Long-term chromospheric activity of non-eclipsing RS CVn-type stars

Context. The IUE database provides several UV high and low-resolution spectra of RS CVn-type stars from 1978 to 1996. In particular, many of these stars were monitored continuously during several seasons by IUE. Aims. Our main purpose is to study the short and long-term chromospheric activity of the...

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Autores principales:	Buccino, A.P., Mauas, P.J.D.
Formato:	JOUR
Materias:	Stars binaries: spectroscopic Stars: activity Ultraviolet: stars Chromophores Flip flop circuits Polyethylene glycols Rapid solidification Chromospheric activities HR 1099 Lomb-scargle periodogram Resolution spectrum Rotational modulations V711 taus Stars
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_00046361_v495_n1_p287_Buccino
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_00046361_v495_n1_p287_Buccino
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spelling	todo:paper_00046361_v495_n1_p287_Buccino2023-10-03T14:00:25Z Long-term chromospheric activity of non-eclipsing RS CVn-type stars Buccino, A.P. Mauas, P.J.D. Stars binaries: spectroscopic Stars: activity Ultraviolet: stars Chromophores Flip flop circuits Polyethylene glycols Rapid solidification Chromospheric activities HR 1099 Lomb-scargle periodogram Resolution spectrum Rotational modulations Stars: activity Ultraviolet: stars V711 taus Stars Context. The IUE database provides several UV high and low-resolution spectra of RS CVn-type stars from 1978 to 1996. In particular, many of these stars were monitored continuously during several seasons by IUE. Aims. Our main purpose is to study the short and long-term chromospheric activity of the RS CVn systems most observed by IUE: HD 22 468 (V711 Tau, HR 1099, K1IV+G5V), HD 21 242 (UX Ari, K0IV+G5V), and HD 224 085 (II Peg, K2IV).Methods. We first obtained the Mount Wilson index from the IUE high and low-resolution spectra. Secondly, we used the Lomb-Scargle periodogram to analyse the mean annual index and the amplitude of the rotational modulation of the index. Results. For HD 22 468 (V711 Tau, HR 1099), we find a possible chromospheric cycle with a period of ~18 years and a shorter cycle with a period of ~3 years, which could be associated to a chromospheric "flip-flop" cycle. The data of HD 224 085 (II Peg) also suggest a chromospheric cycle of ~21 years and a flip-flop cycle of ~9 years. Finally, we obtained a possible chromospheric cycle of ~7 years for HD 21 242 (UX Ari).. © 2009 ESO. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v495_n1_p287_Buccino
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Stars binaries: spectroscopic Stars: activity Ultraviolet: stars Chromophores Flip flop circuits Polyethylene glycols Rapid solidification Chromospheric activities HR 1099 Lomb-scargle periodogram Resolution spectrum Rotational modulations Stars: activity Ultraviolet: stars V711 taus Stars
spellingShingle	Stars binaries: spectroscopic Stars: activity Ultraviolet: stars Chromophores Flip flop circuits Polyethylene glycols Rapid solidification Chromospheric activities HR 1099 Lomb-scargle periodogram Resolution spectrum Rotational modulations Stars: activity Ultraviolet: stars V711 taus Stars Buccino, A.P. Mauas, P.J.D. Long-term chromospheric activity of non-eclipsing RS CVn-type stars
topic_facet	Stars binaries: spectroscopic Stars: activity Ultraviolet: stars Chromophores Flip flop circuits Polyethylene glycols Rapid solidification Chromospheric activities HR 1099 Lomb-scargle periodogram Resolution spectrum Rotational modulations Stars: activity Ultraviolet: stars V711 taus Stars
description	Context. The IUE database provides several UV high and low-resolution spectra of RS CVn-type stars from 1978 to 1996. In particular, many of these stars were monitored continuously during several seasons by IUE. Aims. Our main purpose is to study the short and long-term chromospheric activity of the RS CVn systems most observed by IUE: HD 22 468 (V711 Tau, HR 1099, K1IV+G5V), HD 21 242 (UX Ari, K0IV+G5V), and HD 224 085 (II Peg, K2IV).Methods. We first obtained the Mount Wilson index from the IUE high and low-resolution spectra. Secondly, we used the Lomb-Scargle periodogram to analyse the mean annual index and the amplitude of the rotational modulation of the index. Results. For HD 22 468 (V711 Tau, HR 1099), we find a possible chromospheric cycle with a period of ~18 years and a shorter cycle with a period of ~3 years, which could be associated to a chromospheric "flip-flop" cycle. The data of HD 224 085 (II Peg) also suggest a chromospheric cycle of ~21 years and a flip-flop cycle of ~9 years. Finally, we obtained a possible chromospheric cycle of ~7 years for HD 21 242 (UX Ari).. © 2009 ESO.
format	JOUR
author	Buccino, A.P. Mauas, P.J.D.
author_facet	Buccino, A.P. Mauas, P.J.D.
author_sort	Buccino, A.P.
title	Long-term chromospheric activity of non-eclipsing RS CVn-type stars
title_short	Long-term chromospheric activity of non-eclipsing RS CVn-type stars
title_full	Long-term chromospheric activity of non-eclipsing RS CVn-type stars
title_fullStr	Long-term chromospheric activity of non-eclipsing RS CVn-type stars
title_full_unstemmed	Long-term chromospheric activity of non-eclipsing RS CVn-type stars
title_sort	long-term chromospheric activity of non-eclipsing rs cvn-type stars
url	http://hdl.handle.net/20.500.12110/paper_00046361_v495_n1_p287_Buccino
work_keys_str_mv	AT buccinoap longtermchromosphericactivityofnoneclipsingrscvntypestars AT mauaspjd longtermchromosphericactivityofnoneclipsingrscvntypestars
_version_	1782026486274850816

Long-term chromospheric activity of non-eclipsing RS CVn-type stars

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