The Photometric Brightness Variation of Geostationary Orbit Satellite

Abstract

Photometric observation is one of the most effective techniques for determining the physical characteristics of unknown space objects and space debris. In this research, we examine the change in brightness of the Communication, Ocean, Meteorological Satellite-1 (COMS-1) Geostationary Orbit Satellite (GEO), and compare it to our estimate model. First, we calculate the maximum brightness time using our calculation method and then derive the light curve shape using our rendering model. The maximum brightness is then calculated using the induced equation from Pogson's formula. For a comparison with our estimation, we carried out photometric observation using an optical telescope. The variation in brightness and the shape of the light curve are similar to the calculations achieved using our model, but the maximum brightness shows a slightly different value from our calculation result depending on the input parameters. This paper examines the photometric phenomenon of the variation in brightness of a GEO satellite, and the implementation of our approach to understanding the characteristics of space objects.

Analysis of the angle-only orbit determination for optical tracking strategy of Korea GEO satellite, COMS

“…Seo et al (2013) showed that the apparent magnitude of the COMS varied between 12 and 16. Additionally, taking into consideration that the average apparent magnitude of the 66 geostationary satellites that are observable from the Korean peninsula is approximately 11, the COMS is a relatively faint satellite.…”

Short timescale imaging polarimetry of geostationary satellite Thor-6: The nature of micro-glints

“…In principle, the problem can be reversed, and the satellite's orientation and physical parameters of reflection can be empirically determined from well-sampled multi-colour polarimetric lightcurves (polarisation degree and angle), assuming some basic shape properties and geometry (aided by lightcurve analysis, e.g. Seo et al, 2013) as priors, by fitting a Mueller matrix chain (describing the optical action of each reflecting element) directly onto the total observed wavelengthdependent polarisation as a function of angle. This is a method frequently used in calibration and design of optical telescopes and instruments, where we can fit for the orientation and indices of refraction of reflecting surfaces as free parameters in the components of the Mueller matrix chain made up of all optical components (see e.g.…”

Physical Characteristics of Small Space Objects at High Orbits Based on Optical Methods

“…In addition, because different satellites have different brightnesses, optical photometric observations provide information about a satellite's position, attitude and material properties (Jah & Madler 2007;Hall 2010). Moreover, optical observation is an important method for empirical interpretation and determining the shapes of asteroids (Schildknecht et al 2008;Seo et al 2013). Optical surveys primarily provide statistical information about the environment, including rough characterization of the orbits and brightnesses (magnitude, unit: [ m ]) of objects.…”