The Na i D resonance lines in main-sequence late-type stars

We study the sodium D lines (D1: 5895.92 Å; D2: 5889.95 Å) in late-type dwarf stars. The stars have spectral types between F6 and M5.5 (B - V between 0.457 and 1.807) and metallicity between and 0.6. We obtained medium-resolution echelle spectra using the 2.15-m telescope at the Argentinian observat...

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Autores principales:	Díaz, R.F., Cincunegui, C., Mauas, P.J.D.
Formato:	JOUR
Materias:	Stars: activity Stars: chromospheres Stars: late-type
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_00358711_v378_n3_p1007_Diaz
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_00358711_v378_n3_p1007_Diaz
record_format	dspace
spelling	todo:paper_00358711_v378_n3_p1007_Diaz2023-10-03T14:46:49Z The Na i D resonance lines in main-sequence late-type stars Díaz, R.F. Cincunegui, C. Mauas, P.J.D. Stars: activity Stars: chromospheres Stars: late-type We study the sodium D lines (D1: 5895.92 Å; D2: 5889.95 Å) in late-type dwarf stars. The stars have spectral types between F6 and M5.5 (B - V between 0.457 and 1.807) and metallicity between and 0.6. We obtained medium-resolution echelle spectra using the 2.15-m telescope at the Argentinian observatory Complejo Astronómico El Leoncito (CASLEO). The observations have been performed periodically since 1999. The spectra were calibrated in wavelength and in flux. A definition of the pseudo-continuum level is found for all our observations. We also define a continuum level for calibration purposes. The equivalent width of the D lines is computed in detail for all our spectra and related to the colour index (B - V) of the stars. When possible, we perform a careful comparison with previous studies. Finally, we construct a spectral index as the ratio between the flux in the D lines and the bolometric flux. We find that, once corrected for the photospheric contribution, this index can be used as a chromospheric activity indicator in stars with a high level of activity. Additionally, we find that combining some of our results, we obtain a method to calibrate in flux stars of unknown colour. © 2007 The Authors. Journal compilation © 2007 RAS. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00358711_v378_n3_p1007_Diaz
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: activity Stars: chromospheres Stars: late-type
spellingShingle	Stars: activity Stars: chromospheres Stars: late-type Díaz, R.F. Cincunegui, C. Mauas, P.J.D. The Na i D resonance lines in main-sequence late-type stars
topic_facet	Stars: activity Stars: chromospheres Stars: late-type
description	We study the sodium D lines (D1: 5895.92 Å; D2: 5889.95 Å) in late-type dwarf stars. The stars have spectral types between F6 and M5.5 (B - V between 0.457 and 1.807) and metallicity between and 0.6. We obtained medium-resolution echelle spectra using the 2.15-m telescope at the Argentinian observatory Complejo Astronómico El Leoncito (CASLEO). The observations have been performed periodically since 1999. The spectra were calibrated in wavelength and in flux. A definition of the pseudo-continuum level is found for all our observations. We also define a continuum level for calibration purposes. The equivalent width of the D lines is computed in detail for all our spectra and related to the colour index (B - V) of the stars. When possible, we perform a careful comparison with previous studies. Finally, we construct a spectral index as the ratio between the flux in the D lines and the bolometric flux. We find that, once corrected for the photospheric contribution, this index can be used as a chromospheric activity indicator in stars with a high level of activity. Additionally, we find that combining some of our results, we obtain a method to calibrate in flux stars of unknown colour. © 2007 The Authors. Journal compilation © 2007 RAS.
format	JOUR
author	Díaz, R.F. Cincunegui, C. Mauas, P.J.D.
author_facet	Díaz, R.F. Cincunegui, C. Mauas, P.J.D.
author_sort	Díaz, R.F.
title	The Na i D resonance lines in main-sequence late-type stars
title_short	The Na i D resonance lines in main-sequence late-type stars
title_full	The Na i D resonance lines in main-sequence late-type stars
title_fullStr	The Na i D resonance lines in main-sequence late-type stars
title_full_unstemmed	The Na i D resonance lines in main-sequence late-type stars
title_sort	na i d resonance lines in main-sequence late-type stars
url	http://hdl.handle.net/20.500.12110/paper_00358711_v378_n3_p1007_Diaz
work_keys_str_mv	AT diazrf thenaidresonancelinesinmainsequencelatetypestars AT cincuneguic thenaidresonancelinesinmainsequencelatetypestars AT mauaspjd thenaidresonancelinesinmainsequencelatetypestars AT diazrf naidresonancelinesinmainsequencelatetypestars AT cincuneguic naidresonancelinesinmainsequencelatetypestars AT mauaspjd naidresonancelinesinmainsequencelatetypestars
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The Na i D resonance lines in main-sequence late-type stars

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