Stellar wind as a key to the understanding of spectral activity of IN Com

  • O.V. Kozlova Crimean Astrophysical Observatory of Taras Shevchenko National University of Kiev, Nauchnyi, Ukraine
  • I.Yu. Alekseev Crimean Astrophysical Observatory of Taras Shevchenko National University of Kiev, Nauchnyi, Ukraine

Abstract

We present long-term spectral observations (R = 20000) of IN Com in the region of Hα, Hβ and HeI 5876 lines. The distinguishing characteristic of stellar spectrum is the presence in the Hα line the extended two-component emission with limits up to ± 400 km/s. Emission parameters show the rotation modulation with the stellar rotation period and a significant variability on the long-term scale. Similar emission is observed also in Hβ and HeI 5876 lines. Our results allow us to conclude that observational emission profiles are formed in optically thin hot gas. It is a result of presence of circumstellar gas disk around IN Com. Its size does not exceed some stellar radii. The material for the disk is supported by IN Com stellar wind. The detected variability of Hα emission parameters shows an evident connection with photopolarimetric activity of the star. This fact allows us to associate the long-term spectral variability with cycles of stellar activity of IN Com.

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Published
2013-07-01
How to Cite
Kozlova O., Alekseev I., 2013. Izvestiya Krymskoi Astrofizicheskoi Observatorii, vol. 109, no. 3, pp. 161-172. Available at: https://jn.craocrimea.ru/index.php/izvcrao/article/view/414 (Accessed: 4December2020)
Section
Сonference proceedings