Stellar Astronomy and Astrophysics

5.

Stellar Evolution: Main Sequence Phase

5.1.

Zero-Age Main Sequence

5.1.1.

Arrival Conditions

5.1.2.

Pre-Main-Sequence Contraction

5.1.3.

Onset of Hydrogen Burning

5.1.4.

ZAMS Properties

5.2.

Nuclear Fusion Processes

5.2.1.

Hydrogen Burning

5.2.1.1.

Proton-Proton Chain

5.2.1.1.1.

5.2.1.1.2.

5.2.1.1.3.

5.2.1.2.

5.2.1.2.1.

5.2.1.2.2.

5.2.1.2.3.

Temperature Dependence

5.2.2.

Core Conditions

5.2.2.1.

Temperature Requirements

5.2.2.2.

Pressure Requirements

5.2.2.3.

Quantum Tunneling

5.2.2.4.

5.3.

Main Sequence Structure

5.3.1.

Mass-Dependent Structure

5.3.1.1.

5.3.1.2.

Intermediate-Mass Stars

5.3.1.3.

High-Mass Stars

5.3.2.

Convective Cores

5.3.2.1.

Convective Core Mass

5.3.2.2.

Core Hydrogen Depletion

5.3.2.3.

5.3.3.

Radiative Envelopes

5.3.3.1.

Energy Transport

5.3.3.2.

Opacity Effects

5.4.

Main Sequence Evolution

5.4.1.

Compositional Changes

5.4.1.1.

Hydrogen Depletion

5.4.1.2.

Helium Accumulation

5.4.1.3.

Mean Molecular Weight

5.4.2.

Structural Changes

5.4.2.1.

Core Contraction

5.4.2.2.

Envelope Expansion

5.4.2.3.

Luminosity Evolution

5.4.3.

Evolutionary Timescales

5.4.3.1.

Nuclear Timescale

5.4.3.2.

Main Sequence Lifetime

5.4.3.3.

Mass-Lifetime Relation

5.5.

Mass-Dependent Properties

5.5.1.

Mass-Luminosity Relation

5.5.1.1.

Theoretical Basis

5.5.1.2.

Observational Confirmation

5.5.1.3.

Mass Range Validity

5.5.2.

Mass-Radius Relation

5.5.2.1.

Structural Dependence

5.5.2.2.

Equation of State Effects

5.5.3.

Mass-Temperature Relation

5.5.3.1.

Core Temperature

5.5.3.2.

Effective Temperature

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6. Post-Main-Sequence Evolution