Sternberg State Astronomical Institute

Moscow, Russia

Sternberg State Astronomical Institute

Moscow, Russia

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Pugacheva S.G.,Sternberg State Astronomical Institute | Feoktistova E.A.,Sternberg State Astronomical Institute | Shevchenko V.V.,Sternberg State Astronomical Institute
Earth, Moon and Planets | Year: 2016

The present paper attempts to assess the characteristics of the impactor that formed the Shackleton crater, located at the south pole of the Moon. The crater’s morphometric parameters were analyzed based on the data of the Lunar Orbiter Laser Altimeter aboard the Lunar Reconnaissance Orbiter. Conclusions were drawn regarding the possible range of the impact angle and the parameters of the transient crater, such as depth and volume. The thickness of ejecta deposits on the transient crater rim and the volume of these deposits at a certain distance from the crater rim were assessed. These assessments enabled determining the type and characteristics of impactors (velocity, density, size, and impact angle) that could have formed the Shackleton crater. It was shown that the Shackleton crater could have been formed by an impact of a low-velocity (3 km/s) comets with diameter 4–4.5 km, chondrite or achondrite with a diameter of 2 km at a 45°–50° angle, whose velocity did not exceed 6 km/s, as well as stony–iron or iron–nickel impactors with a 1–2 km diameter for stony–iron asteroids and 1–1.5 km for iron–nickel asteroids. The impact velocity of stony–iron impactors, according to the authors’ calculations, can reach 12 km/s. The impact velocities of iron–nickel asteroids range from 6 to 9 km/s. The impactor’s substance mass that could have remained in the crater after it was formed was assessed. © 2016 Springer Science+Business Media Dordrecht


Gusev A.V.,Sternberg State Astronomical Institute | Tsybankov I.V.,Sternberg State Astronomical Institute
Moscow University Physics Bulletin | Year: 2011

The statistical problem of the synthesis of a digital processing algorithm for the output signal of the Snail resonant gravitational antenna by analog prototype is considered. The discretization step in the ADC-DAC system is selected on the basis of the Kotelnikov theorem (a sampling theorem) for quasi-harmonic signals. © 2011 Allerton Press, Inc.


Shevchenko V.V.,Sternberg State Astronomical Institute | Pinet P.C.,Observatory Midi Pyrines | Shevrel S.D.,Observatory Midi Pyrines | Dadu Y.,Observatory Midi Pyrines | And 4 more authors.
Solar System Research | Year: 2012

Slope movements of material in lunar craters are investigated based on remote spectral studies carried out on board the Clementine spacecraft, and data obtained during the large-scale survey on board the LRO (Lunar Reconnaissance Orbit) spacecraft. The morphological analysis of crater forms based on large-scale images and spectral and spectropolarized assessments of the exposition age (or maturity) of the slope material has led to the conclusion that the formation process of observed outcrops probably is a modern feature. The lower age limit of these structures is estimated at 40-80 years. Thus, slope movements of surface materials can continue at the present time, regardless of the age of the crater studied. Slope movements of crushed granular material lead to fresh outcrops of subsurface layers of marine or continental landscapes and, therefore, extend our capabilities to research the deep material of the Moon. To analyze this phenomenon, craters of 16 and 30 km have been selected. The length of fresh outcrops, while depending strongly on the dimensions of the craters, can be up to several kilometers. In connection with this, the prospect appears of remote analysis of rocks that came to the surface from depths of at least several hundred meters. In this case, there are openings for the contact analysis of subsurface material without the use of labor-intensive operations associated with the delivery of equipment for deep drilling to the lunar surface. © 2012 Pleiades Publishing, Ltd.


Gusev A.V.,Sternberg State Astronomical Institute | Rudenko V.N.,Sternberg State Astronomical Institute
Measurement Techniques | Year: 2010

The lower bound of the probability of incorrect solutions in the statistical problem of recognition of gravitational and pseudo-gravitational signals at the output of a resonant gravitational antenna is calculated. The additive noise in the individual channels of the antenna array is assumed to be Gaussian. © 2010 Springer Science+Business Media, Inc.


Gusev A.V.,Sternberg State Astronomical Institute | Rudenko V.N.,Sternberg State Astronomical Institute | Yudin I.S.,Sternberg State Astronomical Institute
Gravitation and Cosmology | Year: 2012

We suggest a method of detection of quasistatic geophysical signals with long-base gravitational-wave laser interferometric antennas, alternative to the "free spectrum range" regime, under optimal alignment of the optical system. © 2012 Pleiades Publishing, Ltd.


Kuzin S.V.,Sternberg State Astronomical Institute | Zhitnik I.A.,Sternberg State Astronomical Institute | Shestov S.V.,Sternberg State Astronomical Institute | Bogachev S.A.,Sternberg State Astronomical Institute | And 15 more authors.
Solar System Research | Year: 2011

On February 26, 2009, the first data was obtained in the TESIS experiment on the research of the solar corona using imaging spectroscopy. The TESIS is a part of the scientific equipment of the CORONAS-PHO-TON spacecraft and is designed for imaging the solar corona in soft X-ray and extreme ultraviolet regions of the spectrum with high spatial, spectral, and temporal resolutions at altitudes from the transition region to three solar radii. The article describes the main characteristics of the instrumentation, management features, and operation modes. © 2011 Pleiades Publishing, Ltd.


Gusev A.V.,Sternberg State Astronomical Institute | Rudenko V.N.,Sternberg State Astronomical Institute | Yudin I.S.,Sternberg State Astronomical Institute
Gravitation and Cosmology | Year: 2013

We consider the role of an additional mirror (recycling) in the design of long-base gravitational wave laser interferometers for the detection of weak infra-low-frequency geophysical signals by the resonance method © 2013 Pleiades Publishing, Ltd.


Lukyanov L.G.,Sternberg State Astronomical Institute
Solar System Research | Year: 2011

The convergence of Lagrange series is studied on a part of the elliptical orbit for values of eccentricity exceeding the Laplace limit. The regions in the vicinity of the two apses of the orbit are identified in which the Lagrange series converge absolutely and uniformly for the values of the eccentricity greater than the Laplace limit. The obtained results are of practical interest for astronomy when studying motions of stellar bodies in orbits with high eccentricity. In particular, these series may be used to calculate the orbits of comets or asteroids with high eccentricity as they pass through the neighborhood of perihelion or to calculate the orbits of artificial satellites with high eccentricity "hanging" in the vicinity of apogee. In stellar dynamics, these series may be used in cases of close binary stars, many of which move in orbits with an eccentricity greater than the Laplace limit. © 2011 Pleiades Publishing, Ltd.


Emelyanov N.V.,Sternberg State Astronomical Institute | Andreev M.V.,Russian Academy of Sciences | Berezhnoi A.A.,Sternberg State Astronomical Institute | Bekhteva A.S.,Russian Academy of Sciences | And 21 more authors.
Solar System Research | Year: 2011

In 2009, in five Russian observatories photometric observations of Jupiter's Galilean satellites during their mutual occultations and eclipses were carried out. Based on these observations, an original method was used to ascertain astrometric results such as the difference between the coordinates of pairs of satellites. Fifty-three phenomena were successfully observed. A total of 94 light curves of satellites were measured. The error in the coordinates of satellites due to random errors in photometry, calculated on all data obtained, was 0.041″ in right ascension and 0.046″ in declination. The discrepancies between the theory and observations in these coordinates was found to be 0.060″ and 0.057″, respectively. The results were uploaded to the common database for all observations of natural satellites of planets at the Natural Satellites Data Center (NSDC), which is available online athttp://www. sai. msu. ru/neb/nss/index. htm.http://www. sai. msu. ru/neb/nss/index. htm.For twhich is available online me in the practice of photometric observations of satellites in epochs of mutual occultations and eclipses a new method of observation was tested, which eliminates from astrometric results the major systematic errors caused by an inaccurate account of the background level. The tests were conducted in the Terskol Observatory and the observatory of the Crimean laboratory of the Sternberg State Astronomical Institute of the Moscow State University. The application of the new method showed that the elimination of the background level at these observatories was carried out correctly. © 2011 Pleiades Publishing, Ltd.

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