Eras

0.0 (before 2.4 billion BCE)

Pre-Pylistroph

1.0 (c. 2.4 billion BCE)

The Pylistroph

2.0 (c. 1.2 billion BCE)

Flight of the Daamin & Schism of the Hlutr. Nephestal founded.
2.1 (c. 600 million BCE)
Empire of the Iaranori
2.2 (c. 22 million BCE)
Virgo Wars
2.4 (c. 5.2 million BCE)
Avethellan Empire
2.6 (c. 1.63 million BCE)
Dorascan Empire
2.8 (c. 900,000 BCE)
Marpethtal Empire
2.9 (c. 800,000 BCE)
Empire of the Miethara

3.0 (c. 100,000 BCE)

Pre-Imperial Terra
3.75 Dance for the Ivory Madonna
3.962 "Gamester"
3.958 "Big Improvement"

4.0 (2153 CE/TE 0/12,153 HE)

5.0 (2624 CE/TE 471/12,624 HE)

Interregnum
5.38 A Rose From Old Terra

6.0 (2488 CE/12,488 HE)

New Continuum
6.55 "The Geas Ingenerate"

7.0 (10,274 CE/20,274 HE)

Second Terran Empire

8.0 (10,356 CE/24,356 HE)

Post-Imperial Humanity
8.5 The Leaves of October

9.0 (c. 3 million HE)

Endtime

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Mu Cassiopeiae

Primary of Odudua.

Spectral Class: G5

Mu Cassiopeiae (μ Cas, μ Cassiopeiae) is a binary star system in the constellation Cassiopeia. This system shares the name Marfak with Theta Cassiopeiae, and the name was from Al Marfik or Al Mirfaq (المرفق), meaning "the elbow".

In 1961 the close binary nature of this system was discovered by Nicholas E. Wagman at the Allegheny Observatory. Since then the orbital elements of the two stars have been fairly well established. The two stars are separated by a semimajor axis of 7.61 AUs with distance range of 3.3-11.9 AUs. In 1966, the individual components were first resolved by the American astronomer Peter A. Wehinger using the 84-inch reflector at the Kitt Peak National Observatory, allowing an initial estimate of separate masses.

Compared to other nearby stars, this pair are moving at a relatively high velocity of 167 km/s through the Milky Way galaxy. They are low metal, Population II stars that are thought to have formed before the galactic disk first appeared.

This star will be in constellation Perseus around 5200 AD.

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Mu Cassiopeiae