The Sun is a cornerstone of stellar astrophysics, offering a uniquely detailed benchmark due to its proximity. However, our ability to observe it spans only a brief window of its 4.5-billion-year evolution, raising the question: how typical is the Sun among solar-type stars? This has led to the identification of solar twins—stars nearly identical to the Sun in parameters such as effective temperature, gravity, metallicity, age, luminosity, and magnetic activity—and solar analogues, which broadly resemble the Sun but allow for greater variation. Recent advances in asteroseismology have transformed stellar characterisation by detecting solar-like oscillations in hundreds of main-sequence stars. These oscillations allow precise measurements of stellar masses, radii, and ages. When combined with high-resolution spectroscopy, they yield the most accurate fundamental parameters to date and have led to the identification of seismic solar analogues: stars that resemble the Sun in both atmospheric properties and internal structure. This work presents a combined seismic and spectroscopic analysis of six solar analogues observed by Kepler/K2, HERMES, and Gaia. By integrating individual oscillation frequencies, high-resolution spectroscopic abundances, and precise astrometric data, we derive detailed stellar structure and evolution models. This approach enables unprecedented insight into the internal properties of these stars and helps place the Sun within a broader evolutionary framework.