A5087398820- Stellar, planetary, and galactic studies
- Astronomical Observations and Instrumentation
- Astro and Planetary Science
- Astronomy and Astrophysical Research
- Planetary Science and Exploration
- Astrophysics and Star Formation Studies
- Solar and Space Plasma Dynamics
- History and Developments in Astronomy
- Calibration and Measurement Techniques
- Space Exploration and Technology
- Geophysics and Gravity Measurements
- Astronomical and nuclear sciences
- Adaptive optics and wavefront sensing
- Gamma-ray bursts and supernovae
- Isotope Analysis in Ecology
- Atmospheric Ozone and Climate
- Historical Astronomy and Related Studies
- Astrophysical Phenomena and Observations
- Inertial Sensor and Navigation
- Field-Flow Fractionation Techniques
- Aerospace Engineering and Control Systems
- CCD and CMOS Imaging Sensors
- Advanced Research in Science and Engineering
- Currency Recognition and Detection
- Geomagnetism and Paleomagnetism Studies
Institute of Applied Astronomy
2024
Pulkovo Observatory
2015-2024
Russian Academy of Sciences
2008-2015
Astronomical Observatory
2011
During the 2014–2015 mutual events season, Institut de Mécanique Céleste et Calcul des Éphémérides (IMCCE), Paris, France, and Sternberg Astronomical Institute (SAI), Moscow, Russia, led an international observation campaign to record ground-based photometric observations of Galilean moon occultations eclipses. We focused on processing complete data base compute new accurate astrometric positions. used our method derive positions from light curves events. developed model eclipses, while...
The F3 main sequence star KIC 8462852 (Boyajian's Star) showed deep (up to 20%) day-long brightness dips of unknown cause during the 4 years Kepler mission. A 0.164 mag (16%) dimming between 1890 and 1990 was claimed, based on analysis photographic plates from Harvard Observatory. We have gathered an independent set historic Sonneberg Observatory, Germany, covering 1934-1995. With 861 magnitudes in B, 397 V, we find be constant within 0.03 per century (3%). Consistent outcomes are found...
Abstract We present the orbit and mass estimates for components of visual binary star 61 Cyg obtained with positional observations, including high‐precision Gaia data, measurements differences in radial velocities accelerations components. Since orbital period this significantly exceeds using allows us to reduce uncertainty determination elements total system.
Context. In 2003, the Sun and Earth passed through both equatorial plane of Jupiter therefore orbital planes its main satellites.
The trigonometric parallaxes of 71 stars with large proper motion were determined the 26-inch refractor at Pulkovo Observatory. Relative targets derived using three or four separate series observations (three pointings over 1.5 2 years for each one). Observations performed period 2007–2011. We used from 5 to 20 reference per field. applied a correction relative absolute parallax based on photometric stars. latter estimated infrared colours (J − Ks) and reduced motions stars, simulated...
We report the final results of 1997 campaign photometric observations mutual phenomena Galilean satellites carried out at observatories in Kazakhstan, Russia, and Ukraine. Our contribute substantially to world data bank such will allow model motion be further refined. To facilitate use data, we reduced them by computing planetocentric rectangular coordinate differences satellite pairs for a number instants time so deduce one instant from observed light curve. It is these that constitute...
Abstract We present 18,365 astrometric observations of 290 visual binaries obtained with the 26‐inch refractor Pulkovo Observatory during 2014–2019. The separation between components is from 1″.3 to 37″ a median value 4″.8 . For single observation, mean error 0″.013 , and position angle 0 ∘ .44/ ρ where an angular distance in arcseconds. compare sample stars data Gaia DR2 catalog results ground‐based performed other telescopes.
Two methods of determining the orbit a wide binary star are compared. The Apparent Motion Parameters (AMP) method is applicable to limited number stars, since it requires use not only positional observations stars in sky plane, but also additional data on radial velocities, parallaxes and masses stars. Thiele-Innes gives reliable result if arc large enough for cover different phases relative positions components orbit. We considered 96 orbits calculated by AMP 825 method. As result, obtained...