| We have collected a mass of stellar activity and rotation data of late-type stars. Combining with the results of Hipparcos satellite, we reserch the relation between stellar activity and rotation(include rotation period and Rossby number), and discuss the distribution of stellar rotation period and the evolution of angle momentum of late-type stars. Furthermore, we also reserch the influence of setllar age to stellar activity of late-type stars.The relation of stellar chromospheric activity and rotation of late-type main sequence stars depend on stellar spectral type. For A-early F type MS stars, stellar chromospheric activity decrease with stellar rotation period, but increase with Rossby number; For M type MS stars, stellar chromospheric activity increase with stellar rotation period and Rossby number, and stellar chromospheric activity reach saturation at large color index; For the MS stars between mid-F to M type, stellar chromospheric activity decrease with stellar rotation period and Rossby number. From the distribution of rotation period and convection parameter of M type stars, stellar chromospheric activity of M type stars depart from the anticipation of a. dynamo theory obviously. According to the analysis of the relation of between angle momentum and magneticmomentum, we find that a2 dynamo is main mechanism for the stars withdeep interior convection zone similarly late-M type stars. By the reserching the relation between stellar chromospheric activity and color index, we find that stellar ages play a pivotal role for producing Vaughan-Preston gap of MS stars. The relation between stellar chromospheric activity and rotation of evolution stars have a good relativity. But meticulous analysis show chromospheric activity of evolution stars depend on stellar spectral type and effective temperature strongly. We provide several possible explain for those phenomena.The corona activity of late-type main sequence stars also depend on the stellar spectral type. The corona activity of late-type MS stars exist a inflexion nearby F5. There have two fold reason. One reason is the change of interior convection zone with spectral type produce the phenomena; Another reason is the differential rotation of F type stars exist a upper limit. The corona activity of G, K, M type stars decrease with color index increasing as a whole. The result of statistics show the ratio of strong activity samples in M type MS stars is larger than that in other G, K type MS stars, the relation of between angle momentum and magnetic momentum of M type stars also depart from the whole relation of MS stars. Though this departure is not obvious, the result still support the conclusion in the analysis of stellar chromospheric activity. For evolution stars,wo don't, obtain significative result because the deficient samples. But the statistics analysis show the distrbution of corona activity of late type with color index and rotation period exist upper limit. And thoselimit have inflexion nearby B-V=1.0 and log P=1.75 respectively. Thoseinflexion are brought by the energy balance and heating mechanism in stellar chromosphere and corona.Using large samples, we gain several credible numeric relation between different magnetic activity index and rotational parameters.Between chromospheric activity index and corona activity index of MS stars, there exist good linear relativity. But for evolution stars, this relation show a large dispersion. This phenomenon farther surport our conclusion in the analysis of evolution stars, i.e. the difference of stellar chromosphere and corona activity of evolution stars is bred by the energy balance and heating mechanism in stellar chromosphere and corona.There have good linear relativity between stellar magnetic activity, rotational period and stellar age of MS stars, but this relativity of evolution stars has different action. For the evolution stars with age less than 109 years, stellar magnetic activity and rotational period decrease with stellar age; For the stars with age larger...
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