Flarestar Observatory located at the island of Malta, holds the International Astronomical Union/Minor Planet Center (IAU/MPC) Observatory Code: 171. This privately-owned observatory is dedicated to conducting high-precision photometric studies of variable stars and asteroids, with an emphasis on contributing to academic research and scientific literature. Its primary research areas include photometric analysis of minor planets, cataclysmic variable stars, microlensing events, and exoplanets. Most of the work is carried out in collaboration with a global network of professional and independent researchers. Flarestar Observatory is managed by||Stephen|M.||Brincat|.

Established in 1986, the observatory began with modest equipment housed in a small structure. Over the years, significant upgrades have been implemented to enhance its capabilities. In 2000, the observatory conducted an asteroid photometric collaboration with an observatory in the United States (MPC Code: 713), addressing the challenges posed by the Earth's rotational period. This pioneering effort marked the first instance of a coordinated photometric study across international observatories, a practice that has now become routine to many asteroid studies. Flarestar observatory has also contributed to the scientific community through several research publications.
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​The observatory's primary instrument is a robotic 0.25-meter aperture f/6.3 Schmidt-Cassegrain Telescope (SCT), housed within an automated run-off roof observatory. This telescope is adeptly configured to provide optimal photometric observations. For more detailed information regarding the observatory's equipment, please refer to the Observatory Page.

Targets of Interest

  • Variable Stars
  • Asteroids
  • Micro-Lensing
  • Binary Stars
  • Exoplanets
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Variable stars, which are stars whose brightness varies over time, account for a significant portion of the telescope time at Flarestar. The causes of these variations can be intrinsic, such as pulsations or explosions, or extrinsic, such as eclipses or dust clouds. Different types of variable stars are distinguished by their light curves, which are graphs that plot their brightness against time. Some examples of variable stars are Cepheid variables, which are pulsating stars that serve as cosmic distance indicators; eclipsing binaries, which are pairs of stars that obscure each other periodically; and novae and supernovae, which for the latter are violent explosions that can briefly outshine entire galaxies.​
A light curve, representing brightness variation over time, of the flare star EV Lac, obtained from Flarestar Observatory during approximately nine hours of observation. The two peaks in the graph indicate the occurrence of two distinct flaring events.
[Left Image]: A computer-generated depiction of a flare star undergoing an outburst.
Asteroids are remnants of the early solar system that orbit the Sun, mostly in the region between Mars and Jupiter. They are small, rocky bodies that can reveal insights into the formation and evolution of the solar system. As they rotate around their own axis, their brightness varies over time. Their rotational periods can inform us about their shape, density, composition, orientation, pole, and spin state, which are important for understanding their physical and dynamical properties, their origin and evolution. The observation of these objects occupies a significant part of the observational program at Flarestar Observatory. In this field, collaborational work has been conducted with several professional and amateur observatories across the globe.  The graph displayed here is a light curve that plots the brightness of an asteroid against time, as it rotates around its own axis. The analysis of the data of such light curves allow us to determine the asteroids' rotational period.
Flarestar light curve (graph) of the main-belt asteroid Palisana depicting brightness variations as it rotates on its axis over a period of around 8.7 hours. 
Micro-lensing events, characterized as rare and transient phenomena, occur when a massive foreground object, like a star or a planet, functions as a gravitational lens for a more distant background light source, such as another star or potentially an exoplanet. The gravitational influence of the foreground object bends and intensifies the light from the background source, leading to a noticeable increase in brightness observable from Earth. These events are pivotal in revealing the existence and properties of typically invisible or faint objects, including exoplanets, brown dwarfs, and black holes.
In this realm of study, Flarestar Observatory collaborates with Dr. Lukasz Wyrzykowski from the University of Warsaw. The observatory is a recognized body that forwards its observations of micro-lensing events to the Gaia Satellite Working Group GW-10. This group comprises astronomers who utilize data from the Gaia satellite to delve into micro-lensing events and their broader astrophysical implications.
Image Source; NASA/ JPL-Caltech; /Warsaw University Observatory
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. Flarestar has discovered several new variable stars where a number of these are binary star systems.
The graph above illustrates the light curve of a binary variable star discovered at Flarestar Observatory. The observed variations in brightness result from the stars periodically eclipsing each other
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. A number of exoplanet transits have been observed from Flarestar Observatory and reported to the ExoClock Project where this transit data will be used for the upcoming Ariel Satellite Mission.
Light curve of a transit event of exoplanet TRes-3b as observed from Flarestar Observatory.

Flarestar's numbers in a nutshell

Photometric Observations (Var. Stars):     203765
Asteroid Rotational Periods (MPB):             131
New Variable Stars Discovered:                  12
Visual Variable Star Obs. (AAVSO):             7398
Photometric Obs. to OPTICON Alliance:     2450
Supernovae Search Observations:             3317 
​Recorded Exoplanet Transits:                     22
Other observations (incl. astrometric):     92625​​
Flarestar actively collaborates with the following institutions, providing its observational findings as a committed research partner.

Recent authored and co-authored publications

The scientific papers displayed here represent publications from 2024/2025. A complete list of over 80 scientific papers can be accessed through the links provided below. Click on the ADS or ORCiD items to access all the scientific publications co-authored and authored by Brincat S.M. from Flarestar Observatory.
https://orcid.org/0000-0002-9205-5329
  • [Minor Planet Bulletin] Photometric Observations and Lightcurve Analysis of Five Main-Belt Asteroids From Six Observatories [2026] 
  • [Advances in Space Research] The Power of Collaborative Optical Techniques in Asteroid Studies: A Closer Look at the Koronis Asteroids [2026]
  • [Open European Journal of Variable Stars] BY Draconis Stars in Two Galactic Clusters: Exploring the Rotation and Cyclical Variability of the Brighter Members [2025] 
  • [The Astronomical Journal] Exoclock project IV: A homogeneous catalogue of 620 updated exoplanet ephemerides [2025]
  • [MRAS] TESS and ground-based observations of WZ Sge-type dwarf novae in outburst [2025]
  • [Minor Planet Bulletin] Rotation Period of 4163 Saaremaa  [2025] 
  • [Astronomy & Astrophysics]  AT2021uey: A planetary microlensing event outside the Galactic bulge  [2025]
  • [Minor Planet Bulletin] Rotation Period of 5295 Masayo  [2025]
  • [MNRAS]  Is the Symbiotic Recurrent Nova T CrB Late? Recent Photometric Evolution and Comparison with Past Pre-Outburst Behavior [2025]​
  • [Minor Planet Bulletin] Observations of Mutual Events between 617 Patroclus and Menoetius on September 25, October 6 and October 23, 2024 [2025]
  • [Astronomy & Astrophysics] Constraining Lens Masses in Moderately to Highly Magnified Microlensing Events from Gaia [2025] 
  • [Minor Planet Bulletin] Lightcurve and Rotation Period of 1367 Nongoma [2025]
  • [Minor Planet Bulletin] Photometric Observations and Analysis of Seven Asteroids [2025]
  • [Astronomy & Astrophysics] GOTO065054+593624: a 8.5 mag amplitude dwarf nova identified in real time via Kilonova Seekers [2025] ​
  

Poster Papers & Infographics

Flarestar's Light Pollution Survey​

Flarestar's Weather
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This polar light pollution map shows the sky above Flarestar Observatory, with the zenith at the center and the edge 20° above the horizon. Red dots indicate SQM measurements.
Despite notable pollution near the southeastern horizon, the observatory continues to gather valuable data. [Copyright - Flarestar Observatory, 2024].