Very massive stars in the local universe. ([2014])

• Record Type: Book
• Further Information: Note: Jorick S. Vink, editor.
• Editors: Vink, Jorick S
• Contents: Preface; Contents; Chapter1 Very Massive Stars in the Local Universe; 1.1 Introduction; 1.2 The Role of Very Massive Stars in the Universe; 1.3 Definition of a Very Massive Star; 1.4 The Very Existence of Very Massive Stars; 1.5 The Evolution and Fate of Very Massive Stars; References; Chapter2 Empirical Properties of Very Massive Stars; 2.1 Historical Background and Definition; 2.2 Very Massive Single Stars; 2.2.1 Atmosphere Models and Determination of StellarParameters; 2.2.2 Uncertainties on the Luminosity; 2.2.3 Uncertainties in Evolutionary Tracks. 2.2.4 The Best Cases for Very Massive Single StarsThe Arches Cluster; R136 in 30 Doradus; NGC 3603; Other Candidates; 2.3 Very Massive Stars in Binary Systems; 2.3.1 Massive Binaries and Dynamical Masses; Types of Binaries; Orbital Elements and Dynamical Masses; 2.3.2 The Most Massive Binary Systems; WR20a; NGC 3603 A1; R144 and R145; Summary and Conclusions; References; Chapter3 The Formation of Very Massive Stars; 3.1 Introduction; 3.2 The Formation of Very Massive Stars by Accretion; 3.2.1 Fragmentation; 3.2.2 Radiation Pressure; 3.2.3 Ionization Feedback; 3.2.4 Stellar Winds. 3.3 The Formation of Very Massive Stars by Collision3.3.1 Gas Accretion-Driven Collision Models; 3.3.2 Gas-Free Collision Models; 3.3.3 Stellar Evolution and Massive Star Mergers; 3.4 Observational Consequences and Tests; 3.4.1 The Shape of the Stellar Mass Function; 3.4.2 Environmental-Dependence of the Stellar Mass Function; 3.4.3 Companions to Massive Stars; Conclusions and Summary: Does Star Formation Have an Upper Mass Limit?; References; Chapter4 Mass-Loss Rates of Very Massive Stars; 4.1 Introduction; 4.2 O Stars with Optically Thin Winds; 4.2.1 Stellar Wind Equations. 4.2.2 CAK Solution4.2.3 Predictions Using a Monte Carlo Radiative Transfer Approach; 4.2.4 Line Acceleration Formalism g(r) for Monte Carlo Use; 4.3 Wolf-Rayet Stars with Optically Thick Winds; 4.3.1 Wolf-Rayet (WR) Stars; 4.3.2 WR Wind Theory; 4.3.3 Hydrodynamic Optically Thick Wind Models; 4.4 VMS and the Transition Between Optically Thin and Thick Winds; 4.4.1 Analytic Derivation of Transition Mass-Loss Rate; 4.4.2 Models Close to the Eddington Limit; 4.5 Predictions for Low Metallicity Z and Pop III Stars; 4.6 Luminous Blue Variables; 4.6.1 What Is an LBV?
• Publisher Details: Cham : Springer
• Publication Date: 2014
• Copyright Date: 2015
• Extent: 1 online resource (xi, 268 pages), illustrations (some color)
• Subjects: 523.8/8; Physics; Supergiant stars; SCIENCE -- Astronomy; Supergiant stars; Astronomy, space & time; Science -- Astrophysics & Space Science; Astrophysics; Electronic books
• Languages: English
• ISBNs: 9783319095967; 3319095951; 9783319095950
• Related ISBNs: 331909596X; 9783319095950
• Notes: Note: Includes bibliographical references and index.; Note: Online resource; title from PDF title page (SpringerLink, viewed November 14, 2014).
• Access Rights: Legal Deposit; Only available on premises controlled by the deposit library and to one user at any one time; The Legal Deposit Libraries (Non-Print Works) Regulations (UK).
• Access Usage: Restricted: Printing from this resource is governed by The Legal Deposit Libraries (Non-Print Works) Regulations (UK) and UK copyright law currently in force.