Return to Japan 2303AD Index

Note on canonicity: This entire page is non-canon.
Thanks to the discovery of the Kuroishi brown dwarf in 2293 by the Japanese starship Tosa, Japan was able to open up a direct route to the 61 Cygni binary. The discovery was maintained as a secret for some time, and, coupled with the advent of the Kafer, resulted in a massive development effort by the Japanese military.
Considerable resources were poured into the development effort, which was primary aimed at developing a military sihpyard preparing for a possible Kafer invasion of the Sol system. Mitsuboshi Starframes was the lead developer, and brought with it a plethora of affiliated enteprises providing the diverse range of technologies needed to build starships.
While there are no habitable planets in the complex 61 Cygni system, and no suitably bright star to provide sunlight for solar power or agiculture at levels sufficient to operate a facility like the Mitsuboshi L-4 plant, readily-available material (including radioactives) has made it possible to establish a self-sufficient base.
The 61 Cygni binary star system is located about 11.4 light-years from Sol, in the south central part (21:08:52.1+38:56:51:D~, ICRS 2000.0) of constellation Cygnus, the Swan. 61 Cygni A and B orbit each other at an "average" distance (semi-major axis) of 86 astronomical units -- which is more than twice Pluto's orbital distance in the Solar System.
61 Cygni A and B have a highly elliptical orbit (e= 0.40) so that they are between 51.7 and 121.0 AUs apart, with one year equal to 721 Terran years.
The tidal stresses generated by the two stars in relatively close proximity, and their elliptical orbits, have created a massive jumble of asteroidal material, with no planet-sized bodies extant. There are a number of Luna-sized bodies, however, and a number of asteroidal clusters in relatively (>one million years) stable orbits. The majority of material is in the same plane of the starsf motion relative to each other, and normally all stutterwarping is done to a position relatively far from the ecliptic.
A major conglomeration of asteroidal material exists at the leading and trailing Trojan points of the binary star. The leading Trojan point (as viewed from Sol) is the center of most activity currently.

61 Cygni A
This star is an orange-red main sequence dwarf star, type K5.0 Ve. It is about 70 percent the mass of Sol, 72 percent of the diameter of Sol, and only about 8.5 percent as bright. It is a variable star.
The habitable zone (where liquid water would exist) around 61 Cygni A is centered around only 0.30 AU -- about three fourth's of Mercury's orbital distance in the Solar System. There is a moon-sized, airless rock there, with an orbital period of about 76.8 days -- less than a fourth of an Earth year. It has been named Yomi (‰©ς) and the sunward side is covered with extensive facilities for producing energy, foodstuffs and a range of organic materials.

61 Cygni B
This star is a orange-red main sequence dwarf star, type K7.0 Ve. It has about 63 percent of the mass of Sol, 67 percent the diameter and only 3.9 percent the luminosity. It is a variable.
The habitable zone for 61 Cygni B would be centered around only 0.20 AU -- about half of Mercury's orbital distance in the Solar System. A planet there would have an orbital period of about 46.6 days, but unfortunately none exists.

Distances to nearby stars according to Warp98 (2300AD.str)
DM+59 1915A (Struve 2398 AB) 6.04
DM+43 4305A (EV Lacertae) 6.03
DM-39 14192 1.50
Groombridge 34A 6.84
Kruger 60A 5.12
Ross 248 5.43
Kuroishi 6.55
Barnard's Star 9.3
BD+68 946 AB 9.7
Altair (BD+08 4236) 9.8

Ships under construction
IJS-FF20 Kobayakawa Hideaki ¬‘μGH
IJS-FF21 Mori Terumoto –Ρ—˜GŒ³
IJS-FF22 Ishida Mitsunari Ξ“cŽO¬
IJS-FF23 Ukita Hideie ‰FŠμ‘½G‰Ζ
IJS-OG5 Kalabaw (troops) .
IJS-OG6 Matefaaib (troops) .
IJS-DD14 Shiga Ž ‰κ
IJS-DD15 Tokushima “Ώ“‡
IJS-DD16 Fukuoka •Ÿ‰ͺ
IJS-CG06 Tokachi \Ÿ
IJS-CG07 Kirishima –Ά“‡
IJS-CG08 Unzen ‰_ε
IJS-BC03 Benkei •ΩŒc
IJS-BC04 Yamamoto Isoroku ŽR–{Œά\˜Z

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This page created 15 May 2008 and last revised on 26 May 2008.
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