal keyword(s): stars: magnetic field - stars: chemically peculiar - stars: individual: β UMa - stars: individual: θ Leo

Simbad objects: 9

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Number of rows : 9

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 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A1V+DA 1395 0
2 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1046 1
3 * gam Leo ** 10 19 58.35056 +19 50 29.3468   3.79 2.37     K1-III+G7IIIb 69 0
4 * bet UMa PM* 11 01 50.4765370 +56 22 56.733912 2.35 2.35 2.37 2.31 2.35 A1IVps 406 1
5 * tet Leo PM* 11 14 14.4044630 +15 25 46.454086 3.40 3.33 3.35 3.32 3.34 A2IV 308 0
6 * 2 CVn * 12 16 07.5489242996 +40 39 36.645600522 9.17 7.21 5.66     M0.5III 70 0
7 * alf02 CVn a2* 12 56 01.6662171 +38 19 06.154110 2.44 2.76 2.88 2.98 3.05 A0VpSiEu 640 0
8 * iot Her bC* 17 39 27.8860861 +46 00 22.800110 2.940 3.630 3.800     B3IV 430 1
9 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2505 0

    Equat.    Gal    SGal    Ecl

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2020.07.11-10:18:15

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