Paper

International observational campaign of the 2014 eclipse of EE Cep

Smela, T, Boyd, D, McDonald, P, Pieńkowski, D, Gazeas, K, Kundera, T, Ogłoza, W, Semkov, E, Apostolovska, G, Menke, J, Dróżdż, M, Heras, T A, Pigulski, A, Pakońska, P, Hambálek, L, A Capetillo Blanco, Dean, S, Martignoni, M, Dimitrov, D, Wiersema, K, Świerczyński, E, Biskupski, M, Kamiński, T, Plauchu-Frayn, I, Zoła, S, Kjurkchieva, D, Marchev, D, Nedoroščik, J, Tomov, T, Kubicki, D, Winiarski, M, Baran, A, Sanchez, A, Garai, Z, Kołaczkowski, Z, J -L Gonzalez Carballo, Siwak, M, Zahajkiewicz, E, Rodriguez, D, Dubois, F, Gałan, C, Ribeiro, J, Sergey, I, Moździerski, D, Conidis, G J, Bruś, P, Richardson, N, Staels, B, Rodriguez, M, Peneva, S, Mikołajewski, M, Ibryamov, S, Armiński, A, Kankiewicz, P, Corp, L, Miller, I, Pribulla, T, Kneip, R, Dȩbski, B, Kardasis, E, Donchev, Z, Kundra, E, Wychudzki, P, Logie, L, Conseil, E, Lopatovský, J, J Kare Trandem Qvam

2020

Overview

Context. EE Cep is one of few eclipsing binary systems with a dark, dusty disk around an invisible object similar to {\\epsilon} Aur. The system is characterized by grey and asymmetric eclipses every 5.6 yr, with a significant variation in their photometric depth, ranging from ~ 0 m .5 to ~ 2 m .0. Aims. The main aim of the observational campaign of the EE Cep eclipse in 2014 was to test the model of disk precession (Galan et al. 2012). We expected that this eclipse would be one of the deepest with a depth of ~ 2 m .0. Methods. We collected multicolor observations from almost 30 instruments located in Europe and North America. This photometric data covers 243 nights during and around the eclipse. We also analyse the low- and high-resolution spectra from several instruments. Results. The eclipse was shallow with a depth of 0 m .71 in V-band. The multicolor photometry illustrates small color changes during the eclipse with a total amplitude of order ~ +0 m . 15 in B-I color index. The linear ephemeris for this system is updated by including new times of minima, measured from the three most recent eclipses at epochs E = 9, 10 and 11. New spectroscopic observations were acquired, covering orbital phases around the eclipse, which were not observed in the past and increased the data sample, filling some gaps and giving a better insight into the evolution of the H {\\alpha} and NaI spectral line profiles during the primary eclipse. Conclusions. The eclipse of EE Cep in 2014 was shallower than expected 0 m .71 instead of ~ 2 m . 0. This means that our model of disk precession needs revision.

• Publisher: Cornell University Library, arXiv.org
• Subject: Binary systems / Color / Eclipses / Line spectra / Model testing / Photometry / Precession / Upgrading