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We report new mid-eclipse times of the short-period sdB/dM binary HW Vir,which differ substantially from the times predicted by a previous model. Theproposed orbits of the two planets in that model are found to be unstable. Wepresent a new secularly stable solution, which involves two companions orbitingHW VIr with periods of 12.7 yr and 55 +/-15 yr. For orbits coplanar with thebinary, the inner companion is a giant planet with mass M_3 sin i_3 = 14 M_Jupand the outer one a brown dwarf or low-mass star with a mass of M_4 sin i_4 =30-120 M_Jup. Using the mercury6 code, we find that such a system would bestable over more than 10^7 yr, in spite of the sizeable interaction. Our modelfits the observed eclipse-time variations by the light-travel time effectalone, without invoking any additional process, thereby providing support forthe planetary hypothesis of the eclipse-time variations in close binaries. Thesignature of non-Keplerian orbits may be visible in the data.

The quest for companions to post-common envelope binaries: III. A reexamination of HW Virginis