| Autor: |
Pieńkowski, D. Gałan, C. Tomov, T. Gazeas, K. Wychudzki, P. Mikołajewski, M. Kubicki, D. Staels, B. Zoła, S. Pakońska, P. Dèbski, B. Kundera, T. Ogłoza, W. Dróz, M. Baran, A. Winiarski, M. Siwak, M. DImitrov, D. Kjurkchieva, D. Marchev, D. Armiński, A. Miller, I. Kołaczkowski, Z. Mozdzierski, D. Zahajkiewicz, E. Bruś, P. Pigulski, A. Smela, T. Conseil, E. Boyd, D. Conidis, G.J. Plauchu-Frayn, I. Heras, T.A. Kardasis, E. Biskupski, M. Kneip, R. Hambálek, L. Pribulla, T. Kundra, E. Garai, Z. Rodriguez, D. Kamiński, T. Dubois, F. Logie, L. Capetillo Blanco, A. Kankiewicz, P. Swierczyński, E. Martignoni, M. Sergey, I. Kare Trandem Qvam, J. Semkov, E. Ibryamov, S. Peneva, S. Gonzalez Carballo, J.-L. Ribeiro, J. Dean, S. Apostolovska, G. Donchev, Z. Corp, L. McDonald, P. Rodriguez, M. Sanchez, A. Wiersema, K. Conseil, E. Menke, J. Sergey, I. Richardson, N. |
| Jazyk: |
angličtina |
| Rok vydání: |
2020 |
| Popis: |
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. © ESO 2020. |
| Databáze: |
OpenAIRE |
| Externí odkaz: |
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