Physical and geometrical parameters of CVBS XIV: the two nearby systems HIP 19206 and HIP 84425

Al-Wardat, Mashhoor A.; Abu-Alrob, Enas M.; Hussein, Abdallah M.; Mardini, Mohammad K.; Taani, Ali; Widyan, Hatem; Yousef, Zahraa T.; Al-Naimiy, Hamid M. K.; Yusuf, N.A.

doi:10.1088/1674-4527/21/7/161

Cited by 11 publications

(6 citation statements)

References 30 publications

(38 reference statements)

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“…Since then, it has been used for the estimation of the atmospheric and fundamental parameters of the components of BMSSs. It was successfully and accurately used to analyze several systems (see, e.g., Al-Wardat 2009, 2009Al-Wardat et al 2014a, 2014b, 2021bAl-Tawalbeh et al 2021;Yousef et al 2021;) and for analyzing multiple hierarchical systems like (Bochanski et al 2018).…”

Section: Methodsmentioning

confidence: 99%

Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems

Abu-Alrob

Hussein

Al-Wardat

2023

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We present detailed analyses of eight triple stellar systems (lying between 20 and 155 pc) and nine quadruple stellar systems (lying between 20 and 250 pc) with different configurations. Most of these systems are hierarchical. The systems are HIP 4239, HIP 5588, HIP 11072, HIP 12548, HIP 13498, HIP 17895, HIP 19915, HIP 22607, HIP 25240, HIP 28614, HIP 41171, HIP 51255, HIP 51966, HIP 54611, HIP 78977, HIP 89234, and HIP 111805. We followed a method that can be applied to all multiple stellar systems, including the main sequence and subgiant evolutionary stages, to obtain their masses, ages, and atmospheric and fundamental parameters. These parameters were assured by the combined analysis of the astrometric measurements, photometric measurements, dynamical analysis, synthetic photometry, metallicity, and positions of the components on the H-R diagram. The estimated individual masses are of higher accuracy than those given by the dynamical solutions and listed in the MSC. The results show that all components of each of these systems have precisely the same age and metallicity. This ensures that fragmentation is the most probable theory for the formation of these multiple stellar systems. A quadratic fit was calculated for the mass–luminosity relation of the main-sequence subset components. We found that the primary component in all of these systems has evolved off the main-sequence stage, and some of these stars have already entered the subgiant stage.

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Section: Methodsmentioning

confidence: 99%

Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems

Abu-Alrob

Hussein

Al-Wardat

2023

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“…Atmospheric and fundamental parameters of the components of BMSs have been estimated using Al-Wardat's method Al-Wardat et al (2021a). The method was successfully used to accurately analyze several BMSs (see, e.g., Al-Wardat 2002, 2009a, 2009bAl-Wardat et al 2014a, 2014b, 2016Masda et al 2016;Al-Wardat et al 2017;Masda et al 2018Masda et al , 2019aMasda et al , 2019bAl-Tawalbeh et al 2021;Yousef et al 2021;Al-Wardat et al 2021b). It has been shown to be an effective tool for investigating the accuracy of the measured trigonometric parallaxes by the Hipparcos and Gaia astrometric missions.…”

Section: Methodsmentioning

confidence: 99%

Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars

Hussein

Al-Wardat

Abushattal

et al. 2022

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We present the complete set of atmospheric and fundamental parameters, in addition to the masses, for the individual components of eight stellar systems. The list of the systems, whose orbital solutions were published recently, includes seven binaries (HIP 14524, HIP 16025, HIP 46199, HIP 47791, HIP 60444, HIP 61100, HIP 73085) and one triple system (HIP 28671). The systems were analyzed using a spectrophotometric computational technique known as Al-Wardats method for analyzing binary and multiple stellar systems, which makes use of ATLAS9 line-blanketed plane-parallel model atmospheres. Using these estimated parameters, the positions of the components were located on the Hertzsprung–Russell diagram, evolutionary tracks and isochrones to estimate their ages, the range depending on the uncertainties in their metallicities. Five systems were found to be pre-main-sequence stars (HIP 14524, HIP 46199, HIP 60444, HIP 61100, HIP 73085), two were main-sequence stars (the zero-age HIP 28671 and the 6.3 Gyr HIP 16025), and one is a subgiant system (HIP 47791) with an age of 1.4 Gyr. Fragmentation is proposed as the most probable formation process for the eight systems. A comparison between the estimated masses and the dynamical ones lead to new dynamical parallaxes for four systems: (28.63 ± 0.56) mas for HIP 14524, (15.6 ± 0.63) mas for HIP 16025, (9.73 ± 0.26) mas for HIP 47791, and (16.53 ± 0.59) mas for HIP 73085. Hence, the orbital solutions were reclassified. We conclude that Gaia DR3 parallaxes are more precise than those given by Gaia DR2 and Hipparcos 2.

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“…In 2002, we proposed a new approach to analyze BMSSs [3]. This novel method has been applied to a wide range of binary systems (e.g., [5], [6] [7], [1], [8], [9], and [4]). HIP 84092 is analyzed using our method for the first time in this work.…”

Section: Analysis Of Hip 84092mentioning

confidence: 99%

Gaia vs Hipparcos: the Accuracy of Parallax Measurements

Al-Wardat¹,

Hussein²,

Abu-Alrob³

2022

Proceedings of the Multifaceted Universe: Theory and Observations - 2022 — PoS(MUTO2022)

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We present a solution for the problem of the discrepancy in the measured trigonometric parallaxes for the stellar binary system HIP 84092. To solve the discrepancy, we used the orbital parameters and our method for analyzing binary and multiple stellar systems (BMSSs)s, described by Al-Wardat in 2002. We used all the available parallax measurements from Gaia DR3, DR2 and Hipparcos-2 in estimating the fundamental parameters of the individual components of the system. Such measurements are usually affected by the orbital motion of the components and the shift of the system photocenter. The masses estimated using the Al-Wardat method along with the modified orbital elements lead to a new dynamical parallax for the system 𝜋 𝐷𝑦𝑛 = 8.24 ± 0.15 mas, which lies in between the measurements of Hipparcos-2 (8.29±0.97 mas) and Gaia DR3 (8.4806±0.4863 mas), while the parallax from Gaia DR2 (20.0561 ± 1.1615 mas) is far from being accurate. This can be explained by the fact that the Gaia telescope has a higher resolution than that of Hipparcos. Based on the fundamental parameters of the binary system components and their positions on the evolutionary tracks, we conclude that the system consists of A7.5 and F1 solar-metalicity mainsequence stars with an age of 0.708 Gyr. Fragmentation is proposed as the most likely scenario for the formation and evolution of the system.

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Physical and geometrical parameters of CVBS XIV: the two nearby systems HIP 19206 and HIP 84425

Cited by 11 publications

References 30 publications

Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems

Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems

Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars

Gaia vs Hipparcos: the Accuracy of Parallax Measurements

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