Over a large part of its spectrum, from the UV to the mid-IR, the emitted flux from a planet originates in the incident flux scattered by major atmospheric constituents and haze particles, or reflected on the surface, with a certain albedo coefficient. Therefore a strong correlation does exist between the planetary spectrum and the spectrum of the central star, with a wavelength shift which depends on the orbital velocity projection on the line of sight. Although absorption features from atmospheric constituents affect the planetary spectrum, they significantly decrease the correlation effect only when similar in narrowness to the stellar spectrum structures. Taking advantage of a wide spectral range, high resolution spectroscopy, high coronographic efficiency and long integration time, it is proposed to look for maxima in the cross-correlation functions between the spectra of selected nearby stars and their close surrounding space. Refering to the star spectrum auto-correlation function indicates the confidence level of possible detections. As compared to others, such an approach might extend the search to Earth-like planets. Algorithms are then presented and the potential performances are discussed and illustrated by using the solar spectrum as an exemple.