​Flarestar Observatory, a private astronomical station on Malta island, has the IAU/MPC Observatory Code: 171. The observatory’s main objective is to obtain precise photometric data of variable stars and minor planets (asteroids). Flarestar disseminates all of its observational data, research and discoveries to established institutions and academic journals dedicated to professional scientific research.  
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The observatory actively engages in photometric research endeavors encompassing various celestial objects, including minor planets, cataclysmic variable stars, microlensing events and exoplanets. These pursuits form a substantial component of the observational program, fostering regular collaboration with professional and independent researchers globally through collaborative campaigns. 
Flarestar also actively participates in the identification of new variable stars and has successfully detected 12 previously unknown variable stars. The first discovery occurred on December 6, 2015, unveiling a new 16th magnitude eclipsing variable star in the constellation Perseus. The comprehensive list of discoveries made by Flarestar Observatory is accessible here.

A historic milestone for Flarestar involved the first-ever asteroid international photometric collaboration that was performed with Thornton Observatory - USA (MPC Code: 713) in the year 2000. The objective of this collaboration was to overcome the 24-hour commensurability of the Earth’s rotation. This collaboration has set a precedent for professional and amateur observatories worldwide.
​Flarestar's main instrument is a Meade 0.25-m aperture f/6.3 Schmidt-Cassegrain Telescope (SCT) that is permanently housed in an automated run-off roof observatory. The telescope is mounted on a EQ8 PRO German equatorial mount where all equipment is controlled and programmed remotely. Further details of the equipment used can be found in the Observatory Page here.

Flarestar's Targets of Interest

  • Variable Stars
  • Asteroids
  • Micro-Lensing
  • Binary Stars
  • Exoplanets
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Variable stars are stars whose brightness changes over time. This can be caused by intrinsic factors, such as pulsations or explosions, or by extrinsic factors, such as eclipses or dust clouds. Variable stars are classified into different types based on their light curves, which are graphs that show how their brightness changes with time. Some examples of variable stars are Cepheid variables, which pulsate and are used to measure cosmic distances; eclipsing binaries, which dim when one star passes in front of the other; and novae and supernovae, which are cataclysmic explosions that can outshine entire galaxies. ​
Asteroids are small, rocky objects that orbit the Sun, mostly between the orbits of Mars and Jupiter. They are remnants of the early solar system, and they can provide clues about its formation and evolution. Their brightness changes over time due to their rotation around their own axis. Their rotational periods can help us determine their shape, size, density, composition, orientation, pole, and spin state. They can help us learn about the physical and dynamical characteristics of these objects, and their origin and evolution.
Flarestar is involved frequently contributes to the Asteroid Lightcurve Database (LCDB), which is a catalog of asteroid light curves maintained by the Minor Planet Center (IAU).. The light curve shown here is a graph that shows how the brightness of an asteroid changes with time, as it rotates around its own axis. By analyzing the light curve, astronomers can estimate the rotational period, shape, size, and pole of the asteroid
Micro-lensing events are astronomical phenomena that occur when a massive object, such as a star or a planet, passes in front of a more distant light source, such as another star or a quasar. The gravity of the foreground object bends the light of the background source, creating a magnified and distorted image that can be observed from Earth. Micro-lensing events can reveal the presence and properties of objects that are otherwise too faint or dark to be detected, such as exoplanets, brown dwarfs, black holes, and dark matter.
Binary stars are systems of two stars that orbit around a common center of gravity. They are very common in the Milky Way Galaxy, and they can help us learn about the formation and evolution of stars and the universe. Binary stars vary in brightness because of their orbital motion and their interactions with each other. Depending on the orientation of their orbits, some binary stars can eclipse or transit each other, causing periodic changes in their apparent brightness. These are called eclipsing binaries or photometric binaries. Other binary stars can exchange mass or energy, causing changes in their size, temperature, or luminosity. These are called interacting binaries or cataclysmic variables
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Exoplanets are planets that orbit stars other than the Sun. They are also called extrasolar planets. Exoplanets can have different sizes, shapes, compositions, temperatures, and orbits. Some exoplanets may be similar to Earth and potentially habitable, while others may be very different and hostile to life. 
The transit method is one of the most common and successful ways of finding exoplanets. The transit method works by observing the brightness of a star over time. When an exoplanet passes in front of the star, it blocks some of the star’s light, causing a small dip in the brightness. This is called a transit. By measuring the amount and duration of the dip, astronomers can estimate the size and orbital period of the exoplanet
Satellite  Weather 
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Flarestar's Active Partners


​Authored and co-authored Publications from Flarestar Observatory (Brincat S.M.)

- Discovery [International Variable Star Index]: Discovery of new variable star  -  TYC 1634-394-1 [2023]
​- Paper [Publications of the Astronomical Society of Japan]: 2021 superoutburst of the WZ Sge-type dwarf nova V627 Pegasi lacks an early superhump phase [2023]
- Paper [Minor Planet Bulletin]: Synodic Period Determination of Seven Main-belt Asteroids from Maltese Observatories [2023]
- Paper [Minor Planet Bulletin]: Lightcurve Analysis and Rotation Period for Asteroid 5147 Maruyama [2023]
- Paper [Minor Planet Bulletin]: Lightcurve Analysis of Asteroid 2685 Masursky [2023]
- Paper [The Astrophysical Journal]: ExoClock Project III: 450 exoplanet ephemerids from ground and space observations [2022]
- Paper [Open European Journal on Variable Stars]: A photometric study of the Active EW/RS Binary Star System: GSC 05586-00371 [2022]   
​- Paper [Minor Planet Bulletin]: Collaborative Asteroid Photometry of Six Main-Belt Asteroids [2022]
- Paper [The Variable Star Bulletin]: Analysis of the IW And star ASAS J071404+7004.3 [2022]   
- Paper [The Astrophysical Journal]: Investigating the low-flux states in six Intermediate Polars [2022]   
- Discovery [International Variable Star Index]: Discovery of new variable star  -  Cl Melotte 20 523  in the Alpha Persei Cluster [2022]
- Paper [Minor Planet Bulletin]: Photometric Observations of Main-Belt Asteroids 2229 Mezzarco, 3648 Raffinetti and 3919 Maryanning [2022]  ​
  

Snippets from Flarestar's Activities 

Observational Campaigns

Flarestar's Light Pollution Survey
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A light pollution survey conducted at the observatory's site shows that light pollution is significant at low elevations over the south-eastern horizon. However, despite this setback useful scientific data could still be obtained... Click Here to know more.

Scientific Publications by Flarestar Observatory

Click here to find out all about the scientific publications produced by BSM from Flarestar Observatory. Publications are hosted on the SAO/NASA Astrophysics Data System server. Click Here to access Flarestar's publications or click on the ORCiD logo to access the ORCiD database.