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Fundamental Properties of High Mass X-Ray Binaries

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Fundamental Properties of High Mass X-Ray Binaries Fundamental properties of High-Mass X-ray Binaries Ana González Galán Fundamental properties of High-Mass X-ray Binaries Ana González-Galán PhD Thesis June 2014 Contents Contents 3 1 High Mass X-ray Binaries 9 1.1 About the donor star: OB supergiants . 11 1.1.1 The life of OB Supergiants ................. 14 1.1.2 Stellar winds of Supergiants . 17 1.2 About the compact object: Neutron stars . 18 1.3 Interaction mechanisms . 22 1.3.1 Tidal effects: Orbital circularisation . 22 1.3.2 Mass transfer: Accretion . 22 1.3.3 X-ray production and Eddington limit . 25 1.3.4 The theory of wind accretion . 26 1.4 Classification of HMXBs . 29 1.4.1 Roche-lobe overflow HMXBs . 29 1.4.2 BeX-rayBinaries . .. .. .. .. .. .. .. .. 30 1.4.3 Supergiant X-ray Binaries . 30 1.5 Formation and evolution of HMXBs . 33 1.5.1 Overview of the formation picture . 34 1.5.2 Evolution during the HMXB phase . 35 1.5.3 The "Common Envelope Phase" . 36 1.5.4 Final evolution of HMXBs . 37 2 Characterisation of HMXBs 39 2.1 Observations ............................ 41 2.1.1 Optical spectra . 41 2.1.2 X-ray light curves . 45 2.2 Dataanalysis ............................ 47 3 4 CONTENTS 2.2.1 Reduction of optical spectra . 47 2.2.2 Stellar atmosphere models: Synthetic spectra . 54 2.2.3 Measuring radial velocities . 57 2.2.4 Orbital solutions . 63 2.2.5 Hα variations ........................ 68 2.2.6 X-ray flux behaviour along the orbit . 69 3 FRODOSpec data reduction pipeline 71 3.1 Overview............................... 75 3.1.1 Input data . 75 3.1.2 Reduction process . 78 3.1.3 Ouput data products . 80 3.1.4 Codingplatform ....................... 80 3.2 Howtousethepipeline . .. .. .. .. .. .. .. .. .. 80 3.3 Step by step of my pipeline . 83 3.3.1 MODULE 1 . 85 3.3.2 MODULE 2 . 86 3.3.3 MODULE 3 . 88 3.3.4 MODULE 4 . 90 3.3.5 MODULE 5 . 92 3.3.6 MODULE 6 . 93 3.3.7 MODULE 7 . 98 3.3.8 MODULE 8 . 101 3.3.9 MODULE 9 . 102 3.3.10MODULE10.........................103 3.4 My results vs Officialresults .. .. .. .. .. .. .. ..105 4 IGR J00370+6122 111 4.1 Observations ............................112 4.2 Data analysis & Results . 112 4.2.1 Distance ...........................112 4.2.2 FASTWIND modelfit .....................118 4.2.3 Orbital solution . 121 4.2.4 X-ray light curves . 125 4.2.5 Evolution of Hα .......................129 4.3 Discussion..............................129 4.3.1 Orbital parameters . 131 4.3.2 Evolutionary context . 133 4.3.3 The zoo of wind-fed X-ray binaries . 138 CONTENTS 5 4.4 Conclusions .............................140 5 XTE J1855-026 143 5.1 Observations ............................148 5.2 Data Analysis & Results . 151 5.2.1 FASTWIND modelfit .....................151 5.2.2 Radial velocities & Orbital solutions . 154 5.2.3 Hα and He lines.......................164 5.2.4 X-ray light curves . 171 5.3 Discussion..............................172 5.3.1 Orbitalperiod ........................172 5.3.2 Spectral classification . 174 5.3.3 Orbital solution . 176 5.3.4 X-ray flux behaviour . 179 5.4 Conclusions .............................181 6 Two SFXTs: AX J1841.0-0535 & AX J1845.0-0433 183 6.1 Observations ............................187 6.2 Data Analysis & Results . 187 6.2.1 Spectral classification of AX J1841.0-0535 . 187 6.2.2 Radial velocity determinations . 191 6.2.3 Hα evolution.........................198 6.2.4 X-ray light curves . 202 6.3 Discussion..............................205 6.4 Conclusions .............................211 7 Conclusions & Future Work 213 A Resumen en Lengua Oficial de la Comunidad Valenciana 217 A.1 Contexto Científico . 217 A.1.1 Sobre la estrella "normal": Supergigantes OB . 219 A.1.2 Sobre la estrella compacta: Estrellas de neutrones . 221 A.1.3 Mecanismos de Interacción . 221 A.1.4 Clasificación de HMXBs . 223 A.1.5 Formación y Evolución de HMXBs . 226 A.2 Caracterización de fuentes . 227 A.3 Programa de reducción de datos del espectrográfo FRODOSpec 228 A.4 Resultados..............................229 A.4.1 IGR J00370+6122 . 229 6 CONTENTS A.4.2 XTEJ1855-026 . .. .. .. .. .. .. .. .. ..232 A.4.3 Dos SFXTs: AX J1841.0-0535 & AX J1845.0-0433 . 237 A.5 Conclusiones ............................239 List of Figures 241 List of Tables 245 Bibliography 247 Abstract The aim of this thesis is to characterise a sample of High Mass X-ray Binaries (HMXBs) formed by: IGR J00370+6122, XTE J1855-026, AX J1841.0-0535 and AX J1845.0-0433. These objects are composed of pulsars (rotating neu- tron stars) accreting material from the wind of their supergiant companions. The X-rays are produced in the interaction of the accreted material with the strong gravitational field of the neutron star that accelerates this material and heats it up to 107 K. ∼ The study of HMXBs has strong implications in several areas of Physics and Astrophysics. They contain neutron stars whose study is essential to constrain the equation of state of nuclear dense matter, and provides insights on the astrophysical models of core collapse and Supernovae explosions. HMXBs considered as a population give information on the properties of the galaxy. In addition they are excellent test-beds to study accretion physics and outflows. The X-ray behaviour of these systems determines the class of system (classical HMXBs, Supergiant Fast X-ray Transients, Be/X-ray Binaries). The differences in the X-ray emission are supposed to be due to the different properties of the binary systems, such as the orbital properties, the magnetic field of the neutron star or the spectral type of the donor star. HMXBs in this thesis are wind-fed systems, therefore, the properties of the wind (which depend on the spectral type) and the interaction of this wind with the gravitational field of the compact object are key elements to understand the X-ray emission. Therefore, in this thesis an orbital solution for each target of study has been determined using optical spectra of the donor star. Moreover, to check if wind variability is related to the orbit of the binary system, analysis of Hα varia- tions have been carried out. Furthermore, in the case of IGR J00370+6122 7 8 CONTENTS and XTE J1855-026 we have obtained an atmosphere model for each of the donor stars allowing us to characterise the atmospheres of these stars, and consequently to determine physical parameters such as the Teff or the log g. Finally publicly available X-ray light curves have been analysed to study the X- ray emission of the different sources against their orbital periods. As a general conclusion, it seems there is a continuum of properties of these systems more than a strict classification. A combination of factors, of which some of them could be unknown, might be the cause of their different X-ray flux behaviours. The outline of this thesis is as follows: the scientific context is given in Chap- ter 1; an overview of the analysis performed for each of the sources of study is presented in Chapter 2; Chapter 3 is dedicated to the description of a pipeline optimised for the reduction of FRODOSpec spectra of obscured red sources (donor stars of the targets of study); Chapters (4, 5 and 6) present the charac- terisation of the four sources in this thesis, which are different kind of wind-fed systems; and finally general conclusions and future work are given in Chap- ter 7. CHAPTER 1 High Mass X-ray Binaries The discovery of the first extra-solar X-ray source [Sco X-1; Giacconi et al., 1962] constituted the beginning of X-ray astronomy. Since then, the interest and discoveries related to X/γ-ray astronomy has grown thanks to the ability to send X-ray space missions above the Earth’s atmosphere with more than half a million X-ray sources detected up to date. X-ray binaries (XRBs) are point-like X-ray sources. These systems consist of a compact object – a neutron star (NS) or a black hole (BH) – orbiting a com- panion, or donor, star from which there is an accretion of material. Following the canonical model, first proposed by Shklovskii [1967], this material is ac- celerated in the strong gravitational field of the compact star and heated up to 107 K before being accreted, giving as a result the observed X-ray radiation. The∼ basic division of XRBs into the high-mass (HMXBs) and low-mass (LMXBs) systems refers to the mass of the donor star. The donor star of LMXBs is a low- mass star, with a typical mass of . 1 M , and a spectral type later than B. While the masses of donor stars in HMXBs⊙ are normally taken to be & 10 M , they are hot luminous OB supergiants. There have been detected 300 high⊙ en- ergy binary systems in the Milky Way of which 60% are LMXBs∼ and 40% are HMXBs [Chaty, 2013]. ∼ ∼ Most of the compact objects hosting HMXBs [& 60%; in’t Zand et al., 2007] are known to be pulsars, i.e. rotating NSs (see Fig. 1.1 for an scheme of this kind of system). These pulsars have strong magnetic fields ( 1012 G) of which magnetic axis is not aligned with its rotational axis (see Fig.∼ 1.2). Therefore, the X-ray radiation coming from the material accreted on to the pulsar is mod- 9 Chapter 1. High Mass X-ray Binaries Figure 1.1: Scheme of a HMXB with an rotating NS (© HKU@LCSD). ulated by the stellar rotation of the pulsar. For a review of this subject, see e.g., Nagase [1989].
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