Quantifying stellar parameters and magnetic activity for cool stars in double-lined spectroscopic binaries (SB2) is not straightforward, as both stars contribute to the observed composite spectra and are likely variable. Disentangled component spectra allow a detailed analysis of a component’s magnetic activity. We aim at separating the spectra of the two stellar components of the HR7275 SB2 system. Our further aim is a more accurate orbital solution by cleaning the observed radial velocities (RV) from activity perturbations of the spotted primary (“RV jitter”) and obtain a surface image of this component. We provide time-series high- and ultra-high resolution optical spectra and apply two different disentangling methods. RV residuals are modeled with three-sine function fits. The primary’s spectral-line profiles are modeled with the Doppler imaging code iMAP. Magnetic fields are measured for the primary based on least-square deconvolved Stokes-V line profiles. Chromospheric emission is determined from the line-cores of Ca II H&K, Ca II IRT 8542 Å, and Balmer Hα. Before applying those analyses, we provide a disentangling technique to determine the system properties more accurately. The Doppler image of the primary shows two large cool spots of size ≈20% of the visible hemisphere plus three smaller spots, each still ≈13% in size. In total, HR7275a exhibited an impressive spottedness of ≈40% of its entire surface in May-June 2022. The RV is modulated by the rotation of the primary with maximum amplitudes of 320 ms−1 and 650 ms−1 for two different modulation behaviors during the 250 d of our observations. This jitter is primarily caused by the varying asymmetries of the apparent disk brightness due to the cool spots. Its removal resulted in roughly ten times higher precision of the orbital elements. Our snapshot magnetic-field measurements reveal phase dependent (large-scale) surface fields between +0.6±2.0G at phase 0.1 and −15.2±2.7G at phase 0.6, indicating a complex magnetic morphology related to the location of the photospheric spots. We also obtain a logarithmic lithium abundance of 0.58±0.1 for HR7275a, indicating considerable mixing, and 0.16 for HR7275b, which is an extremely low value.
Read more: Adebali, Weber, Strassmeier, et al. 2026, A&A, in press. arXiv:2512.09521