Variable Star Discoveries
Flarestar Observatory has carried out a ground based photometric survey specifically designed to discover variable stars that where yet unknown to the astronomical community.
The survey was initiated on December 6, 2015. During the first night of the survey, two new variable stars were discovered. Data acquired on subsequent nights divulged the nature of the variability of these stars.
Analysis suggest that the variability of these two stars was caused by the presence of a companion star that blocked the light from the primary star called an eclipse, as the stars revolved around their centre of gravity.
This initial success prompts well for similar survey projects that are intended for the future.
Discovered from Flarestar Observatory on December 6th, 2015 during the first survey intended to seek out possible undiscovered variable stars. Data shows that this Algol-type variable star is a binary star system of Algol class.
Discovered from Flarestar Observatory on July 27, 2016 during a search in a field of an asteroid that was being studied at the time. Data shows that this variable star is a binary star system of W UMa class.
Fifth Discovery by Flarestar Observatory of a variable star within the constellation of Delphinus. First imaged on 2017 July 13 when following asteroid 219 Thusnelda.
Second Discovery by Flarestar Observatory of a variable star within the same field of UCAC4 735-019611. Also first imaged on December 6th., however period is half as much as that of the first discovery.
Discovered from Flarestar Observatory on October 30, 2016 following a search in a field of an asteroid that was being followedat the time. Data shows that this variable star is a binary star system of EW/RS CVn class
The sixth variable star discovery by Flarestar Observatory concerns a star located within the constellation of Aquila. It was first imaged on 2017 July 31 on images obtained by Dr Charles Galdies when following asteroid 9927 Tyutchev. Stephen M. Brincat discovered the star through this set of images and subsequently monitored the star on a number of nights from Flarestar Observatory. Observations revealed that the period is near half a day. thus it could would be difficult to determine the period from a single location. Therefore, observations from the ASAS-SN survey were added to achieve an accurate period.