Physical and geometrical parameters of VCBS XIII: HIP 105947

Masda, Suhail G.; Al-Wardat, Mashhoor A.; Pathan, J. M.

doi:10.1088/1674-4527/18/6/72

Cited by 13 publications

(11 citation statements)

References 46 publications

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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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Section: Methodsmentioning

confidence: 99%

Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars

Hussein

Al-Wardat

Abushattal

et al. 2022

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“…Nordström et al (2004) observed a double-lined RV spectrum for component A, affirming that the star is a subbinary system. The system was also determined as binary by Balega et al (2006), Mason et al (2010), andMasda et al (2018b). The first orbit for HIP 105947 was built by Balega et al (2006), using the Monet (1979) orbital analysis method.…”

Section: Hip 105947mentioning

confidence: 99%

“…Mason et al (2010) modified the orbit of the system using the newly released positional measurements and estimated a mass sum of 2.30 ± 1.14M e . The most recent analyses for HIP 105947 were performed by Masda et al (2018b) and Tokovinin (2019). Masda et al (2018b) estimated the physical parameters of the system as a binary using the method.…”

Section: Hip 105947mentioning

confidence: 99%

“…This makes it ideal for analyzing BMSSs and finding their physical properties. In fact, a lot of systems have been analyzed using this novel method since 2002 (e.g., , 2008, 2012Masda et al 2016Masda et al , 2018bMasda et al , 2019cYousef et al 2021;Yousef et al 2022). These papers used the analysis results to estimate the physical parameters of CVBMSSs, as well as to propose formation and evolution theories for the systems based on the parameters obtained.…”

Section: Introductionmentioning

confidence: 99%

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The True Nature of the Brightest Local Triple Stellar Candidates within 100 pc in the Galaxy

Yousef

Annuar

Al-Wardat

et al. 2023

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We present a study of a sample of bright (V ≤ 10 mag) and close (d ≤ 100 pc) triple–stellar system candidates in the galaxy, consisting of eight systems in total. Our aim is to determine their actual multiplicity and the physical properties of each stellar component in the systems. The sample was analyzed using a complex spectrophotometric technique by Al-Wardat that utilizes ATLAS9 line-blanketed plane-parallel model atmospheres. Based on our analysis, we found that five of the systems (HIP 109951, HIP 105947, HIP 40523, HIP 35733, and HIP 23824) are indeed triples, while the remaining three systems (HIP 9642, HIP 59426, and HIP 101227) are more consistent with being quadruples. We estimated the physical properties of the individual components using the most recent parallax measurements from the GAIA Data Release 3 catalog. We also examined the applicability of the well-established Mass–Luminosity (M–L) relation for individual components of all the stellar systems that have been analyzed by the Al-Wardat technique. We found that generally, the components are in good agreement with the established relationship. This further supports the reliability of the method in determining the physical properties of multiple stellar systems. In addition, we investigated the M–L relation for each order of stellar multiplicity (i.e., binary, triple, and quadruple) by performing linear fitting to the data. It was found that the slopes for each multiplicity are consistent with each other. The relations also seem to shift down in luminosity for a given total mass, as the order of multiplicity increases from binary to quadruple.

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“…These make it an ideal technique to study the properties of these systems. A series of papers that determine the complete set of physical and orbital properties of CVBMSs using this method and dynamical modeling technique developed by Tokovinin (1992), respectively, have been published for many systems (e.g., Al-Wardat 2007, Al-Wardat & Widyan 2009, Al-Wardat 2009, Al-Wardat 2012, Al-Wardat et al 2014a, Al-Wardat et al 2014b, Al-Wardat et al 2017, Masda et al 2018, Masda et al 2019band Masda et al 2019a). These analytical papers aim at taking the advantage of CVBMSs in estimating the key properties of the stellar components which is crucial in understanding the formation and evolution of the systems.…”

Section: Introductionmentioning

confidence: 99%

The stellar system HIP 101227: is it a binary, a triple or a quadruple system?

Yousef,

Annuar,

Hussein

et al. 2021

Preprint

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In this paper, we present the analysis of the stellar system HIP 101227 to determine the actual number of components in the system, and their properties. We use dynamical modeling and complex spectrophotometric (involving atmospheric modeling) techniques with recent data, to determine the physical properties and orbital solution for the system, respectively, with better accuracy than past studies. Based on our analysis, we found that the system is more consistent with being a quadruple rather than a binary, or a triple system as that suggested by previous studies. The total mass of the system determined from our SED analysis is 3.42 ± 0.20 M , which are distributed almost equally between the four stars. The stars are found to be zero-age main sequence stars; i.e., at the last stage of pre-main sequence,with age less than 200 Myr and spectral types K0. All four stars have very similar physical characteristics, suggesting that fragmentation process is the most likely theory for the formation and evolution of the system.

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Physical and geometrical parameters of VCBS XIII: HIP 105947

Cited by 13 publications

References 46 publications

Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars

Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars

The True Nature of the Brightest Local Triple Stellar Candidates within 100 pc in the Galaxy

The stellar system HIP 101227: is it a binary, a triple or a quadruple system?

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