Lab 04: Mass-Luminosity Relation and Main-Sequence Lifetimes for Real Stars

Apply the mass-luminosity relation and lifetime scaling to the Sun, Alpha Centauri A/B, and Sirius A.

Apparatus and Setup

This lab applies the mass-luminosity relation and main-sequence lifetime scaling (Lecture 07) to four real, precisely measured stars: the Sun, Alpha Centauri A and B, and Sirius A (all carried forward with established provenance from ASTR 230/ASTR 310).

Materials and Data

StarMass (M⊙)Measured L (L⊙)
Sun1.0001.000
Alpha Centauri A1.07881.5059
Alpha Centauri B0.90920.4981
Sirius A2.06325.4

Procedure

  1. For each of the three non-solar stars, compute the mass-luminosity prediction L ≈ M^3.5 and the percent agreement with the measured luminosity in the data table.
  2. For each of the four stars, compute the main-sequence lifetime estimate t_MS = 10 Gyr × (M/M⊙)/(L/L⊙) using the measured (not predicted) luminosity.
  3. Rank the four stars by main-sequence lifetime, and state which single input (mass or luminosity) is most responsible for Sirius A having by far the shortest lifetime of the four.
  4. The Sun's actual age is about 4.57 Gyr. Compare this to your computed solar main-sequence lifetime, and state what fraction of its total main-sequence lifetime the Sun has completed so far.

Analysis and Uncertainty

Sirius A's percent agreement (step 1) is expected to be noticeably worse than Alpha Centauri A/B's; state explicitly why a single fixed mass-luminosity exponent (3.5) is not expected to fit equally well across a wide range of stellar masses.

Deliverables

Assessment Criteria

References and Provenance