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| ==Determining Orbital Durations (Years)==
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| 1. Determine '''base mass''':
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| {| align="center" border="2" style="background:#BDBDBD; text-align: center"
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| |+ '''Stellar Mass'''
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| |-
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| | '''Star Types''' || '''Solar Masses'''
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| |-
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| | D (White dwarf) || 0.36
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| |-
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| | B (Blue-white) || 4.4
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| |-
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| | A (White) || 2.1
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| |-
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| | F (Yellow-white) || 1.3
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| |-
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| | G (Yellow) || 0.94
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| |-
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| | K (Orange) || 0.57
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| |-
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| | M (Red) || 0.331
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| |}
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| 2) Add or subtract 1d10% from base mass for '''specific mass'''.
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| 3) Compute the orbital period using this formula: P = sqrt((D^3)/M), ''i.e.'', square root of D<sup>3</sup> divided by M, where:
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| * P = period in standard years (to third decimal); also list (in parenthesis) standard days (converted as by multiplying years by 365.24, to single decimal).
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| * D = Distance in AUs (as pre-determined by planetary surveys)
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| * M = specific mass of star
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