| Issue |
A&A
Volume 411, Number 3, December I 2003
|
|
|---|---|---|
| Page(s) | 489 - 502 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20031377 | |
| Published online | 17 November 2003 | |
Rotational modulation of the photospheric and chromospheric activity in the young, single K2-dwarf PW And *,**
1
Departamento de Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain
2
The Pennsylvania State University, Department of Astronomy and Astrophysics, 525 Davey Laboratory, University Park, PA 16802, USA
Corresponding author: J. López-Santiago, jls@astrax.fis.ucm.es
Received:
20
February
2003
Accepted:
11
August
2003
High resolution echelle spectra of PW And (HD 1405) have been
taken during eight observing runs from 1999 to 2002.
The detailed analysis of the spectra allow us to determine its
spectral type (K2V),
mean heliocentric radial velocity (
km s
)
rotational velocity (
km s),
and equivalent width of the lithium
line 
(EW(Li i) = 273 mÅ).
The kinematic (Galactic Velocity (U,V,W))
confirms its membership in the Local Association moving group,
in agreement with the age (30 to 80 Myrs) inferred from the
color magnitude diagram and the lithium equivalent width.
Photospheric activity (presence of cool spots that disturb the profiles
of the photospheric lines) has been
detected as changes in the bisectors of the
cross correlation function (CCF) resulting of
cross-correlate the spectra of PW And with the spectrum of
a non-active star of similar spectral type.
These variations of the CCF bisectors are related to the
variations in the measured radial velocities and are modulated
with a period similar to the photometric period of the star.
At the same time, chromospheric activity has been analyzed,
using the spectral subtraction technique and simultaneous spectroscopic
observations of the Hα, Hβ, Na i D1
and D2, He i D3,
Mg i b triplet, Ca ii H&K, and Ca ii infrared triplet lines.
A flare was observed during the last observing run of 2001,
showing an enhancement in the observed chromospheric lines.
A less powerful flare was observed on 2002 August 23.
The variations of the chromospheric activity indicators seem to be related
to the photospheric activity.
A correlation between radial velocity, changes in the CCF bisectors
and equivalent width of different chromospheric lines is observed
with a different behaviour between epochs 1999, 2001 and 2002.
Key words: stars: activity / stars: chromospheres / stars: starspots / stars: late-type / stars: flare / stars: rotation
Based on observations made with the 2.2 m telescope of the German-Spanish Astronomical Centre, Calar Alto (Almería, Spain), operated by the Max-Planck-Institute for Astronomy, Heidelberg, jointly with the Spanish National Commission for Astronomy, with the Nordic Optical Telescope (NOT), operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway and Sweden, in the Spanish Observatorio del Roque de Los Muchachos of the Instituto de Astrofísica de Canarias, with the Isaac Newton Telescope (INT) operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de Los Muchachos of the Instituto de Astrofísica de Canarias, with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Centro Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de Los Muchachos of the Instituto de Astrofisica de Canarias and with the Hobby-Eberly Telescope (HET) operated by McDonald Observatory on behalf of The University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen.
© ESO, 2003
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