Context.The main chromospheric activity indicator is the S index, which is the ratio of the flux in the core of the Ca II H and K lines to the continuum nearby, and is well studied for stars from F to K. Another chromospheric proxy is the Hα line, which is believed to be tightly correlated with the Ca II index. Aims.In this work we characterize both chromospheric activity indicators, the one associated with the H and K Ca II lines and the other with Hα, for the whole range of late type stars, from F to M. Methods.We present periodic medium-resolution echelle observations covering the complete visual range, taken at the CASLEO Argentinean Observatory over 7 years. We use a total of 917 flux-calibrated spectra for 109 stars that range from F6...
Context. Strong spectral lines are useful indicators of stellar chromospheric activity. They are phy...
In this work we present spectroscopic observations centered in the spectral lines most widely used a...
We present Echelle spectra of 91 late-type dwarfs, of spectral types from F to M and of different le...
Context.The main chromospheric activity indicator is the S index, which is the ratio of the flux in ...
Context.The main chromospheric activity indicator is the S index, which is the ratio of the flux in ...
The main chromospheric activity indicator is the S index, which is esentially the ratio of the flux ...
In this work we analyze the behaviour of the excess Ca II H and K and H_ ε emissions in a sample of ...
We study the sodium D lines (D1: 5895.92Å D2: 5889.95Å) in late-type dwarf stars. The stars have sp...
In this work we analyze the behaviour of the excess Ca II H & K and H emissions in a sample of 73 c...
Context. Understanding stellar activity in M dwarfs is fundamental to improving our knowledge of the...
We present a homogeneous study of chromospheric and coronal flux–flux relationships using a sample o...
The main purpose of this study is to use the IUE spectra in the analysis of magnetic activity of ma...
The magnetic phenomena on the solar surface have been the subject of several investigations over the...
© 1995 EDP Sciences. This work has been supported by the Universidad Complutense de Madrid and the S...
Context. The largest dataset of stellar activity measurements available at present is the one obtai...
Context. Strong spectral lines are useful indicators of stellar chromospheric activity. They are phy...
In this work we present spectroscopic observations centered in the spectral lines most widely used a...
We present Echelle spectra of 91 late-type dwarfs, of spectral types from F to M and of different le...
Context.The main chromospheric activity indicator is the S index, which is the ratio of the flux in ...
Context.The main chromospheric activity indicator is the S index, which is the ratio of the flux in ...
The main chromospheric activity indicator is the S index, which is esentially the ratio of the flux ...
In this work we analyze the behaviour of the excess Ca II H and K and H_ ε emissions in a sample of ...
We study the sodium D lines (D1: 5895.92Å D2: 5889.95Å) in late-type dwarf stars. The stars have sp...
In this work we analyze the behaviour of the excess Ca II H & K and H emissions in a sample of 73 c...
Context. Understanding stellar activity in M dwarfs is fundamental to improving our knowledge of the...
We present a homogeneous study of chromospheric and coronal flux–flux relationships using a sample o...
The main purpose of this study is to use the IUE spectra in the analysis of magnetic activity of ma...
The magnetic phenomena on the solar surface have been the subject of several investigations over the...
© 1995 EDP Sciences. This work has been supported by the Universidad Complutense de Madrid and the S...
Context. The largest dataset of stellar activity measurements available at present is the one obtai...
Context. Strong spectral lines are useful indicators of stellar chromospheric activity. They are phy...
In this work we present spectroscopic observations centered in the spectral lines most widely used a...
We present Echelle spectra of 91 late-type dwarfs, of spectral types from F to M and of different le...