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    PR # 31017                                                                   
     We propose an observation of the most luminous FU Orionis star, Z CMa       
     .  It is said that FU Orionis phenomena are episodic ones that young        
     stars experience through mass accretion phase. Though these are most        
     important objects stydying the process of the star formation , no X-r       
     ay observation is reported by far. With an observation of that star b       
     y ASCA, we will get new information about the property and mechanism        
     of mass outflow from the stellar system or its accretion disk, and ab       
     out the influence of heavy mass accretion upon the condition of the s       
     tellar surface. It has been shown that Z CMa is a system which consis       
     ts of a real FU Orionis star and an Ae/Be star heavily shrouded by du       
     st shell, so it might be possible to detect the activity caused by th       
    e interaction of two young sta                                               
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