This star system consists of a single yellow dwarf G-class star. Although such stars have suitable longevity and sizeable habitable
zones, this system has no planets. Often when sufficient mass is available in a gas cloud to produce a G class star, matter that can not
accrete and contribute to star formation forms a protoplanetary disc. As some matter falls onto the star it transfers angular momentum
to other material further out in the disc. This outer material is then orbiting too fast to accrete and may form planets. Sometimes suitable
stars fail to develop planets or lose their planets. Our orbital simulations suggest that this star may have lost its protoplanetary disc in a
close interaction with another star and so planets most probably never formed around it. This star also has an unusually slow rate of
rotation, so much of the available material is likely to have accreted and contributed to star formation, leaving little left for planetary
formation. this is quite a large and luminous yellow dwarf (1.418 solar masses and 1.70 solar luminosities).
Nevertheless, every star is unique. By observing atmospheric and magnetic dynamics in this slow rotator and feeding the acquired data
into our computer models we can refine those models of stellar dynamics.
Acquire electromagnetic data then set a course for a new target system