Photometric analysis of RS CVn eclipsing binary stars

العناوين الأخرى

تحليل ضوئي لنجوم ثنائية كسوفيه من مجموعة ثنائيات كلاب الصيد (رس)‎

مقدم أطروحة جامعية

Ahmad, Ayman Muwaffaq

مشرف أطروحة جامعية

al-Abbudi, Bushra Qasim

أعضاء اللجنة

Zaki, Wafa Hasan Ali
Karam, Nihad Ali
Khalaf, Salman Zaydan

الجامعة

جامعة بغداد

الكلية

كلية العلوم

القسم الأكاديمي

قسم الفلك و الفضاء

دولة الجامعة

العراق

الدرجة العلمية

ماجستير

تاريخ الدرجة العلمية

2013

الملخص الإنجليزي

Our study focuses on eclipsing binary system.

The variations in light intensity from eclipsing binary stars are caused when a star passes in front of the other relative to an observer.

If we assume that the stars are spherical and that they have circular orbits, then we can easily calculate how the light varies as a function of time, which is called a light curve, for eclipsing binary stars.

The discovery and detection of eclipsing binary systems comes from measuring the variation of the intensity of light through photometry.

The observed light intensity varies as the stars move through their orbits.

The light curves clearly show the effects of movement of the components of the system.

In this work, two computer modeling packages are used to study and analyses some of the short period group of the eclipsing RS Canum Venaticorum (RS CVn).

The first model is PHOEBE, which stands for PHysics Of Eclipsing BinariEs (PHOEBE), and the second is Binary Maker 3(BM3).

These packages are tools for the modeling of eclipsing binary stars based on photometric data.

PHOEBE is modeling software for eclipsing binaries which uses the Wilson- Devinney method.

The Wilson-Devinney code, WD method, computes a synthetic model of an eclipsing binary which is based on the Roche model.

The light curves of four selected eclipsing binaries of the short period group RS CVn which are, CG Cyg, CV Boo, RT And and BH Vir were Create PDF files without this message by purchasing novaPDF printer (http://www.novapdf.com) analyzed using PHOEBE and BM3 models.

The physical and geometrical elements were determined such as mass, radii, surface potential.

The results have been compared with the results of other researchers.

The synthetic light curves for these systems were generated using PHOEBE and BM3 models for two cases (unspotted and spotted models) and the physical parameters were determined for each system.

التخصصات الرئيسية

الفلك و علومه

عدد الصفحات

131

قائمة المحتويات

• APA
• MLA
• AMA

لغة النص

الإنجليزية

نوع البيانات

رسائل جامعية

رقم السجل

BIM-604206