LU Vel (GJ 375): A M3.5Ve Flare and Double-Lined Spectroscopic Binary

Erratum: Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue. II. Two spotted M<1 Mo systems at different evolutionary stages (not published, article has been modified directly without Erratum)

“…The eclipsing pair itself was previously identified by the Hipparcos satellite (HIP 41322, NLTT 1915, PPM 715320) to be a part of the visual double system CCDM 08259-1623. The brightness ratio from the Montes et al (2007) data is consistent with the magnitude difference of 2.37 mag reported in the Hipparcos catalogue. Note also that the new reduction of Hipparcos data (van Leeuwen 2007) gives the parallax of 21.83 ± 2.25 mas or the distance of 45.8 ± 4.7 pc.…”

“…ASAS-08 was reported as a double-lined spectroscopic binary (SB2) by Christian & Mathioudakis (2002), who also provided the equivalent widths of the H α and H β lines separately for every component. The first spectroscopic orbital solution was recently derived by Montes et al (2007). They obtained five highresolution echelle spectra, two of which were at the orbital phase φ = 0.…”

“…Values of the period and zero-phase as well as e and ω for ASAS-08 are from the combined RV + LC analysis. We did not include the data of Montes et al (2007) for ASAS-08. Still, our solution is quite consistent with theirs.…”

“…We aimed to keep the flux ratio in V unchanged at the level given by the Hipparcos photometry and Montes et al (2007) data (see Sect. 2.2), but we had no constrains for the I band.…”

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

“…When the third I flux level was too low, we ended up with a situation where the third component is hotter (smaller V − I) than the binary components. If that is the case, and if it is gravitationally bound to ASAS-08, as suggested by Montes et al (2007), one should expect it to be brighter in V than the binary. We could also reject some solutions by inspections of model light curves, which for example did not reproduce the depth of one of the minima.…”