Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-28T01:48:34.581Z Has data issue: false hasContentIssue false
  • English
  • Français

Contribution of small telescopes at the Oukaïmden observatory in Morocco to study atmospheric dynamics and shocks waves in variables stars RR Lyr and R Scuti

Published online by Cambridge University Press:  19 March 2024

A. Benhida Open the ORCID record for A. Benhida [Opens in a new window] ,
F. L. Sefyani ,
K. Chafouai ,
Y. El Jariri ,
J. Chouqar ,
Z. Benkhaldoun Open the ORCID record for Z. Benkhaldoun [Opens in a new window] ,
K. Kolenberg  and
S. Sylla
A. Benhida*
Affiliation:
Oukameden Observatory, LPHEA FSSM and FSTG Cadi Ayyad University, BP 618 Marrakech, Morocco
F. L. Sefyani
Affiliation:
Oukameden Observatory, LPHEA FSSM and FSTG Cadi Ayyad University, BP 618 Marrakech, Morocco
K. Chafouai
Affiliation:
Oukameden Observatory, LPHEA FSSM and FSTG Cadi Ayyad University, BP 618 Marrakech, Morocco
Y. El Jariri
Affiliation:
Oukameden Observatory, LPHEA FSSM and FSTG Cadi Ayyad University, BP 618 Marrakech, Morocco
J. Chouqar
Affiliation:
Oukameden Observatory, LPHEA FSSM and FSTG Cadi Ayyad University, BP 618 Marrakech, Morocco
Z. Benkhaldoun
Affiliation:
Oukameden Observatory, LPHEA FSSM and FSTG Cadi Ayyad University, BP 618 Marrakech, Morocco
K. Kolenberg
Affiliation:
Department of Physics, University of Antwerp, Groenenborgerlaan 171, 2020 Antwerpen email: [email protected]
S. Sylla
Affiliation:
University Cheikh Anta Diop, Senegal email: [email protected]
*
email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Through Spectroscopy, we aim to develop the field of pulsating stars, especially the atmospheric dynamics of high amplitude pulsators such as RR Lyr and R Scuti, in order to establish new models of the mechanical and thermal behavior of their atmospheres (shock waves, relaxation time, energy loss…). We used high-resolution spectra over a total of 81 nights from made with the spectrograph Eshell during years 2013 and 2015 runs from Oukaïmeden observatory in the High Atlas mountains (Morocco) completed with made with the spectrograph ELODIE (Haute Provence observatory, France) during years 1994–1997. A detailed analysis of line profile variations over the whole pulsation cycle is performed. Shock wave velocity and lines intensity were used as indicators of atmospheric dynamics activities. We have obtained and compared our results with those obtained by the large telescopes, we have obtained thanks to our site very satisfactory results, Indeed : For RR lyr: For the first time the second apparition of Helium (D3) was detected using our Telescope (0.35m) at Oukaïmeden Observatory.

For the first time, during the phase of expansion of the star, the emission of the line D3 is visible on various phases Blazhko, including during the minimum of the cycle Blazhko.

Also, we presented the results of a long- term, high-resolution spectroscopic study of the variable star R Sct. We analyzed the features of the optical spectra of this object and found RSct shows irregular behavior in its slight variations for much of the time that it was observed. Its average period is close to 142 d, but some- times the irregularities are so strong that it is not possible to define a periodic variation.

Keywords

variable stars: RR LyrR Scutiatmospheric dynamicsSmall TelescopsSpectrophotometry
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S371: Honoring Charlotte Moore Sitterly: Astronomical Spectroscopy in the 21st Century , August 2022 , pp. 92 - 97
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Benhida et al. 2018, in: The RR Lyrae 2017 Conference, Vol. 6, 279–281 Google Scholar
Benhida et al. 2020, Astronomical Society of the Pacific Conference Series., Volume 529, pgs. 11–16.Google Scholar
Benkhaldoun, Z. 2018, Nature Astron., 2, 352 CrossRefGoogle Scholar
Chafouai, K., Benhida, A., Sefyani, F., et al. 2019, IAU Symposium, 343, 368 CrossRefGoogle Scholar
Gillet, D., et al. 2016, Astron. Astrophysics, 587, A134 CrossRefGoogle Scholar
Gillet, D., Fabas, N., Lebre, A. 2013, Astron. Astrophysics, 553, A59 CrossRefGoogle Scholar
Preston, G., W. 2009, Astron. Astrophysics, 507, 1621 CrossRefGoogle Scholar
Thizy, O., & Cochard, F. 2010, Proc. IAU Symp., 272, 282 CrossRefGoogle Scholar
Wallerstein, G. & Cox, A. N. 1984, PASP, 96, 677 CrossRefGoogle Scholar