Complex Analysis of the Stellar Binary HD25811: A Subgiant System

Al-Wardat, Mashhoor A.; Widyan, Hatem; Al-thyabat, Ahmed

doi:10.1017/pasa.2013.42

Cited by 16 publications

(14 citation statements)

References 35 publications

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“…This is the closest mass to the 3.32 M calculated using Gaia parallax and the orbital elements of Al-Wardat et al (2014a), another indicator of the reliability of Al-Wardat's method. Adopting the physical and geometrical parameters of the system given by Al-Wardat et al (2014a). would suggest a little bit higher parallax than that of Gaia, that is, the system is a bit closer.…”

Section: Notes On Specific Systemsmentioning

confidence: 60%

“…Some of the parallaxes obtained by Hipparcos give masses more consistent with the photometric and dynamic system parameters than DR2. On the other hand, Al-Wardat's method estimated a parallax for the system HD25811, which had no parallax from Hipparcos, as 5.095 ± 0.095 mas in 2014 (Al-Wardat et al 2014a). This value is very close to that of Gaia DR2 -4.953 ± 0.081 mas.…”

Section: Discussionmentioning

confidence: 99%

“…A possible explanation is that the trigonometric parallax measurements have been distorted by the orbital motion of the components of such systems, which affects the position of the photo-centre of the system (Shatskii & Tokovinin 1998). Individual systems are discussed below: HD 25811: This system was analysed using Al-Wardat's method (Al-Wardat et al 2014a). In spite of the fact that there was no measured trigonometric parallax at that time, they estimated M a = 1.55 ± 0.16 M , M b = 1.50 ± 0.15 M , and a dynamical parallax (π = 5.095 ± 0.095 mas, d = 196.27 pc) depending on an initial value (π = 5.24 ± 0.6 mas, d = 191 pc) taken from Al-Wardat (2003).…”

Section: Notes On Specific Systemsmentioning

confidence: 99%

“…We investigated how measurements of the dynamical masses of the selected CVBSs are affected by the distances inferred from the parallax measurements in each of the catalogues discussed above. We also compared these results with masses estimated from two different indirect methods: Malkov's photometric masses (Malkov et al 2012a,b) and Al-Wardat's multi-parameter approach for analysing CVBSs (Al-Wardat 2002a,b, 2007Al-Wardat et al 2014b;Al-Wardat, Widyan, & Al-thyabat 2014a;Al-Wardat et al 2016, 2017Masda, Al-Wardat, & Pathan 2018a;Masda, Al-Wardat, & Pathan 2018c). The latter is a computationally complex method employing colours, colour indices, and magnitude differences of the system along with its parallax to build individual synthetic spectral energy distributions (SED) for each component of the system.…”

Section: Introductionmentioning

confidence: 99%

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Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses

Al-Wardat

Hussein

Al-Naimiy

et al. 2021

Publ. Astron. Soc. Aust.

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Precise measurement of the fundamental parameters of stellar systems, including mass and radius, depends critically on how well the stellar distances are known. Astrometry from space provides parallax measurements of unprecented accuracy, from which distances can be derived, initially from the Hipparcos mission, with a further refinement of that analysis provided by van Leeuwen in 2007. The publication of the Gaia DR2 catalogue promises a dramatic improvement in the available data. We have recalculated the dynamical masses of a sample of 1 700 close visual binary stars using Gaia DR2 and compared the results with masses derived from both the original and enhanced Hipparcos data. We show the van Leeuwen analysis yields results close to those of Gaia DR2, but the latter are significantly more accurate. We consider the impact of the Gaia DR2 parallaxes on our understanding of the sample of visual binaries.

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Section: Notes On Specific Systemsmentioning

confidence: 60%

Section: Discussionmentioning

confidence: 99%

Section: Notes On Specific Systemsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses

Al-Wardat

Hussein

Al-Naimiy

et al. 2021

Publ. Astron. Soc. Aust.

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“…These parameters include the effective temperatures, radii, orbital elements, spectral types, luminosity classes and masses for both components of the binary system. The method was successfully applied to several main sequence binary systems: ADS11061, Cou1289, Cou1291, Hip11352, Hip11253, Hip70973 and Hip72479 [1,2,4,6,8], and to the subgiant systems HD25811 and HD375 [7,9].…”

Section: Introductionmentioning

confidence: 99%

Physical and geometrical parameters of the binary system gliese 150.2

et al. 2014

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Atmospheric modeling and dynamical analysis of the components of the visually close binary system (VCBS) HD6009 were used to estimate their individual physical and geometrical parameters. Model atmospheres were constructed using a grid of Kurucz solar metalicity blanketed models, and used to compute the individual synthetic spectral energy distribution (SED) for each component separately. These SEDs were combined together to compute the entire SED for the system from the net luminosities of the components a and b located at a distance d from the Earth. We used the feedback modified parameters and iteration method to get the best fit between synthetic and observational entire SEDs.The physical and geometrical parameters of the system's components were derived as:15M⊙, La = 6.80 ± 0.75L⊙, L b = 6.09 ± 0.75L⊙ and π = 14.43mas dynamical parallax. The system is shown to be consist of G6 IV primary and G6 IV secondary components.

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Stellar parameters of the two binary systems: HIP 14075 and HIP 14230

Masda

Al-Wardat

Pathan³

2018

J Astrophys Astron

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We present the stellar parameters of the individual components of the two old close binary systems HIP 14075 and HIP 14230 using synthetic photometric analysis. These parameters are accurately calculated based on the best match between the synthetic photometric results within three different photometric systems with the observed photometry of the entire system. From the synthetic photometry, we derive the masses and radii of HIP 14075 as: M A = 0.99 ± 0.19 M , R A = 0.877 ± 0.08 R for the primary and M B = 0.96 ± 0.15 M , R B = 0.821 ± 0.07 R for the secondary, and of HIP 14230 as: M A = 1.18 ± 0.22 M , R A = 1.234 ± 0.05 R for the primary and M B = 0.84 ± 0.12 M , R B = 0.820 ± 0.05 R for the secondary, both systems depend on Gaia parallaxes. Based on the positions of the components of the two systems on a theoretical Hertzsprung-Russell diagram, we find that the age of HIP 14075 is 11.5 ± 2.0 Gyr and of HIP 14230 is 3.5 ± 1.5 Gyr. Our analysis reveals that both systems are old close binary systems (≈> 4 Gyr). Finally, the positions of the components of both systems on the stellar evolutionary tracks and isochrones are discussed.

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Complex Analysis of the Stellar Binary HD25811: A Subgiant System

Cited by 16 publications

References 35 publications

Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses

Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses

Physical and geometrical parameters of the binary system gliese 150.2

Stellar parameters of the two binary systems: HIP 14075 and HIP 14230

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