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We present results of our study of the close pre-main sequence spectroscopicbinary CVSO 104 in Ori OB1, based on data obtained within the PENELLOPE legacyprogram. We derive, for the first time, the orbital elements of the system andthe stellar parameters of the two components. The system is composed of twoearly M-type stars and has an orbital period of about 5 days and a mass ratioof 0.92, but contrarily to expectations does not appear to have a tertiarycompanion. Both components have been (quasi-)synchronized, but the orbit isstill very eccentric. The spectral energy distribution clearly displays asignificant infrared excess compatible with a circumbinary disk. The analysisof HeI and Balmer line profiles, after the removal of the compositephotospheric spectrum, reveals that both components are accreting at a similarlevel. We also observe excess emission in H$\alpha$ and H$\beta$, which appearsredshifted or blueshifted by more than 100 km/s with respect to the mass centerof the system depending on the orbital phase. This additional emission could beconnected with accretion structures, such as funnels of matter from thecircumbinary disk. We also analyze the optical companion located at about 2".4from the spectroscopic binary. This companion, that we named CVSO 104B, turnsout to be a background Sun-like star not physically associated with the PMSsystem and not belonging to Ori OB1.

PENELLOPE II. CVSO 104: a pre-main sequence close binary with an optical companion in Ori OB1