| Title: |
Extensive study of HD 25558, a long-period double-lined binary with two SPB components |
| Authors: |
Sodor, A.; De Cat, P.; Wright, D.J.; Neiner, C.; Briquet, M.; Lampens, P.; Dukes, R.J.; Henry, G.W.; Williamson, M.H.; Brunsden, E.; Pollard, K.R.; Cottrell, P.L.; Maisonneuve, F.; Kilmartin, P.M.; Matthews, J.; Kallinger, T.; Beck, P.G.; Kambe, E.; Engelbrecht, C.A.; Czanik, R.J.; Yang, S.; Hashimoto, O.; Honda, S.; Fu, J.N.; Castanheira, B.; Lehmann, H.; Bognar, Zs; Behara, N.; S. Scaringi, Simone; Van Winckel, Hans; Menu, Jonathan; Lobel, A.; Mathias, P.; Saesen, S.; Vuckovic, M. |
| Source: |
ISSN:0035-8711 ; ISSN:1365-2966 ; Monthly Notices of the Royal Astronomical Society, vol. 438 (4), (3535-3556. |
| Publisher Information: |
Oxford University Press (OUP) |
| Publication Year: |
2014 |
| Subject Terms: |
asteroseismology; binaries: spectroscopic; stars: individual: HD 25558; stars: magnetic field; stars: oscillations; stars: rotation; Science & Technology; Physical Sciences; Astronomy & Astrophysics; PULSATING B-STARS; NONRADIAL ADIABATIC PULSATIONS; MAGNETIC-FIELD MEASUREMENTS; PROFILE VARIATIONS; ROTATING STARS; MODE-IDENTIFICATION; MERCATOR TELESCOPE; ACTIVE STARS; DATA-BASE; PHOTOMETRY; astro-ph.SR; 0201 Astronomical and Space Sciences; 5101 Astronomical sciences; 5107 Particle and high energy physics; 5109 Space sciences |
| Description: |
We carried out an extensive observational study of the Slowly Pulsating B (SPB) star, HD 25558. The ≈2000 spectra obtained at different observatories, the ground-based and MOST satellite light curves revealed that this object is a double-lined spectroscopic binary with an orbital period of about nine years. The observations do not allow the inference of an orbital solution. We determined the physical parameters of the components, and found that both lie within the SPB instability strip. Accordingly, both show line-profile variations due to stellar pulsations. 11 independent frequencies were identified in the data. All the frequencies were attributed to one of the two components based on pixel-by-pixel variability analysis of the line profiles. Spectroscopic and photometric mode identification was also performed for the frequencies of both stars. These results suggest that the inclination and rotation of the two components are rather different. The primary is a slow rotator with ≈6 d period, seen at ≈60° inclination, while the secondary rotates fast with ≈1.2 d period, and is seen at ≈20° inclination. Spectropolarimetric measurements revealed that the secondary component has a magnetic field with at least a few hundred Gauss strength, while no magnetic field can be detected in the primary. ; sponsorship: AS acknowledges support of the Belgian Federal Science Policy (project M0/33/029, PI: P.D.C.). AS and ZsB acknowledges support of the Eotvos Scholarship from the Hungarian Scholarship Board Office. MB is F.R.S.-FNRS Postdoctoral Researcher, Belgium. GWH and MHW acknowledge support from NASA, NSF, Tennessee State University and the State of Tennessee through its Centers of Excellence programme. TK acknowledges financial support from the Austrian Science Fund (FWF P23608). PGB was supported through the European Research Council under the European Community's Seventh Framework Programme (FP7/20072013)/ERC grant agreement no. 227224 (PROSPERITY). CAE and RJC acknowledge financial support from NRF and University of ... |
| Document Type: |
article in journal/newspaper |
| File Description: |
application/pdf |
| Language: |
English |
| Relation: |
https://lirias.kuleuven.be/handle/123456789/469663; https://doi.org/10.1093/mnras/stt2466 |
| DOI: |
10.1093/mnras/stt2466 |
| Availability: |
https://lirias.kuleuven.be/handle/123456789/469663; https://lirias.kuleuven.be/retrieve/633d7b48-2324-451c-a46e-117af9286520; https://doi.org/10.1093/mnras/stt2466 |
| Rights: |
info:eu-repo/semantics/openAccess ; public |
| Accession Number: |
edsbas.11B535C3 |
| Database: |
BASE |