Volume 639, July 2020
|Number of page(s)||9|
|Section||Catalogs and data|
|Published online||02 July 2020|
International observational campaign of the 2014 eclipse of EE Cephei⋆
Nicolaus Copernicus Astronomical Centre PAS, Warsaw, Poland
e-mail: firstname.lastname@example.org, email@example.com
2 Nicolaus Copernicus University, Toruń, Poland
3 Section of Astrophysics, Astronomy and Mechanics, Department of Physics, National and Kapodistrian University of Athens, 15784 Zografos, Athens, Greece
4 Sonoita Research Observatory/AAVSO, USA
5 Astronomical Observatory, Jagiellonian University, Cracow, Poland
6 Mount Suhora Astronomical Observatory, Cracov Pedagogical University, ul. Podchorazych 2, 30-084 Cracow, Poland
7 Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria
8 Department of Physics, Shumen University, Shumen, Bulgaria
9 PTMA, Szczecin, Poland
10 Furzehill House, Ilston, Swansea SA2 7LE, UK
11 Instytut Astronomiczny, Uniwersytet Wrocławski, Poland
12 Club d’astronomie de Mont-Bernenchon, France
13 BAA Variable Star Section, West Challow Observatory, Oxfordshire, UK
14 Department of Physics and Astronomy, York University, Toronto, Ontario, Canada
15 Instituto de Astronomía, Universidad Nacional Autonoma de Mexico, Ensenada, BC, Mexico
16 Observatorio Las Pegueras, NAVAS DE ORO (Segovia), Spain
17 Hellenic Amateur Astronomy Association, Athens, Greece
18 Astronomical Institute, Slovak Academy of Sciences, Tatranská Lomnica, Slovak Republic
19 ELTE Eötvös Loránd University, Gothard Astrophysical Observatory, 9700 Szombathely, Hungary
20 MTA-ELTE Exoplanet Research Group, Szent Imre h. u. 112, 9700 Szombathely, Hungary
21 Guadarrama Observatory MPC458, Madrid, Spain
22 Center for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA, USA
23 Astrolab Iris, Zillebeke Belgium, Belgium
24 Institute of Physics, Astrophysics Division, Jan Kochanowski University, Kielce, Poland
25 Stazione Astronomica Betelgeuse, Magnago, Milano, Italy
26 Private Observatory, Maladziechna, Belarus
27 The Faculty of Mathematics and Natural Sciences, Department of Physics, University of Oslo, Oslo, Norway
28 Cerro del Viento Observatory (MPC I84), Badajoz, Spain
29 Observatorio do Instituto Geografico do Exercito – Lisboa, Lisboa, Portugal
30 AstroCamp Observatory (MPC I89), Nerpio, Spain
31 Institute of Physics, Faculty of Science, Ss. Cyril and Methodius University, Skopje, FYR of Macedonia
32 AAVSO, Cambridge, MA 02138, USA
33 Groupe Européen d’Observations Stellaires (GEOS), Bailleau l’Evêque, France
34 Private Observatory Madrid-Ventilla MPC J30, Spain
35 Gualba Observatory, Spain
36 Department of Physics and Astronomy, University of Leicester, Leicester, UK
37 Menke Scientific, Barnesville, MD 20838, USA
38 Amateur society “Astroblocknote”, Minsk, Belarus
39 Mont Mégantic Observator, University of Montreal, Montreal, Canada
Accepted: 17 January 2020
Context. EE Cep is one of few eclipsing binary systems with a dark, dusty disc around an invisible object similar to ε Aur. The system is characterised by grey and asymmetric eclipses every 5.6 yr that have significant variations in their photometric depth, ranging from ∼0.m5 to ∼2.m0.
Aims. The main aim of the observational campaign of the EE Cep eclipse in 2014 was to test the model of disc precession. We expected that this eclipse would be one of the deepest with a depth of ∼2.m0.
Methods. We collected multicoloured observations from almost 30 instruments located in Europe and North America. These photometric data cover 243 nights during and around the eclipse. We also analyzed low- and high-resolution spectra from several instruments.
Results. The eclipse was shallow with a depth of 0.m71 in the V band. The multicoloured photometry illustrates small colour changes during the eclipse with a total amplitude of order ∼+0.m15 in the B − I colour index. We updated the linear ephemeris for this system by including new times of minima, measured from the three most recent eclipses at epochs E = 9, 10, and 11. We acquired new spectroscopic observations, covering orbital phases around the eclipse, which were not observed in the past and increased the data sample, filling some gaps and giving better insight into the evolution of the Hα and Na I spectral line profiles during the primary eclipse.
Conclusions. The eclipse of EE Cep in 2014 was shallower than expected, measuring 0.m71 instead of ∼2.m0. This means that our model of disc precession needs revision.
Key words: binaries: eclipsing / circumstellar matter / stars: emission-line / Be
Tables A1−A29 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/639/A23
© ESO 2020
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