Photoelectric Observations of BD - 3  1413 (HD 44701), a new Eclipsing Binary

Gum, C. S.

doi:10.1093/mnras/111.6.634

Cited by 2 publications

(10 citation statements)

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“…From table 1, where all available photometric data of IM Mon are listed, five photometric data sets (B band data of Gum (1951), B and V band data of Sanyal et al (1965), V band data of Shobbrook (2004) and H p band data of Hipparcos) are selected for simultaneous analysis of LCs together with the RVs of the components using the 2003 version of the Wilson-Devinney LC analysis code (Wilson & Devinney, 1971;Wilson, 1994). Selection was made according to their relative precision among others.…”

Section: Determination Of the Photometric Elementsmentioning

confidence: 99%

“…We estimated the uncertainties by using the uncertainties of the temperatures of the component stars. Considering the Gum, 1951), B2 (Sanyal et al, 1965),…”

Section: Astrophysical Parametersmentioning

confidence: 99%

“…B-band (Gum, 1951) B-band (Sanyal et al, 1965) Hp-band (ESA, 1997) V-band (Sanyal et al, 1965) V-band (Shobbrook, 2003) - uncertainties coming from the bolometric corrections and visual magnitude of the system, the distance modulus indicates a photometric distance of 353(59) pc to IM Mon, which is larger than the distance (304(36) pc) derived for IM Mon by van Leeuwen (2007) from the re-analysis of raw Hipparcos data, but not inconsistent with it in view of the large error bar of both distance determinations. In the original Hipparcos catalogue, the distance to IM Mon is given as 341(85) pc.…”

Section: Relative Intensitymentioning

confidence: 99%

“…IM Mon is a bright (V∼6.5 mag), early-type ((B-V)=-0.14 mag) and short orbital period (P∼1.2 days) eclipsing binary system. Its spectroscopic and photometric variations were discovered by Pearce (1932) and Gum (1951) respectively. The eccentricity of the spectroscopic orbit obtained by Pearce (1932) was commented to be spurious by Cester et al (1978) in their study on the determination of photometric elements of 14 detached systems.…”

Section: Introductionmentioning

confidence: 98%

“…The eccentricity of the spectroscopic orbit obtained by Pearce (1932) was commented to be spurious by Cester et al (1978) in their study on the determination of photometric elements of 14 detached systems. Cester et al (1978) studied early photometric observations of IM Mon, which were collected by Gum (1951) in integral light and by Sanyal, Mahra & Sanwal (1965) in B and V filters. However, due to a large scatter in all photometric observations, which is attributed to the intrinsic variability of one of the components by Sanyal, Mahra & Sanwal (1965), none of the authors was able to find a unique and precise solution for the system.…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Study of Eclipsing Binary and Multiple Systems in OB Associations. I. Orion OB1a- IM Monocerotis

Bakıș

Bakış

Bilir

et al. 2011

Publications of the Astronomical Society of Japan

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All available photometric and spectroscopic observations were collected and used as the basis of a detailed analysis of the close binary IM Mon. The orbital period of the binary was refined to 1. d 19024249(0.00000014). The Roche equipotentials, fractional luminosities (in B, V and H p -bands) and fractional radii for the component stars in addition to mass ratio q, inclination i of the orbit and the effective temperature T eff of the secondary cooler less massive component were obtained by the analysis of light curves. IM Mon is classified to be a detached binary system in contrast to the contact configuration estimations in the literature. The absolute parameters of IM Mon were derived by the simultaneous solutions of light and radial velocity curves as M 1,2 = 5.50(0.24) M ⊙ and 3.32(0.16) M ⊙ , R 1,2 = 3.15(0.04) R ⊙ and 2.36(0.03) R ⊙ , T eff1,2 = 17500(350) K and 14500(550) K implying spectral types of B4 and B6.5 ZAMS stars for the primary and secondary components respectively. The modelling of the high resolution spectrum revealed the rotational velocities of the component stars as V rot1 = 147(15) km s −1 and V rot2 = 90(25) km s −1 . The photometric distance 1 of 353(59) pc was found more precise and reliable than Hipparcos distance of 341 (85) pc. An evolutionary age of 11.5(1.5) Myr was obtained for IM Mon. Kinematical and dynamical analysis support the membership of the young thin-disk population system IM Mon to the Ori OB1a association dynamically. Finally, we derived the distance, age and metallicity information of Ori OB1a sub-group using the information of IM Mon parameters.

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Section: Determination Of the Photometric Elementsmentioning

confidence: 99%

“…We estimated the uncertainties by using the uncertainties of the temperatures of the component stars. Considering the Gum, 1951), B2 (Sanyal et al, 1965),…”

Section: Astrophysical Parametersmentioning

confidence: 99%

Section: Relative Intensitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%