Komplexní studium V436 Per

JANÍK, Jan. Komplexní studium V436 Per. Brno, 2003, 86 s. disertační práce.

Základní údaje

Originální název

Komplexní studium V436 Per

Název česky

Komplexní studium V436 Per

Název anglicky

Complex study of V436 Per

Autoři

JANÍK, Jan ORCID

Vydání

Brno, 86 s. disertační práce, 2003

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Další údaje

Typ výsledku

Účelové publikace

Utajení

není předmětem státního či obchodního tajemství

Označené pro přenos do RIV

Ne

Klíčová slova česky

dvojhvězda V436 Per, fotometrie, spektroskopie

Klíčová slova anglicky

binary star V436 Per, fotometrie, spektroskopie

Příznaky

Recenzováno

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Anotace

V originále

An analysis of new spectroscopic and photoelectric UBV observations, satisfactorily covering the whole orbital period of V436 Per, together with existing data allowed me to improve the knowledge of the basic physical characteristics of the binary and its components. In several aspects, new results differ from the findings of Paper I: In particular, I found that it is the star eclipsed in the secondary minimum which is slightly more massive and larger than the optical primary. I also conclude that the apsidal advance – if present at all – is much slower than that estimated in a previous study. The orbital period might be increasing by 0.28 s per year but also this finding is very uncertain and needs verification by future observations. It is encouraging to note that two completely independent sets of programs for light-curve solutions lead to identical results. A notable finding is that both binary components rotate with very similar – if not identical – rotational periods of 1.45 d and 1.40 d, much shorter than what would correspond to a 10.9 d spinorbit synchronization period at periastron. Rapid line-profile changes reported earlier could not be confirmed from new, dedicated series of high-resolution and S/N spectra.

Česky

An analysis of new spectroscopic and photoelectric UBV observations, satisfactorily covering the whole orbital period of V436 Per, together with existing data allowed me to improve the knowledge of the basic physical characteristics of the binary and its components. In several aspects, new results differ from the findings of Paper I: In particular, I found that it is the star eclipsed in the secondary minimum which is slightly more massive and larger than the optical primary. I also conclude that the apsidal advance – if present at all – is much slower than that estimated in a previous study. The orbital period might be increasing by 0.28 s per year but also this finding is very uncertain and needs verification by future observations. It is encouraging to note that two completely independent sets of programs for light-curve solutions lead to identical results. A notable finding is that both binary components rotate with very similar – if not identical – rotational periods of 1.45 d and 1.40 d, much shorter than what would correspond to a 10.9 d spinorbit synchronization period at periastron. Rapid line-profile changes reported earlier could not be confirmed from new, dedicated series of high-resolution and S/N spectra.

Anglicky

An analysis of new spectroscopic and photoelectric UBV observations, satisfactorily covering the whole orbital period of V436 Per, together with existing data allowed me to improve the knowledge of the basic physical characteristics of the binary and its components. In several aspects, new results differ from the findings of Paper I: In particular, I found that it is the star eclipsed in the secondary minimum which is slightly more massive and larger than the optical primary. I also conclude that the apsidal advance – if present at all – is much slower than that estimated in a previous study. The orbital period might be increasing by 0.28 s per year but also this finding is very uncertain and needs verification by future observations. It is encouraging to note that two completely independent sets of programs for light-curve solutions lead to identical results. A notable finding is that both binary components rotate with very similar – if not identical – rotational periods of 1.45 d and 1.40 d, much shorter than what would correspond to a 10.9 d spinorbit synchronization period at periastron. Rapid line-profile changes reported earlier could not be confirmed from new, dedicated series of high-resolution and S/N spectra.