Интерферометрия и спектрофотометрия двойных звезд солнечного типа

• Автор: Аль-Вардат Машхур Ахмад
• Шифр специальности: 01.03.02
• Научная степень: Кандидатская
• Год защиты: 2003
• Место защиты: Нижний Архыз
• Количество страниц: 171 с. : ил.

Russian Academy of Sciences Special Astrophysical Observatory
published as a manuscript Int. Classification Code: 524.382;520.
AL-WARDAT MASHHOOR AHMAD
Interferometry and Spectrophotometry of
Solar Type Binary Stars
Specialization: 01. 03. 02 - Astrophysics and Radio Astronomy
Dissertation to defend the scientific grade of Candidate (Ph.D.) of Physical- Mathematical Sciences
Supervisor: Doctor of Science, Balega Yu. Yu.
Nizhnij Arkhyz- 2
“Each time I was in a problem, or I faced the dark side of this life
Each time I was in happiness, or I faced the shiny side of this life
There was a hidden strength, either from inside myself or through my relatives and friends, pushing me forward. To the Almighty and holder of that strength, and
To all those whom I felt that strength through,
I dedicate this work. ”
Mashhoor
Table of Contents
Table of Contents
1 The Astrophysical Problems of Studying Binary Stars
1.1 Milestones in the history of binary stars
1.2 Classification of binary stars
1.3 Binary star formation mechanisms
1.4 Statistics of binary stars and their catalogues
1.5 Conclusion
2 Speckle Interferometry of Binary Stars
2.1 Introduction
2.2 Qualitative description
2.3 Theoretical description
2.4 Programme of the stars
2.5 Observations and data analysis
2.6 Results and discussion
2.6.1 HIP
2.6.2 HD 25811 (BAG 4)
2.6.3 COU 1
2.6.4 COU 1
2.6.5 41 Dra
2.7 Conclusions
3 Spectrophotometry of Binary Stars
3.1 Introduction
3.2 Programme of the stars
3.3 Observations and data analysis
3.4 Results and discussion
3.5 Conclusions
4 Physical Parameters of the Components of Binary Stars
4.1 Introduction
4.2 The quadruple system ADS 11
4.2.1 Observational results
4.2.2 Atmospheric modeling and discussion

CHAPTER 2. SPECKLE INTERFEROMETRY OF BINARY STARS

jf •**»

■ 4 * * f. V-
■ '4ra.l№..

Figure 2.2: Short exposure image of a resolvable star taken at the focus of the 6-m telescope.
are two equivalent methods of analysis: the autocorrelation method and the power spectrum method. In the autocorrelation method, an estimate of the ensemble average spatial autocorrelation of the image intensity is found (Fig. 2.3):
C(Ax, Ay) = J J I(x, y)I{x + Aar, y + Ay)dxdy
= I{x,y) + I{x,y) (2-3)
= {0{x,y) ® 0(x,y)} * {P[x,y) © P(x,y)}
In the power (or, more correctly, energy) spectrum method (Fig. 2.4), we find the quantity V(u,u) = (| I{u,u) |2)
(2.4)
= 1 0(u, u) |2-(| P(u, v) |2) where the tilde denotes the Fourier transform, for example,
i(u, v) = J J I(x,y)exp[—2iYi(ux + L>y)]dxdy
By invoking the autocorrelation theorem of Fourier transforms, it is straightforward to show that C(Ax, Ay) and W(u, v) are Fourier transform pairs, so that knowledge of either function is equivalent to that of the other.