Forward modeling solar spectra onto Doppler images of {\lambda} And

TL;DR

This study uses solar spectra and Doppler imaging of {\

Contribution

It introduces a toy model that links surface temperature maps to spectral behavior and activity modulation in {\

Findings

Spectral behavior of {\

Spectral behavior of {\

Spot contributions can largely explain the observed activity modulation.

Abstract

By using the Doppler images of {\lambda} And, we aim to investigate whether surface temperature information can be reversed to create its activity parameters, by feeding a toy model with solar spectra, based on the surface images. At the same time, we examine whether spot contributions alone are sufficient to explain the observed activity modulation of the RS CVn star {\lambda} And while quantifying the differences with the actual observations of this star that are obtained simultaneously with the Doppler images we use. Due to a lack of publicly available starspot models for its stellar type, we adopt observed solar spectra as the only available approximation of {\lambda} And's spots. These spectra are injected into sequence of full disk temperature map derived from Doppler imaging that represent a full stellar rotation. Using this approach, we show that even with simplified assumptions the spectral behavior of {\lambda} And can be qualitatively reproduced. Toy models such as the one presented in this work procure an additional dimension, providing a relation between the surface structures and chromospheric emissions. It also helps to develop a further understanding for the heating mechanisms of these active giants through comparative techniques, where in this case the spot activity seemingly modulates the chromospheric signal and can explain the bulk of its variations over a rotation.