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Sue Ann Heatherly edited results_table.md
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###
Connections to Littlewood’s Conjecture
We show the energy radiated in the convective region to be proportional
to the mass in the radiative layer between the stellar surface and the
upper boundary of the convective zone, as shown in the following table and in Figure \ref{fig:fig1}:
|**Phase** | **Time** | **M\(_ 1\)** | **M\(_ 2\)** | **\(\Delta M\)** | **P** | **\(v_{\rm rot,1}\)** | **\(v_{\rm rot,2}\)** |
|:------------------|:----------|-------------|-------------|----------------|-------|---------------------|---------------------|
|1 ZAMS | 0 | 16 | 15 | – | 5.0 | 230 | 230 |
|2 Case B | 9.89 | 15.92 | 14.94 | 0.14 | 5.1 | 96 | 85 |
|3 ECCB | 11.30 | 3.71 | 20.86 | 6.44 | 42.7 | 40 | 767 |
|4 ECHB | 18.10 | – | 16.76 | – | – | – | 202 |
|5 ICB | 18.56 | – | 12.85 | – | – | – | 191 |
|6 ECCB | 18.56 | – | 12.83 | – | – | – | 258 | Galaxies
We see a different result when imaging galaxies. As seen in the figure below with M123, longer exposure times result in images with greater clarity.
