FLORES TRIVIGNO Matias Gaston
Discovery of an activity cycle in the solar analog HD45184. Exploring Balmer and metallic lines as activity proxy candidates
MATÍAS FLORES; FEDERICO GONZÁLEZ; MARCELO JAQUE ARANCIBIA; ANDREA BUCCINO; CARLOS SAFFE
ASTRONOMY AND ASTROPHYSICS
EDP SCIENCES S A
Lugar: Paris; Año: 2016 vol. 589 p. 1 - 6
Context. Most stellar activity cycles similar to that found in the Sun have been detected by using the chromospheric Ca II H&K linesas stellar activity proxies. However, it is unclear whether such activity cycles can be identified using other optical lines.Aims. We aim to detect activity cycles in solar-analog stars and determine whether they can be identified through other optical lines,such as Fe II and Balmer lines. We study the solar-analog star HD45184 using HARPS spectra. The temporal coverage and high quality of the spectra allow us to detect both long- and short-term activity variations.Methods. We analysed the activity signatures of HD 45184 by using 291 HARPS spectra obtained between 2003 and 2014. To search for line-core flux variations, we focused on Ca II H&K and Balmer H and H lines, which are typically used as optical chromospheric activity indicators. We calculated the HARPS-S index from Ca II H&K lines and converted it into the Mount Wilson scale. In addition, we also considered the equivalent widths of Balmer lines as activity indicators. Moreover, we analysed the possible variability of Fe II and other metallic lines in the optical spectra. The spectral variations were analysed for periodicity using the Lomb-Scargle periodogram.Results. We report for the first time a long-term 5.14-yr activity cycle in the solar-analog star HD 45184 derived from Mount WilsonS index. This makes HD45184 one of most similar stars to the Sun with a known activity cycle. The variation is also evident in thefirst lines of the Balmer series, which do not always show a correlation with activity in solar-type stars. Notably, unlike the solar case,we also found that the equivalent widths of the high photospheric Fe ii lines (4924 Å, 5018 Å and 5169 Å) are modulated (2 mÅ)by the chromospheric cycle of the star. These metallic lines show variations above 4 sigma in the rms spectrum, while some Ba II andTi II lines present variations at 3 sigma level, which could be considered as marginal variations. From short-term modulation of the S indexwe calculate a rotational period of 19.98 days, which agrees with its mean chromospheric activity level. We also clearly show that theactivity cycles of HD45184 can be detected in both Fe II and Balmer lines.