Publication: Rotational modulation of the photospheric and chromospheric activity in the young, single K2-dwarf PW and [asterisks referring to footnotes]
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2003-12
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Abstract
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 (V_hel = - 11.15 km s^-1) rotational velocity (ν sin i = 22.6 km s^-1), and equivalent width of the lithium line λ6707.8 Å (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 D_1 and D_2, He I D_3, 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.
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© ESO 2003.
Asterisk 1 in title refers to footnote:
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 Astrofísica 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.
We would like to thank M. Cruz Gálvez for help in the reduction of the observations, Dr. B. H. Foing for allowing us to use the ESA-MUSICOS spectrograph at Isaac Newton Telescope, and Dr. I. Ilyn for help with SOFIN spectrograph during the observations at the Nordic Optical Telescope (NOT). This work was supported by the Universidad Complutense de Madrid and the Spanish Ministerio de Ciencia y Tecnología (MCYT), Programa Nacional de Astronomía y Astrofísica under grant AYA2001-1448.
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