naa a22 4500 510732100 CHVBK 20180411082956.0 cr unu---uuuuu 180411e20130901xx s 000 0 eng 10.1134/S1063772913090023 doi (NATIONALLICENCE)springer-10.1134/S1063772913090023 The character of solar-type activity and the depth of the convective zone [Elektronische Daten] [M. Katsova, M. Livshits, T. Mishenina] The origin of solar-type activity for low-mass stars of late spectral types is considered. Spectroscopic data were used to study the dependence of the activity level logR′ HK on the lithium abundance logA(Li) and axial rotation rate. A close correlation between logA(Li) and logR′ HK is found for two groups of G stars, hotter and cooler than the Sun. This relation is most clearly expressed in the case of high activity, and is somewhat more strongly expressed for G6-K3 dwarfs, which includes many BY Dra variables, than for F8-G5 stars. It is confirmed that, for stars with high activity, both the lithium abundance and the activity level are determined by the rotation rate, which depends on the age. The lithium abundance exhibits different dependences on the chromospheric activity, depending on the level of this activity. Cooler stars, with detectable lithium and solar-like chromospheres, possess much stronger coronas. This change in the relationship between the relative luminosities of the chromosphere and corona can be reliably traced using larger datasets. The different ratios between the activity of the choromosphere and corona for cooler and hotter G stars may reflect the fact that their convective zones become deeper or shallower than some critical value. This is consistent with observations of parameters describing rotational modulation and the correlation and anti-correlation of chromospheric and photospheric activity indices for stars hotter and cooler than the Sun. Physically, this means that the character of the activity could be related to a changing contribution of the large-scale and local magnetic fields to the generation of the activity. The results of this study confirm the earlier idea that there may be different evolution paths associated with solar-type activity. The results can be used to refine methods for estimating ages of stars from their activity levels (gyrochronology). Pleiades Publishing, Ltd., 2013 Katsova M. Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. 13, 119991, Moscow, Russia aut Livshits M. N.V. Pushkov Institute of Terrestrial Magnetism, the Ionosphere, and Radio-Wave Propagation, Russian Academy of Sciences, Kaluzhskoe shosse 4, 142190, Troitsk, Moscow, Russia aut Mishenina T. Astronomical Observatory, I.I. Mechnikov Odessa National University, Marazlievskaya ul. 1v (T.G. Shevchenko park), 65014, Odessa, Ukraine aut Astronomy Reports Springer US; http://www.springer-ny.com 57/9(2013-09-01), 702-713 1063-7729 57:9<702 2013 57 11444 https://doi.org/10.1134/S1063772913090023 text/html Onlinezugriff via DOI 1 research-article jats NATIONALLICENCE 856 40 https://doi.org/10.1134/S1063772913090023 text/html Onlinezugriff via DOI NATIONALLICENCE 700 1- Katsova M. Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. 13, 119991, Moscow, Russia aut NATIONALLICENCE 700 1- Livshits M. N.V. Pushkov Institute of Terrestrial Magnetism, the Ionosphere, and Radio-Wave Propagation, Russian Academy of Sciences, Kaluzhskoe shosse 4, 142190, Troitsk, Moscow, Russia aut NATIONALLICENCE 700 1- Mishenina T. Astronomical Observatory, I.I. Mechnikov Odessa National University, Marazlievskaya ul. 1v (T.G. Shevchenko park), 65014, Odessa, Ukraine aut NATIONALLICENCE 773 0- Astronomy Reports Springer US; http://www.springer-ny.com 57/9(2013-09-01), 702-713 1063-7729 57:9<702 2013 57 11444 Metadata rights reserved Springer special CC-BY-NC licence nationallicence BK010053 XK010053 XK010000 NATIONALLICENCE NATIONALLICENCE NL-springer