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1979•Publications of the Astronomical Society of JapanRequires access

A Photoelectric Study of the Eclipsing Binary System KO Aquilae

Tadashi Hayasaka

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Abstract

Abstract UBV observations of KO Aquilae were made from 1973 to 1977. A light-curve analysis reveals that the fractional radius of the secondary component is smaller than its Roche limit, supporting Kopal’s (1959) previous classification. With the mass ratio q=m2/m1=0.2 as the most plausible value, it is doubtful that the system is in the pre-main-sequence evolutionary phase. Our observations indicate that the period of the system is increasing at the rate of 4.0×10−8 d per period and that the secondary minimum does not have a variable depth.

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Abstract UBV observations of KO Aquilae were made from 1973 to 1977. A light-curve analysis reveals that the fractional radius of the secondary component is smaller than its Roche limit, supporting Kopal’s (1959) previous classification. With the mass ratio q=m2/m1=0.2 as the most plausible value, it is doubtful that the system is in the pre-main-sequence evolutionary phase. Our observations indicate that the period of the system is increasing at the rate of 4.0×10−8 d per period and that the secondary minimum does not have a variable depth.

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Available abstract

Abstract UBV observations of KO Aquilae were made from 1973 to 1977. A light-curve analysis reveals that the fractional radius of the secondary component is smaller than its Roche limit, supporting Kopal’s (1959) previous classification. With the mass ratio q=m2/m1=0.2 as the most plausible value, it is doubtful that the system is in the pre-main-sequence evolutionary phase. Our observations indicate that the period of the system is increasing at the rate of 4.0×10−8 d per period and that the secondary minimum does not have a variable depth.

Key concepts: Physics, Photoelectric effect, Binary number, Astronomy, Astrophysics, Optics, Arithmetic, Mathematics

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