We present the physical properties of V404 Lyr exhibiting eclipse timing variations and multiperiodic pulsations from all historical data including the { \it Kepler } and SuperWASP observations .
Detailed analyses of 2,922 minimum epochs showed that the orbital period has varied through a combination with an upward-opening parabola and two sinusoidal variations , with periods of P _ { 3 } =649 d and P _ { 4 } =2,154 d and semi-amplitudes of K _ { 3 } =193 s and K _ { 4 } =49 s , respectively .
The secular period increase with a rate of + 1.41 \times 10 ^ { -7 } d yr ^ { -1 } could be interpreted as a combination of the secondary to primary mass transfer and angular momentum loss .
The most reasonable explanation for both sinusoids is a pair of light-travel-time effects due to two circumbinary objects with projected masses of M _ { 3 } =0.47 M _ { \odot } and M _ { 4 } =0.047 M _ { \odot } .
The third-body parameters are consistent with those calculated using the Wilson-Devinney binary code .
For the orbital inclinations i _ { 4 } \gtrsim 43 ^ { \circ } , the fourth component has a mass within the hydrogen-burning limit of \sim 0.07 M _ { \odot } , which implies that it is a brown dwarf .
A satisfactory model for the Kepler light curves was obtained through applying a cool spot to the secondary component .
The results demonstrate that the close eclipsing pair is in a semi-detached , but near-contact , configuration ; the primary fills approximately 93 % of its limiting lobe and is larger than the lobe-filling secondary .
Multiple frequency analyses were applied to the light residuals after subtracting the synthetic eclipsing curve from the Kepler data .
This revealed that the primary component of V404 Lyr is a \gamma Dor type pulsating star , exhibiting seven pulsation frequencies in the range of 1.85 - 2.11 d ^ { -1 } with amplitudes of 1.38 - 5.72 mmag and pulsation constants of 0.24 - 0.27 d. The seven frequencies were clearly identified as high-order low-degree gravity-mode oscillations which might be excited through tidal interaction .
Only eight eclipsing binaries have been known to contain \gamma Dor pulsating components and , therefore , V404 Lyr will be an important test-bed for investigating these rare and interesting objects .