Abstract
The results of a non-LTE analysis of a number of spectral lines formed in the accreting envelopes of UX Ori stars are given. The accretion rate is estimated from an analysis of the first three lines of the Balmer series: M a = 10−8 −10−9 M ⊙ The gas temperature in this region is about 10,000 K. In the immediate vicinity of the star there is a hotter region, with T > 15,000 K, in which the 5876 Å line of neutral helium, observed in the spectra of these stars, is formed. The region of formation of this line has a small geometrical thickness, covers a small fraction of the star’s visible disk, and evidently consists of the site of contact of the accreting gas with the stellar surface. The low gas rotation rates in this region (150–200 km/sec) may mean that rapid rotation of the accreting gas is damped by the star’s magnetic field, which is strong enough to affect the gas stream. We estimate the magnetic field strength in this region to be about 150 G.
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Translated from Astrofizika, Vol. 42, No. 1, pp. 75–88, January–March, 1999.
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Tambovtseva, L.V., Grinin, V.P. & Kozlova, O.V. Non-LTE models of the accretion disks of UX Ori stars. Astrophysics 42, 54–63 (1999). https://doi.org/10.1007/BF02700914
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DOI: https://doi.org/10.1007/BF02700914