摘要：We perform a new analysis of the M-dwarf–M-dwarf eclipsing binary system NSVS 07394765 in order to investigate the reported hyper-inflated radius of one of the component stars. Our analysis is based on archival photometry from the Wide Angle Search for Planets, new photometry from the 32 cm Command Module Observatory telescope in Arizona and the 70 cm telescope at Thacher Observatory in California, and new high-resolution infrared spectra obtained with the Immersion Grating Infrared Spectrograph on the Discovery Channel Telescope. The masses and radii we measure for each component star disagree with previously reported measurements. We show that both stars are early M-type main-sequence stars without evidence for youth or hyper-inflation ( ☉ = - + M M 0.661 1 0.036 0.008 , ☉ = - + M M 0.608 2 0.028 0.003 , ☉ = - + R R 0.599 1 0.019 0.032 , ☉ = - +R R 0.625 2 0.027 0.012 ), and we update the orbital period and eclipse ephemerides for the system. We suggest that the likely cause of the initial hyper-inflated result is the use of moderate-resolution spectroscopy for precise radial velocity measurements.
关键词：binaries: close;binaries: eclipsing;binaries: spectroscopic;stars: fundamental parameters;stars: individual (NSVS 07394765);stars: late-type
