Rotation-Activity Relation of Ca II and Mg I Infrared Emission Lines of Young Stars. (arXiv:2104.02910v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Yamashita_M/0/1/0/all/0/1">Mai Yamashita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Itoh_Y/0/1/0/all/0/1">Yoichi Itoh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takagi_Y/0/1/0/all/0/1">Yuhei Takagi</a>
To reveal the detail of the internal structure, the relationship between
chromospheric activity and the Rossby number, N_R (= rotational period P /
convective turnover time tau_c), has been extensively examined for
main-sequence stars. The goal of our work is to apply the same methods to
pre-main-sequence (PMS) stars and identify the appropriate model of tau_c for
them. Yamashita et al. (2020) investigated the relationship between N_R and
strengths of the Ca II infrared triplet (IRT; lambda 8498, 8542, 8662 A)
emission lines of 60 PMS stars. Their equivalent widths are converted into the
emission line to stellar bolometric luminosity ratio (R’). The 54 PMS stars
have N_R < 10^{-1.0} and show R’ sim 10^{-4.2} as large as the maximum R’ of
the zero-age main-sequence (ZAMS) stars. However, because all R’ was saturated
against N_R, it was not possible to estimate the appropriate tau_c model for
the PMS stars. We noticed that Mg I emission lines at 8808 A is an optically
thin chromospheric line, appropriate for determination of the adequate tau_c
for PMS stars. Using the archive data of the Anglo-Australian Telescope
(AAT)/the University College London Echelle Spectrograph (UCLES), we
investigated the Mg I line of 52 ZAMS stars. After subtracting photospheric
absorption component, the Mg I line is detected as an emission line in 45 ZAMS
stars, whose R’ is between 10^{-5.9} and 10^{-4.1}. The Mg I line is not
saturated yet in “the saturated regime for the Ca II emission lines”, i.e.
10^{-1.6} < N_R < 10^{-0.8}. Therefore, the adequate tau_c for PMS stars can be
determined by measuring of their R’ values.
To reveal the detail of the internal structure, the relationship between
chromospheric activity and the Rossby number, N_R (= rotational period P /
convective turnover time tau_c), has been extensively examined for
main-sequence stars. The goal of our work is to apply the same methods to
pre-main-sequence (PMS) stars and identify the appropriate model of tau_c for
them. Yamashita et al. (2020) investigated the relationship between N_R and
strengths of the Ca II infrared triplet (IRT; lambda 8498, 8542, 8662 A)
emission lines of 60 PMS stars. Their equivalent widths are converted into the
emission line to stellar bolometric luminosity ratio (R’). The 54 PMS stars
have N_R < 10^{-1.0} and show R’ sim 10^{-4.2} as large as the maximum R’ of
the zero-age main-sequence (ZAMS) stars. However, because all R’ was saturated
against N_R, it was not possible to estimate the appropriate tau_c model for
the PMS stars. We noticed that Mg I emission lines at 8808 A is an optically
thin chromospheric line, appropriate for determination of the adequate tau_c
for PMS stars. Using the archive data of the Anglo-Australian Telescope
(AAT)/the University College London Echelle Spectrograph (UCLES), we
investigated the Mg I line of 52 ZAMS stars. After subtracting photospheric
absorption component, the Mg I line is detected as an emission line in 45 ZAMS
stars, whose R’ is between 10^{-5.9} and 10^{-4.1}. The Mg I line is not
saturated yet in “the saturated regime for the Ca II emission lines”, i.e.
10^{-1.6} < N_R < 10^{-0.8}. Therefore, the adequate tau_c for PMS stars can be
determined by measuring of their R’ values.
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