【摘要】 本文给出了41个RS CVn型密近双星系统的J,H和K的测光结果和经证认为IRAS点源的40个Rs CVn系统的数据。对那些子星具有光谱分类的系统,我们讨论了它们的红外色余,发现只有少数系统具有红外色余。在近红外区有UX Ari,Z Her和HR 1099;在12μm处为SZ Psc。对那些具有确切的12、25μm流量并作了K星等测量的系统,我们讨论了他们在logf_2.2/f₁₂和logf₂₅/f₁₂的双色图上的位置。大多数RS CVn系统都在黑体线的附近。这一些结论却和P.Biermann和D.Hall所指出的红外色余是RS CVn型密近双星的一般特性所不相符合。对一些红外辐射有差异的天体应进一步研究。更多还原

【Abstract】 Hall pointed out that the infrared excess is a general characteristic of RS CVn systems. Verma et al. and Antounopolou published their near infrared observations of seyeral RS CVn systems and infrared excesses were presented in some systems. But we consider the above observations are not enough to lead to the conclusion that the infrared excess is a general characteristic of RS CVn systems.Of the 84 RS CVn systems listed in Hall’s catalog we have observed 41 systems in J,H, and K bands with a InSb photometer in 1984. The results are given in Table 1. 40 systems are identified as IRAS point sources, which are listed in Table 2.There are 13 systems in Table 1 whose components have MK spectral classifications. We calculated their (V-J)c, (V-H)c, and (V-K)c and compared them with the observations. The infrared excesses E(V-J), E(V-H), and E(V-K) are given in Table 3. The distribution of E(V-K) is shown in Fig. 1. There are 3 systems, UX Ari, HR1099, and Z Her, showjng infrared excesses. The infrared excesses of UX Ari and HR 1099 have already been observed by Verma et al..The same method was used to the flux at 12 ξm of 10 systems whose components have MK spectral classifications. The theoretical values of (F-[12] )c are calculated with Kurucz’s model. The results are listed in Table 4. Only one system, SZ Psc, show the infrared excess.If the circumstellar dust is presented in the RS CVn systems, the positions of these systems will deviate from the black body radiation line in the infrared color-color diagram. 21 systems that are listed in both Table 1 and Table 2 are plotted in the color-color diagram of log f12/f2.2 vs. log f25/f12. We find most RS CVn systems are close to the black body line. Only f55 And and HR 5110 deviate from the black body line. But if we use the data obtained by Johnson and Verma the positions of f55 And and HR 5110 are still in the normal star region. The difference between the data of Johnson and Verma and our observations of f55 And and HR 5110 is larger than observational error. The reason for the difference is unknown.In conclusion, the infrared excess is not a general characteristic of RS CVn systems.更多还原