'Mass radius relation' presentation slideshows

ASTR377: A six week marathon through the firmament

ASTR377: A six week marathon through the firmament. by Orsola De Marco orsola@science.mq.edu.au Office: E7A 316 Phone: 9850 4241. Week 5, May 17-20, 2009. Overview of the course. Where and what are the stars. How we perceive them, how we measure them.

548 views • 49 slides

Stellar Structure

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Ay 123 Lecture 4 - Energy & Opacity

Ay 123 Lecture 4 - Energy & Opacity. Energy from Nuclear Reactions. Fission. Binding energy per nucleon. Fusion. Atomic # A. Temperature Dependence of p-p & CNO chains. Bound-free Opacity ? bf (?). Ay 123 Lecture 5 - Homology & Main Sequence. Mass-Luminosity Relation. L ? M 3.9.

153 views • 6 slides

1. INTRODUCTION

a 2. r 2. Figure 1 - If the secondary star in a binary fills its Roche lobe and is rotating synchronously, the ratio of its rotational velocity to its projected orbital velocity is a strong function of mass ratio because.

108 views • 1 slides

QCD phase transition in neutron stars and gamma-ray bursts

QCD phase transition in neutron stars and gamma-ray bursts. Wu, K. 1 , Menezes, D. P. 2,3 , Melrose, D. B. 3 and Providencia, C. 4. 1 Mullard Space Science Laboratory, University College London, UK 2 Departmento de Fisica, CFM, Universidade Federal de Santa Catarina, Brazil

223 views • 1 slides

1. INTRODUCTION

a 2. r 2. Figure 1 - If the secondary star in a binary fills its Roche lobe and is rotating synchronously, the ratio of its rotational velocity to its projected orbital velocity is a strong function of mass ratio because.

69 views • 1 slides