Volume 629, September 2019
|Number of page(s)||7|
|Section||Stellar structure and evolution|
|Published online||02 September 2019|
HD 965: An extremely peculiar A star with an extremely long rotation period⋆
European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
2 Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz 369167, Russia
3 Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya St, 119017 Moscow, Russia
4 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
5 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei Mŭnchen, Germany
6 National Astronomical Research Institute of Thailand, Chiangmai 50180, Thailand
Accepted: 23 July 2019
Context. One of the keys to understanding the origin of Ap stars and their significance in the general context of stellar astrophysics is by considering the most extreme properties displayed by some of them. For this reason, HD 965 is particularly interesting as it combines some of the most pronounced chemical peculiarities with one of the longest rotation periods known.
Aims. We characterise the variations of the magnetic field of the Ap star HD 965 and derive constraints about its structure.
Methods. We combined published measurements of the mean longitudinal field ⟨Bz⟩ of HD 965 with new determinations of this field moment from circular spectropolarimetry obtained at the 6-m telescope BTA of the Special Astrophysical Observatory of the Russian Academy of Sciences. For the mean magnetic field modulus ⟨B⟩, literature data were complemented by the analysis of ESO archive spectra.
Results. We present the first determination of the rotation period of HD 965, Prot = (16.5 ± 0.5) yr. The star HD 965 is only the third Ap star with a period longer than ten years for which magnetic field measurements have been obtained over more than a full cycle. The variation curve of ⟨Bz⟩ is well approximated by a cosine wave. Furthermore, ⟨B⟩ does not show any significant variation. The observed behaviour of these field moments is well represented by a simple model consisting of the superposition of collinear dipole, quadrupole, and octupole. The distribution of neodymium over the surface of HD 965 is highly non-uniform. The element appears concentrated around the magnetic poles, especially the negative one.
Conclusions. The shape of the longitudinal magnetic variation curve of HD 965 indicates that its magnetic field is essentially symmetric about an axis passing through the centre of the star. Overall, HD 965 appears similar to the bulk of the long-period Ap stars, as far as its magnetic field is concerned.
Key words: stars: individual: HD 965 / stars: chemically peculiar / stars: rotation / stars: magnetic field
Based on observations collected at the European Southern Observatory under ESO Programmes 52.7-063, 53.7-028, 55.E-0751, 57.E-0637, 61.E-0711, and 72.D-0138; at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii; and at the 6-m telescope BTA of the Special Astrophysical Observatory of the Russian Academy of Sciences. Also based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes 68.D-0254, 70.D-0470, 74.C-0102, 75.C-0234, 76.C-0073, 76.D-0169, 79.C-0170, 279.D-5059, and 80.C-0032.
© ESO 2019
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