About possible explanations to the lines of radioactive elements in the spectrum of Przybylski's star

Yushchenko, A. V.; Gopka, V. F.; Goriely, Stéphane; Nazarenko, Sergey; Шаврина, А. В.; Kim, Chulhee; Doikov, D. N.

doi:10.22323/1.028.0198

Cited by 2 publications

(3 citation statements)

References 14 publications

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“…A similar result was reported by Bidelman (2005). Yushchenko et al (2006) found limits on the abundance of short-lived actinides in the atmosphere of HD 101065. Atmospheric modelling with new transition probabilities for a set of Pm lines ) and Ra and Ac lines ) supported the detection of these ions in HD 101065.…”

Section: Introductionmentioning

confidence: 97%

The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star

Mkrtichian

Hatzes²,

Saio³

et al. 2008

A&A

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Aims. We investigate the oscillation spectrum of the most chemically-peculiar star in the sky, the rapidly-oscillating magnetic (roAp) star HD 101065. Methods. High-precision radial velocity (RV) measurements, spanning four consecutive nights on 3-6 March, 2004, were obtained with the HARPS echelle-spectrometer at the ESO 3.6-m telescope, and photometric data were acquired during 6 nights of observations at the 24-inch telescope of Siding Spring Observatory. The RVs were measured using all spectral lines in the wavelength range 4400-5100 Å. Results. We detected a rich spectrum of oscillation modes with semi-amplitudes ranging between 217 m s −1 and 1.6 m s −1 . These belong to the complete spectrum of high-order, low = 0-2 modes, having a large spacing of Δν = 64.07 ± 0.9 μHz. We calculated the nonadiabatic frequencies of axisymmetric high-order p-modes for main-sequence models with dipole magnetic fields of two chemical compositions (X, Z) = (0.7, 0.02) and (X, Z) = (0.695, 0.025). The former composition provided the best fit model and yielded stellar parameters of mass, M = 1.525 ± 0.025 M , age = (1.5 ± 0.1) × 10 9 yr, effective temperature log T e = 3.821 ± 0.006, luminosity log L/L = 0.797 ± 0.026, surface gravity log g = 4.06 ± 0.04, and polar magnetic field strength, Bp = 8.7 ± 0.3 kG. We are able to identify the modes of all detected oscillation frequencies. The photometric U and B light curves have maxima that precede the RV maximum by 0.16-0.19 in phase.

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Section: Introductionmentioning

confidence: 97%

The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star

Mkrtichian

Hatzes²,

Saio³

et al. 2008

A&A

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“…The resonance line 4297.06 Å, which is expected to be strongest from the lines we considered, should be present in the spectrum, but it is absent. Its calculated profile with the technetium abundance adopted by Yushchenko et al (2006),

\log ϵ

(Tc/H)

\approx 3.5

is in a huge discordance with the observed profile of this blend. The problem is shown in Figure 1 (see also discussion in Ryabchikova 2008, who made first such a conclusion).…”

Section: Spectrum Synthesismentioning

confidence: 71%

“…Yushchenko & Gopka (2004), in their overview, also mentioned the presence of the Tc lines in Przybylski's star. Yushchenko et al (2006) performed a more detailed examination of this problem. The synthetic spectrum technique was applied to fit the 4124.22 Å line of Tc I.…”

Section: Introductionmentioning

confidence: 99%

Abundance of radioactive technetium in Przybylski's star revisited

2023

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We have searched for lines of the radioactive element technetium (Tc) in the spectrum of Przybylski's star (HD 101065). The nuclei of this chemical element are formed in the slow process of capturing thermalized neutrons. The possible lines of Tc I are heavily blended. We have synthesized the profile of one resonance line at 4297.06 Å , which is also a part of the complex blend, and we arrived at a decision that it is not visible in the spectrum (as was first noted by Ryabchikova), casting doubt on the existence of technetium in the atmosphere of the Przybylski's star. Therefore, based on our calculated combined profile, which has been adjusted to the observed blend profile at 4297.2 Å (that may possibly contain the resonance technetium line 4297.06 Å), we reduce the maximum technetium abundance to (Tc/H) = 2.5. This value can be considered only as an upper limit of the technetium abundance in the Przybylski's star.

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About possible explanations to the lines of radioactive elements in the spectrum of Przybylski's star

Cited by 2 publications

References 14 publications

The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star

The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star

Abundance of radioactive technetium in Przybylski's star revisited

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