Comet Oterma 1943 a: A Minor Planet?

1943 ◽  
Vol 55 ◽  
pp. 233
Author(s):  
George H. Herbig ◽  
Delia F. Mcmullin
Keyword(s):  
1990 ◽  
Vol 141 ◽  
pp. 329-336
Author(s):  
B. Morando ◽  
A. Bec-Borsenberger

The observation of minor planets by Hipparcos offers the opportunity to obtain high precision positions for some minor planets. About fifty minor planets are on the programme. Their ephemerides had to be improved in order to reach a precision of 1 arsec and occultations by the Earth and the Moon had to be predicted.From the position of a minor planet on reference great circles at different times better values of the initial position and velocity will be deduced but the reduction of the observations of the minor planets have to take into account the displacement of the photocentre relative to the centre which is due to the shape, the phase effect and the scattering properties of the surface. For some very small planets considered as star like this diplacement will be small and the precise positions obtained will allow to position the dynamical reference system relative to the Hipparcos system. For the bigger minor planets the observations by Hipparcos may give informations on the shape and scattering properties of the surface.


2020 ◽  
Author(s):  
Nick Sioulas

<p>NOAK Observatory, Stavraki (IAU code L02) Ioannina, Greece ([email protected])</p> <p><strong>Introduction</strong></p> <p>In this work, the astrometric observations of four asteroids will be presented which took place on 2019 from NOAK observatory located at Stavraki in Greece. The results and the procedure of submitting the measurements to MinorPlanetCenter will be discussed.</p> <p><strong>Abstract</strong></p> <p>Astrometry is the measurement of positions, parallaxes and proper motion of an astronomical body. Especially the astrometry of Near Earth Objects (NEO) demands great accuracy and the cooperation between the professional and amateur astronomers for better results. All these objects that need confirmation are listed in the Near Earth Object Confirmation Page (NEOCP) and in the Possible Comet Confirmation Page (PCCP) at the site of the Minor Planet Center (MPC). When an object is confirmed, then a Minor Planet Electronic Circular (MPES) is published, including observations, the observers details and the orbital elements of the object. Due to the high number of the objects that need confirmation is important to use all available telescopes to track them.</p> <p>My amateur observatory participates in the effort to record all these objects in the Solar System. The Observatory also conducts observations of various objects and other phenomena such as exoplanet transits contributing to the Ariel Space Mission with the Exoclock Project. However, the main goal of the observatory is to conduct asteroid and comet photometry and the methods, observations and results will be discussed in this presentation.</p> <p>The observatory is registered in IAU as L02, «NOAK Observatory, Stavraki», in the town of Ioannina, Greece.</p> <p><strong>Acknowledgements</strong></p> <p>I would like to thank Anastasia Kokori and Angelos Tsiaras for encouraging me to publish my work and for their advice. </p> <p><strong>References </strong></p> <p>[1] Minor Planet Center: https://www.minorplanetcenter.net/</p> <p>[2] Astrometrica: http://www.astrometrica.at/</p> <p>[3] Roger Dymock: Asteroids and Dwarf Planets</p> <p>[4] Brian D. Warner: A Practical Guide to Lightcurve Photometry and Analysis</p> <p>[5] Project Pluto: https://www.projectpluto.com/</p> <p>[6] NEODyS-2: https://newton.spacedys.com/</p> <p>[7] Center for Near Earth Objects Studies: https://cneos.jpl.nasa.gov/</p>


2022 ◽  
Vol 6 (1) ◽  
pp. 10
Author(s):  
Tom Seccull

Abstract The Jupiter Trojan asteroid 128383 (2004 JW52) was recently reported to have optical colors that are incongruous with its dynamical class. New and archival observations show that this is not the case. This is a reminder that we must always rule out the possibility that the Point-Spread Function of a minor planet is blended with that of a background sidereal source in survey images before its colors in the associated survey catalog can be considered reliable.


1991 ◽  
Vol 127 ◽  
pp. 299-302
Author(s):  
W.Z. Ma

AbstractThis article presents a new method for observing minor planets. The observation is operated with a photo–electronic imaging devise CCD and a lower latitude meridian circle.The CCD is mainly used except it is during the favourable opposition of the minor planet when the meridian circle is mainly used in this method. The method can improve precision of observation of planetary position and enlarge scope of observation of planetary orbit. Therefore, the measured precision of zero point of stellar coordinate could be increased. The key of succeeding is that more precise result is got using the CCD.The experiment in this article indicates that this method is a good way:While a minor planet and calibration stars locate in the same image of the CCD, the measured precisions of the minor plant areσα = ±0″.03, σ´ ±0″.035;While the minor planet and calibration stars are located in different images of the CCD, the precisions areσα = ±0″.06, σδ = ±0″.08.


1872 ◽  
Vol 32 (9) ◽  
pp. 364-364
Author(s):  
M. Prosper-Henry
Keyword(s):  

Nature ◽  
1977 ◽  
Vol 270 (5637) ◽  
pp. 506-507 ◽  
Author(s):  
TAKAFUMI MATSUI ◽  
HITOSHI MIZUTANI
Keyword(s):  

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