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.
• Vydání: Brno, 86 s. disertační práce, 2003.

Další údaje

• Typ výsledku: Účelové publikace
• Utajení: není předmětem státního či obchodního tajemství
• Klíčová slova česky: dvojhvězda V436 Per, fotometrie, spektroskopie
• Klíčová slova anglicky: binary star V436 Per, fotometrie, spektroskopie
• Příznaky: Recenzováno

Anotace

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.

Anotace 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.

Anotace 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.