# Spot evolution on LQ Hya during 2006--2017: temperature maps based on SOFIN and FIES data

## TL;DR

This study uses Doppler imaging to analyze the surface temperature maps of the young star LQ Hya from 2006 to 2017, revealing persistent high-latitude spots and chaotic phase behavior during its turbulent activity phase.

## Contribution

It provides new long-term temperature maps of LQ Hya during its chaotic activity phase, highlighting the persistence of high-latitude spots and their influence on photometric variability.

## Key findings

- High-latitude spot structures are persistent despite chaotic activity.
- Surface temperature shows a weak but systematic increase over time.
- Photometric minima phase jumps are linked to high-latitude spot changes.

## Abstract

Context. LQ Hya is one of the most frequently studied young solar analogue stars. Recently, it has been observed to show intriguing behaviour by analysing long-term photometry: during 2003--2009, a coherent spot structure migrating in the rotational frame has been reported by various authors, but since that time the star has entered a chaotic state where coherent structures seem to have disappeared and rapid phase jumps of the photometric minima occur irregularly over time. Aims. LQ Hya is one of the stars included in the SOFIN/FIES long-term monitoring campaign extending over 25 years. Here we publish new temperature maps for the star during 2006--2017, covering the chaotic state of the star. Methods. We use a Doppler imaging technique to derive surface temperature maps from high-resolution spectra. Results. From the mean temperatures of the Doppler maps we see a weak but systematic increase in the surface temperature of the star. This is consistent with the simultaneously increasing photometric magnitude. During nearly all observing seasons we see a high-latitude spot structure which is clearly nonaxisymmetric. The phase behaviour of this structure is very chaotic but agrees reasonably well with the photometry. Equatorial spots are also frequently seen, but many of them we interpret to be artefacts due to the poor to moderate phase coverage. Conclusions. Even during the chaotic phase of the star, the spot topology has remained very similar to the higher activity epochs with more coherent and long-lived spot structures: we see high-latitude and equatorial spot activity, the mid latitude range still being most often void of spots. We interpret the erratic jumps and drifts in phase of the photometric minima to be caused by changes in the high-latitude spot structure rather than the equatorial spots.