Chromospheric activity in proxima centauri

In this work we present Echelle spectra of the dM5.5e flare star Proxima Centauri, obtained in the CASLEO observatory. We have 44 observations from 1999 to date, taken in 11 different observing runs, which were flux calibrated. The index mostly used to measure stellar activity is the one combining C...

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Detalles Bibliográficos
Publicado: 2005
Materias:
Stars: Activity
Stars: Flare stars
Stars: Individual (Proxima Centauri)
Activation analysis
Atmospherics
Correlation methods
Fluxes
Signal to noise ratio
Spectrum analysis
Proxima centauri
Stars: activity
Stars: flare stars
Stars: individual (Proxima Centauri)
Astronomy
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03796566_v_n560I_p479_Cincunegui
http://hdl.handle.net/20.500.12110/paper_03796566_v_n560I_p479_Cincunegui
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_03796566_v_n560I_p479_Cincunegui
record_format dspace
spelling paper:paper_03796566_v_n560I_p479_Cincunegui2023-06-08T15:40:42Z Chromospheric activity in proxima centauri Stars: Activity Stars: Flare stars Stars: Individual (Proxima Centauri) Activation analysis Atmospherics Correlation methods Fluxes Signal to noise ratio Spectrum analysis Proxima centauri Stars: activity Stars: flare stars Stars: individual (Proxima Centauri) Astronomy In this work we present Echelle spectra of the dM5.5e flare star Proxima Centauri, obtained in the CASLEO observatory. We have 44 observations from 1999 to date, taken in 11 different observing runs, which were flux calibrated. The index mostly used to measure stellar activity is the one combining Ca II H&K line fluxes. These lines, which are formed in the stellar chromosphere, are not particularly adequate to study cool stars, which are intrinsically faint and red. We construct an index from Hα, which shows a good correlation with the Ca II lines and is more suitable for this cool star, due to its longer wavelength. We found that the He I D3 line can be a useful proxy to discriminate the average chromospheric activity from the frequent flaring activity. We could separate this transient activity using this index, and we found that the remaining variability is compatible with the existence of an activity cycle of around 1300 days as suggested in previous works. 2005 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03796566_v_n560I_p479_Cincunegui http://hdl.handle.net/20.500.12110/paper_03796566_v_n560I_p479_Cincunegui
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: Flare stars
Stars: Individual (Proxima Centauri)
Activation analysis
Atmospherics
Correlation methods
Fluxes
Signal to noise ratio
Spectrum analysis
Proxima centauri
Stars: activity
Stars: flare stars
Stars: individual (Proxima Centauri)
Astronomy
spellingShingle Stars: Activity
Stars: Flare stars
Stars: Individual (Proxima Centauri)
Activation analysis
Atmospherics
Correlation methods
Fluxes
Signal to noise ratio
Spectrum analysis
Proxima centauri
Stars: activity
Stars: flare stars
Stars: individual (Proxima Centauri)
Astronomy
Chromospheric activity in proxima centauri
topic_facet Stars: Activity
Stars: Flare stars
Stars: Individual (Proxima Centauri)
Activation analysis
Atmospherics
Correlation methods
Fluxes
Signal to noise ratio
Spectrum analysis
Proxima centauri
Stars: activity
Stars: flare stars
Stars: individual (Proxima Centauri)
Astronomy
description In this work we present Echelle spectra of the dM5.5e flare star Proxima Centauri, obtained in the CASLEO observatory. We have 44 observations from 1999 to date, taken in 11 different observing runs, which were flux calibrated. The index mostly used to measure stellar activity is the one combining Ca II H&K line fluxes. These lines, which are formed in the stellar chromosphere, are not particularly adequate to study cool stars, which are intrinsically faint and red. We construct an index from Hα, which shows a good correlation with the Ca II lines and is more suitable for this cool star, due to its longer wavelength. We found that the He I D3 line can be a useful proxy to discriminate the average chromospheric activity from the frequent flaring activity. We could separate this transient activity using this index, and we found that the remaining variability is compatible with the existence of an activity cycle of around 1300 days as suggested in previous works.
title Chromospheric activity in proxima centauri
title_short Chromospheric activity in proxima centauri
title_full Chromospheric activity in proxima centauri
title_fullStr Chromospheric activity in proxima centauri
title_full_unstemmed Chromospheric activity in proxima centauri
title_sort chromospheric activity in proxima centauri
publishDate 2005
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03796566_v_n560I_p479_Cincunegui
http://hdl.handle.net/20.500.12110/paper_03796566_v_n560I_p479_Cincunegui
_version_ 1768545286897008640

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