Results 41 to 50 of about 1,052,795 (334)
Vestnik Samarskogo Gosudarstvennogo Tehničeskogo Universiteta. Seriâ: Fiziko-Matematičeskie Nauki, 2008 : The choice of Adams methods with divided differences has been validated for solving of the equations of motion of small bodies of the Solar system. The numerical integration with a variable step size of differential equations of motion of the asteroid ...
V. V. Abramov
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Constraining planet formation around 6$M_{\odot}$-8$M_{\odot}$ stars [PDF]
, 2020 Identifying planets around O-type and B-type stars is inherently difficult; the most massive known planet host has a mass of only about $3M_{\odot}$. However, planetary systems which survive the transformation of their host stars into white dwarfs can be detected via photospheric trace metals, circumstellar dusty and gaseous discs, and transits of ...
arxiv +1 more source
CHEMICAL ABUNDANCES IN THE EXTERNALLY POLLUTED WHITE DWARF GD 40: EVIDENCE OF A ROCKY EXTRASOLAR MINOR PLANET [PDF]
, 2009 We present Keck/High Resolution Echelle Spectrometer data with model atmosphere analysis of the helium-dominated polluted white dwarf GD 40, in which we measure atmospheric abundances relative to helium of nine elements: H, O, Mg, Si, Ca, Ti, Cr, Mn, and
B. Klein +5 more
semanticscholar +1 more source
Asteroid phase curves from Lowell observatory photometric database
Atti della Accademia Peloritana dei Pericolanti : Classe di Scienze Fisiche, Matematiche e Naturali, 2011 We present results obtained from processing large photometric data base. We make use of low-precision (generally rounded to 0.1 mag) and low-accuracy (rms magnitude uncertainties of ±0.2 to 0.3 mag) data obtained from the Minor Planet Center and modified
D. A. Oszkiewicz +6 more
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DIGITAL ARCHIVE OF UKRVO: THE POSITIONAL ACCURACY OF MINOR PLANETS DETERMINATIONS
Odessa Astronomical Publications, 2013 Scanning and astrometric processing of two 30x30 cm photographic plates with images of minor planets were conducted. The plates were obtained at the double wide-angle astrograph (DWAA, 400/2000) on the program of photographic sky survey and the program ...
V. Golovnya, V. Andruk
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Post-main-sequence evolution of icy minor planets. III. water retention in dwarf planets and exo-moons and implications for white dwarf pollution [PDF]
, 2017 Studies suggest that the pollution of white dwarf (WD) atmospheres arises from the accretion of minor planets, but the exact properties of polluting material, and in particular the evidence for water in some cases are not yet understood. Previous works studied the water retention in minor planets around main-sequence and evolving host stars, in order ...
arxiv +1 more source
The Statistical Analysis of Exoplanet and Host Stars Based on Multi-Satellite Data Observations
UniverseIn recent years, the rapid development of exoplanet research has provided us with an opportunity to better understand planetary systems in the universe and to search for signs of life.
Yanke Tang +7 more
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Constraints on Evolutionary Timescales for M Dwarf Planets from Dynamical Stability Arguments
The Astrophysical Journal, 2023 The diversity of dynamical conditions among exoplanets is now well established. Yet, the relevance of orbital dynamical timescales to biological evolutionary timescales is poorly understood.
Katie Teixeira, Sarah Ballard
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ASTEROIDS EXPLORATION WITH BALDONE SCHMIDT TELE-SCOPE
Odessa Astronomical Publications, 2018 CCD observations of asteroids were ob-tained in 2008 with the Baldone Schmidt telescope (aper-ture/diameter/focal length = 80/120/240 cm) at the Bal-done Astrophysical observatory (code 069) of the Institute of Astronomy of the University of Latvia.
I. Eglitis
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Determination of Orbital Elements and Ephemerides using the Geocentric Laplace’s Method
Journal of Astronomy and Space Sciences, 2020 This paper presents a methodology for Initial Orbit Determination (IOD) based on a modification of the Laplace’s geocentric method. The orbital elements for Near-Earth asteroids (1864) Daedalus, 2003 GW, 2019 JA8, a Hungaria-type asteroid (4690 ...
Daniela Espitia +2 more
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