Cool Stars 14 - Submitted Abstract # 70 This version created on 05 October 2006 Emission Line from Exotorus Tsubasa Fukue, Kyoto University Emission line profiles from an optically thin emitting torus in an extrasolar system are investigated with model calculation under various conditions. The torus is assumed to be optically thin, rigidly rotating. When the rotational velocity of the torus is larger than the thermal motion and the inclination angle is high, emission lines have double peaks. When the inclination angle is low, on the other hand, emission lines do not have double peaks, but the intensity is larger than that of near edge-on. The companion can be detected via the shadow within emission lines of the torus. The dip owing to the shadow can be periodically shifted as the companion orbits. In addition, the effect by the shadow of the companion resembles to the Rossiter--McLaughlin effect. When the density has non-axisymmetric distribution and the line emitter is concentrated around the companion, the emission line is periodically Doppler shifted as the orbital phase of the companion. Moreover, on additional dimming of a line during transit, the transit time of the torus is longer than that of the central object of the torus, and the peak of the transit effect is different from that of the central object, because of the shape of the torus. The detection of a line which can not be interpreted as comes from the central object or the companion may lead to the detection of the exotorus. ----------------------------------