Zobrazeno 1 - 4
of 4
pro vyhledávání: '"Ehsan Paki"'
Autor:
Atila Poro, Ehsan Paki, Mark G. Blackford, Fatemeh Davoudi, Yasemin Aladag, Shiva Zamanpour, Soroush Sarabi, Afshin Halavati, Nazim Aksaker, Halil Bagis, Jabar Rahimi, Hamidreza Guilani, Aysun Akyuz, Faezeh Jahediparizi, Ozge Doner, Zohreh Ashrafzadeh
We present the photometric analysis of six short-period systems (EI Oct, V336 TrA, NX Boo, V356 Boo, PS Boo, and V2282 Cyg). This is the first photometric analysis of these systems except for V336 TrA. Observations were conducted for 27 nights at thr
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::e8e1f6bfa9d985ba4c712b2115a00106
Autor:
Ehsan PAKI
Publikováno v:
Recent Advances in Science and Engineering.
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::185e0cedba1afc7eb6d10816f66debad
https://doi.org/10.14744/rase.2022.0007
https://doi.org/10.14744/rase.2022.0007
Autor:
R. Foroughi, Amir Ghalee, T. Farjadnia, Ehsan Paki, A. Mazidabadi~Farahani, Atila Poro, F. Hasheminasab, S. M. Mousavi, M. Roshana, P. Mirshafie~Khozani, Fatemeh Davoudi, F. Ahangarani~Farahani, F. Nasrollahzadeh, S. Rezvanpanah
WASP-12 b, WASP-33 b, WASP-36 b, and WASP-46 b are four transiting planetary systems which we have studied. These systems' light curves were derived from observations made by the Transiting Light Exoplanet Survey Satellite (TESS) and some ground-base
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::8d06f0c47fd44da1164d18f1c6411ad7
http://arxiv.org/abs/2012.01486
http://arxiv.org/abs/2012.01486
Autor:
A. M. Zubareva, Ehsan Paki, Amir Ghalee, Filiz Kahraman Alicavus, Atila Poro, Mahshid Nourmohammad, Fatemeh Davoudi, A. A. Popov, Zahra Sabaghpour Arani, Golnaz Mazhari, Soroush Sarabi, Behjat Zarei Jalalabadi, Farzaneh Ahangarani Farahani, Hamidreza Guilani
Publikováno v:
Publications of the Astronomical Society of the Pacific. 133:084201
The multi-color CCD photometric study of 27 Delta Scuti stars is presented. By using approximately three years of photometric observations, we obtained the times of maxima and magnitude changes during the observation time interval for each star. The
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::254467c072a263e66c500b850a763d23
https://doi.org/10.1088/1538-3873/ac12dc
https://doi.org/10.1088/1538-3873/ac12dc