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   61231
   With the ASCA PV phase, we detected Class I sources deeply embedded in
   the Rho-Oph dark cloud. One of the hard X-ray sources (EL29) shows a
   flare associated with a heat-up and cooling, while another (WL6)
   exhibits sinusoidal variation with no large spectral change. The later
   would be due to the spin rotation of the protostar. The period of the
   sinusoidal variation is about 1 day, which is shorter than the
   rotational period of T Tauri stars, or more evolved star than
   protostars, of $\\sim$3--7 day. The goal of this survey project is TO
   DETECT THE SPIN PERIOD OF PROTOSTARS. Protostar itself cannot be
   detected in any other wave lengths because of the high absorption
   (Av$>$100mag), then the spin of the star can be detected only in the
   hard X-ray of ASCA.
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