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Journal articles on the topic 'Minor planets, asteroids: general'

Author: Grafiati

Published: 4 June 2021

Last updated: 16 February 2022

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1

A’Hearn, M., L. Kresak, and J. Rahe. "Commission No. 15: Physical Study of Comets, Minor Planets and Meteorites (Etude Physique des Cometes, des Petites Planetes et des Meteorites)." Transactions of the International Astronomical Union 20, no. 2 (1988): 175–83. http://dx.doi.org/10.1017/s0251107x00016230.

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Tribute is paid to those members of Commission 15 who have passed away since the last General Assembly: Dr. Ludwig BIERMANN, Dr. Nicholas BOBROVNIKOFF, Dr. Richard Heinrich GIESE, Dr. Marie-Therese MARTEL, Dr. Reginald WATERFIELD.The Commission had one Business Session, two Science Sessions on “News in Cometary Research” (organized by C. Arpigny), one Science Session on “News in Minor Planet Research” (organized by A.W. Harris), a Joint Discussion with Commission 20 on “Major Observing Programs and Data Bases” (organized by Y. Kozai and L. Kresak), and a Joint Discussion with Commission 22 on

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Mochi, Maddalena, and Giacomo Tommei. "New Tools for the Optimized Follow-Up of Imminent Impactors." Universe 7, no. 1 (2021): 10. http://dx.doi.org/10.3390/universe7010010.

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The solar system is populated with, other than planets, a wide variety of minor bodies, the majority of which are represented by asteroids. Most of their orbits are comprised of those between Mars and Jupiter, thus forming a population named Main Belt. However, some asteroids can run on trajectories that come close to, or even intersect, the orbit of the Earth. These objects are known as Near Earth Asteroids (NEAs) or Near Earth Objects (NEOs) and may entail a risk of collision with our planet. Predicting the occurrence of such collisions as early as possible is the task of Impact Monitoring (

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3

IORIO, L. "EFFECTS OF STANDARD AND MODIFIED GRAVITY ON INTERPLANETARY RANGES." International Journal of Modern Physics D 20, no. 02 (2011): 181–232. http://dx.doi.org/10.1142/s0218271811018780.

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We numerically investigate the impact on the two-body range of several Newtonian and non-Newtonian dynamical effects for some Earth-planet (Mercury, Venus, Mars, Jupiter, Saturn) pairs, in view of the expected cm-level accuracy in some future planned or proposed interplanetary ranging operations. The general relativistic gravitomagnetic Lense–Thirring effect should be modeled and solved for in future accurate ranging tests of Newtonian and post-Newtonian gravity, because it falls within their measurability domain. It could a priori "imprint" the determination of some of the target parameters o

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4

Tichá, J., M. Tichý, and Z. Moravec. "Brief summary of Kleť photographic search programme for minor planets." International Astronomical Union Colloquium 173 (1999): 189–92. http://dx.doi.org/10.1017/s0252921100031419.

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AbstractA long-term photographic search programme for minor planets was begun at the Kleť Observatory at the end of seventies using a 0.63-m Maksutov telescope, but with insufficient respect for long-arc follow-up astrometry. More than two thousand provisional designations were given to new Kleť discoveries. Since 1993 targeted follow-up astrometry of Kleť candidates has been performed with a 0.57-m reflector equipped with a CCD camera, and reliable orbits for many previous Kleť discoveries have been determined. The photographic programme results in more than 350 numbered minor planets credite

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5

Chapman, C. R., L. Kresak, B. D. Donn, et al. "Commission 15: Physical Study of Comets, Minor Planets, and Meteorites." Transactions of the International Astronomical Union 19, no. 1 (1985): 167–87. http://dx.doi.org/10.1017/s0251107x00006295.

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The last three years have witnessed a growing interest in the physical properties of the small bodies in the solar system. Perhaps the most significant impetus to research on small bodies has been the imminent arrival of Comet Halley in the inner solar system. This famous comet, which was recovered in autumn 1982, has been the object of intense study during the past year as it has approached the sun and developed a tail. Much of the international, ground-based astronomical research on Halley has been coordinated through the International Halley Watch program. Spacecraft from several nations ha

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Mouret, Serge, D. Hestroffer, and F. Mignard. "Asteroid mass determination with the Gaia mission." Proceedings of the International Astronomical Union 2, S236 (2006): 435–38. http://dx.doi.org/10.1017/s1743921307003535.

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AbstractThe main-belt asteroids are generally considered as the principal source for the near-Earth asteroids (NEAs). The ESA astrometric mission Gaia, due for launch in late 2011, will observe a very large number of asteroids (∼300,000 brighter than V = 20), the majority lying in the main-belt and with an unprecedented positional precision (at the sub-milliarcsecond level). Such high precision astrometry will enable to derive direct measures of the masses of the largest asteroids of which their precise determination will be of utmost significance for the knowledge of physical properties of as

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Chernykh, N. S., and A. G. Sokolsky. "Ita-Crao Minor Planet Survey: Results and Prospects." International Astronomical Union Colloquium 165 (1997): 567–70. http://dx.doi.org/10.1017/s0252921100047138.

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AbstractResults of minor planet observation programme that is made jointly by the Institute of Theoretical Astronomy and the Crimean Astrophysical Observatory during three decades with the Zeiss 40-cm double astrograph at Crimea are presented. Almost all permanently numbered minor planets were observed. A catalogue of astrometrical results obtained in the course of this survey contains more than 60 thousand minor planet positions. Many thousand unnumbered asteroids were discovered, 875 of which had received permanent numbers by June of 1996.In the development of this survey programme we plan t

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8

Bykov, O. P. "On the Accuracy of CCD and Photographic Observations of Asteroids and Their Current Orbit Determinations." Symposium - International Astronomical Union 167 (1995): 351–52. http://dx.doi.org/10.1017/s0074180900056758.

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An application of the Classical Laplacian Method and new Pulkovo AMP-method for current asteroid orbit determinations is given. The CERES software package created at the Institute of Theoretical Astronomy (Russia) was applied to calculate (O-C)-differences for 200 numbered minor planets observed irregularly and quasisimultaneously in 1993 by CCD as well as by photographic techniques at 25 observatories (ESO, SERGA, Kitt Peak etc.). The accuracy of the observations was estimated by means of the standard error of the average (O-C) differences for each type of observation obtained by each telesco

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9

Li, Jian, Zhihong Jeff Xia, and Liyong Zhou. "Calibration of the angular momenta of the minor planets in the solar system." Astronomy & Astrophysics 630 (September 23, 2019): A68. http://dx.doi.org/10.1051/0004-6361/201834196.

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Aims. We aim to determine the relative angle between the total angular momentum of the minor planets and that of the Sun-planets system, and to improve the orientation of the invariable plane of the solar system. Methods. By utilizing physical parameters available in public domain archives, we assigned reasonable masses to 718 041 minor planets throughout the solar system, including near-Earth objects, main belt asteroids, Jupiter trojans, trans-Neptunian objects, scattered-disk objects, and centaurs. Then we combined the orbital data to calibrate the angular momenta of these small bodies, and

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10

García, A. López, Yu D. Medvedev, and J. A. Moraño Fernández. "Using Close Encounters of Minor Planets for the Improvement of their Masses." International Astronomical Union Colloquium 165 (1997): 199–204. http://dx.doi.org/10.1017/s0252921100046558.

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AbstractThe orbits of 6807 numbered minor planets on the time interval 1975–2010 have been integrated. The possibility of determining masses for asteroids with close encounters with each other has been investigated, including several kinds of situations. The importance of the observational time arc, as well as the distribution of observations, for determining the masses are shown. The mass of asteroid (24) Themis from its perturbations on asteroid (2296) Kugultinov, and the mass of (10) Hygiea from its perturbations on (1259) Ógyalla have been determined.

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Pirani, S., A. Johansen, B. Bitsch, A. J. Mustill, and D. Turrini. "Consequences of planetary migration on the minor bodies of the early solar system." Astronomy & Astrophysics 623 (March 2019): A169. http://dx.doi.org/10.1051/0004-6361/201833713.

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Pebble accretion is an efficient mechanism that is able to build up the core of the giant planets within the lifetime of the protoplanetary disc gas-phase. The core grows via this process until the protoplanet reaches its pebble isolation mass and starts to accrete gas. During the growth, the protoplanet undergoes a rapid, large-scale, inward migration due to the interactions with the gaseous protoplanetary disc. In this work, we have investigated how this early migration would have affected the minor body populations in our solar system. In particular, we focus on the Jupiter Trojan asteroids

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Hestroffer, D., and B. Morando. "Solar system objects observed by Hipparcos." Symposium - International Astronomical Union 172 (1996): 437–42. http://dx.doi.org/10.1017/s0074180900127822.

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The ESA satellite Hipparcos provides valuable photometric and astrometric results on minor planets and natural satellites. Observations of 48 asteroids, JII-Europa, S VI-Titan and S VIII-Iapetus were made from November 1989 to March 1993. A twenty seconds averaged normal place is constructed, providing thus positions accurate to a few hundredths of arcseconds and relative to a very precise and homogeneous reference frame.

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13

Fernández, Julio A., Makoto Yoshikawa, Giovanni B. Valsecchi, et al. "COMMISSION 20: POSITIONS AND MOTIONS OF MINOR PLANETS, COMETS AND SATELLITES." Proceedings of the International Astronomical Union 4, T27A (2008): 169–70. http://dx.doi.org/10.1017/s1743921308025428.

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Commission 20 has been involved in the discussion on discovery credit rules of solar system objects (mainly concerned with asteroids) in particular with the role played by dynamicists in recovering objects by linking their orbits with previous apparitions. A working group was set up to discuss the issue that was integrated by professional astronomers as well as amateurs. There was some exchange of opinions and conflicting views, but the trend of the majority was to keep the discovery credit for the discoverer whose observations led to the object's principal designation, as expressed in the MPC

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Banik, Deepayan, Kumar Gaurav, and Ishan Sharma. "Axisymmetric landslides on top-shaped asteroids." EPJ Web of Conferences 249 (2021): 03048. http://dx.doi.org/10.1051/epjconf/202124903048.

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Spin rates of minor planets or asteroids are known to have been affected by several agents including but not limited to tidal fly-bys, impacts and solar radiation. Surface processes like landslides occur as a result of such rotational changes. We study the evolution of landslides on top-shaped rubble pile asteroids like 101955 Bennu and 162173 Ryugu, with the underlying core modeled as two solid cones fused back to back. Using a depth averaged avalanche theory applicable to granular flows we solve for axisymmetric landslides occurring at various spin rates and regolith friction. Static regions

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15

van der Hucht, Karel A. "The IAU and hazardous Near Earth Objects – a clear and present danger." Proceedings of the International Astronomical Union 13, S349 (2018): 79–89. http://dx.doi.org/10.1017/s1743921319000164.

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AbstractThe Minor Planet Center, established in 1947 by the IAU, is the international repository and clearinghouse for the world’s minor planet observations. Since 1989, CCD surveys of Near Earth Objects at ground-based astronomical observatories are operational, mainly in the USA. As of 23 August, 2018, a total of 18,545 Near Earth Asteroids (NEAs) and 107 Near Earth Comets (NECs) have been registered and daily updates are made publicly available on the internet by the MPC, NASA-JPL-CNEOS and ESA-SSA-NEOCC.Concern about the possibility of NEO impacts has been picked up by the United Nations C

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16

Scotti, James V., and Robert Jedicke. "Observation of small solar system objects with spacewatch." Symposium - International Astronomical Union 172 (1996): 389–98. http://dx.doi.org/10.1017/s007418090012772x.

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Since beginning an automated full-time survey for Near-Earth objects in September 1990, the Spacewatch project has discovered 95 new Near-Earth asteroids (NEAs), 3 new comets, and 3 new Centaur asteroids. Spacewatch typically identifies about 2000 main-belt asteroids each lunation while covering about 150 square degrees to a limiting magnitude of Vlim ∼ 20.9. We report automatically measured astrometric asteroid detections to the Minor Planet Center where known and multiply detected objects are identified. NEAs and other interesting objects are identified by their angular rates of motion near

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17

Zappala, Vincenzo, H. Uwe Keller, M. Bailey, et al. "Commission 15: Physical Study of Comets, Minor Planets, and Meteorites (L’Etude Physique des Cometes, des Petites Planetes et des Meteorites)." Transactions of the International Astronomical Union 24, no. 1 (2000): 93–114. http://dx.doi.org/10.1017/s0251107x00002650.

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The present report of Commission 15 has been, as usual, prepared primarily by the chairpersons of the two working groups. E. Tedesco wrote the section about Asteroids and Meteorites, with the assistance of A. Cellino, G. Consolmagno and C.-I. Lagerkvist. W. F. Huebner prepared the section about Comets, with the assistance of J. Benkhoff, H. Boehnhardt, J. Brandt, M. T. Capria, A. Cochran, G. Cremonese, M. Duncan, W. Huntress, H. Levison, and G. P. Tozzi. Moreover, the whole document has been assembled by K. Muinonen, who did the final editing, to merge the two reports and fit the document into

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Kholshevnikov, K. V., and A. S. Shchepalova. "On Distances between Orbits of Planets and Asteroids." Vestnik St. Petersburg University, Mathematics 51, no. 3 (2018): 305–16. http://dx.doi.org/10.3103/s1063454118030044.

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19

Garcia, A. Lopez, J. L. Valdes Navarro, A. Ortiz Gil, et al. "Joint Program for Automatic Analysis of Astrographic Plates." Symposium - International Astronomical Union 166 (1995): 355. http://dx.doi.org/10.1017/s0074180900228386.

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Pulkovo and Valencia observatories are developing measuring machines based on the “Ascorecord” microscope that allow to undertake automatic measuring programs of different kind of plates (Ortiz et al., 1993). All aspects of astrometry work are covered now by our software: field maps and plate files creation from the PPM and the GSC; precise ephemeris calculation of minor planets and comets, including planetary perturbations; image identification and automatic plate measurement and reduction (Lopez et al., 1994a). For these tasks, correction tables for GSC catalogue vs. PPM, systematic errors (

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20

Veras, Dimitri, and Kevin Heng. "The lifetimes of planetary debris discs around white dwarfs." Monthly Notices of the Royal Astronomical Society 496, no. 2 (2020): 2292–308. http://dx.doi.org/10.1093/mnras/staa1632.

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ABSTRACT The lifetime of a planetary disc that orbits a white dwarf represents a crucial input parameter into evolutionary models of that system. Here we apply a purely analytical formalism to estimate lifetimes of the debris phase of these discs, before they are ground down into dust or are subject to sublimation from the white dwarf. We compute maximum lifetimes for three different types of white dwarf discs, formed from (i) radiative YORP break-up of exo-asteroids along the giant branch phases at 2–100 au, (ii) radiation-less spin-up disruption of these minor planets at ${\sim} 1.5\!-\!4.5\

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Marov, Mikhail, and Sergei Ipatov. "Migration Processes and Volatiles Delivery." Symposium - International Astronomical Union 213 (2004): 295–98. http://dx.doi.org/10.1017/s007418090019343x.

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Migration processes of comets and asteroids from the outer regions of the solar system, including the Edgeworth–Kuiper belt, are regarded as important mechanisms for the formation and evolution of the inner planets. These minor bodies may be responsible for the delivery of volatile matter to the inner planets and thus be responsible for the origin of life. We estimate that the cumulative mass of icy comets impacting on the Earth during the formation of the giant planets is similar to the mass of water in the Earth oceans, and that Mars acquired more water per unit planet mass than Earth. We fi

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Szabó, Gy, K. Sárneczky, and L. L. Kiss. "The O–C diagrams of minor planets − a new approach to modelling the rotation." International Astronomical Union Colloquium 173 (1999): 185–88. http://dx.doi.org/10.1017/s0252921100031407.

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AbstractA widely used tool in studying quasi-monoperiodic processes is the O–C diagram. This paper deals with the application of this diagram in minor planet studies. The main difference between our approach and the classical O–C diagram is that we transform the epoch (=time) dependence into the geocentric longitude domain. We outline a rotation modelling using this modified O–C and illustrate the abilities with detailed error analysis. The primary assumption, that the monotonity and the shape of this diagram is (almost) independent of the geometry of the asteroids is discussed and tested. The

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López-García, Francisco, and Adrian Brunini. "Dynamical Behaviour of Asteroids in the 4:1 Resonance." International Astronomical Union Colloquium 172 (1999): 377–78. http://dx.doi.org/10.1017/s0252921100072791.

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We study the dynamics of mean motion resonance with Jupiter in the 4:1 gap using only gravitational methods. This mechanism is capable of explaining this Kirkwood gap in an uniform way (see Ferraz-Mello, 1994; Ferraz-Mello et al., 1994; Moons, 1997; Yoshikawa, 1989). We considered the asteroidal motion in two and three dimensions and we carried out our investigations integrating numerically the full equations of motion and taking into account Mars, Jupiter and Saturn as disturbing planets. The orbital evolution of asteroids was obtained considering the elements variation. The numerical investi

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Devyatkin, A. V., A. P. Kulish, V. V. Kouprianov, et al. "The observations of Near Earth Objects by the automatic mirror astrograph ZA–320M at Pulkovo observatory." Proceedings of the International Astronomical Union 2, S236 (2006): 391–98. http://dx.doi.org/10.1017/s1743921307003481.

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AbstractAt Pulkovo Observatory, we conduct observations of various Solar System bodies: major planets, their satellites, comets, and asteroids, including Near Earth Objects. For these purposes, a robotic telescope was constructed on the base of the ZA–320 Mirror Astrograph (D=320 mm, F=3200 mm). It can perform CCD observations of Solar System bodies with the limiting magnitude of up to 19.0.Independent ephemeris support is provided by the EPOS software package developed at Pulkovo Observatory; it includes tracing of catalogues of comets and asteroids, regular ephemeris calculations, and contro

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Kozai, Yoshihide. "A Mechanism for Asteroids to Avoid Close Approach and Collision to Planets." Highlights of Astronomy 11, no. 1 (1998): 229–32. http://dx.doi.org/10.1017/s1539299600020633.

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AbstractIn this paper it is explained how asteroids with large aphelion distances avoid very close approach to Jupiter. Namely, since for asteroids with resonant mean motions the critical arguments librate as it has been known for many years, and for those with non-resonant mean motions the eccentricities change with the argument of perihelion so the distance to Jupiter cannot be very small.Also some behaviours of Kuiper-belt asteroids are studied by a similar way and it is found that the libration region for the argument of perihelion appears only when the eccentricity is very large. Therefor

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Vieira Neto, E., and O. C. Winter. "Gravitational Capture of Asteroids by Gas Drag." Mathematical Problems in Engineering 2009 (2009): 1–11. http://dx.doi.org/10.1155/2009/897570.

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Several irregular satellites of the giant planets were found in the last years. Their orbital configuration suggests that these satellites were asteroids captured by the planets. The restricted three-body problem can explain the dynamics of the capture, but the capture is temporary. It is necessary some kind of dissipative effect to turn the temporary capture into a permanent one. In this work we study an asteroid suffering a gas drag at an extended atmosphere of a planet to turn a temporary capture into a permanent one. In the primordial Solar System, gas envelopes were created around the pla

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Johansen, Anders, Mordecai-Mark Mac Low, Pedro Lacerda, and Martin Bizzarro. "Growth of asteroids, planetary embryos, and Kuiper belt objects by chondrule accretion." Science Advances 1, no. 3 (2015): e1500109. http://dx.doi.org/10.1126/sciadv.1500109.

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Chondrules are millimeter-sized spherules that dominate primitive meteorites (chondrites) originating from the asteroid belt. The incorporation of chondrules into asteroidal bodies must be an important step in planet formation, but the mechanism is not understood. We show that the main growth of asteroids can result from gas drag–assisted accretion of chondrules. The largest planetesimals of a population with a characteristic radius of 100 km undergo runaway accretion of chondrules within ~3 My, forming planetary embryos up to Mars’s size along with smaller asteroids whose size distribution ma

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Veras, Dimitri, Michael Efroimsky, Valeri V. Makarov, et al. "Orbital relaxation and excitation of planets tidally interacting with white dwarfs." Monthly Notices of the Royal Astronomical Society 486, no. 3 (2019): 3831–48. http://dx.doi.org/10.1093/mnras/stz965.

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Abstract Observational evidence of white dwarf planetary systems is dominated by the remains of exo-asteroids through accreted metals, debris discs, and orbiting planetesimals. However, exo-planets in these systems play crucial roles as perturbing agents, and can themselves be perturbed close to the white dwarf Roche radius. Here, we illustrate a procedure for computing the tidal interaction between a white dwarf and a near-spherical solid planet. This method determines the planet’s inward and/or outward drift, and whether the planet will reach the Roche radius and be destroyed. We avoid const

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29

Sokolov, L. L., I. A. Balyaev, G. A. Kuteeva, N. A. Petrov, and B. B. Eskin. "Approaches and collisions of asteroids with the Moon and planets." Journal of Physics: Conference Series 1959, no. 1 (2021): 012047. http://dx.doi.org/10.1088/1742-6596/1959/1/012047.

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Shuygina, N. V., and E. I. Yagudina. "The FK5 equinox and equator from combined radar and optical data of the near-earth asteroids." Symposium - International Astronomical Union 172 (1996): 469–74. http://dx.doi.org/10.1017/s0074180900127895.

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Minor planets optical observations have long been used for the purpose of establishing a Celestial reference frame. Being in existence since the early 1960s modern high-accuracy radar measurements of the so-called near-Earth asteroids (NEAs) have been widely extended to the orbit determination process and predicting of the next apparition of the asteroid. Even few radar measurements, when added to optical ones, significantly improve asteroid's ephemeris and reduce standard deviations of the orbital elements (Yeomans et al., 1987). The idea to connect optical and radar data in the problem of th

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Veras, Dimitri, Nikolaos Georgakarakos, Alexander J. Mustill, Uri Malamud, Tim Cunningham, and Ian Dobbs-Dixon. "The entry geometry and velocity of planetary debris into the Roche sphere of a white dwarf." Monthly Notices of the Royal Astronomical Society 506, no. 1 (2021): 1148–64. http://dx.doi.org/10.1093/mnras/stab1667.

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ABSTRACT Our knowledge of white dwarf planetary systems predominately arises from the region within a few Solar radii of the white dwarfs, where minor planets breakup, form rings and discs, and accrete on to the star. The entry location, angle, and speed into this Roche sphere has rarely been explored but crucially determines the initial geometry of the debris, accretion rates on to the photosphere, and ultimately the composition of the minor planet. Here, we evolve a total of over 105 asteroids with single-planet N-body simulations across the giant branch and white dwarf stellar evolution pha

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Mochi, Maddalena, and Giacomo Tommei. "New Tools for the Optimized Follow-Up of Imminent Impactors." Universe 7, no. 1 (2021): 10. http://dx.doi.org/10.3390/universe7010010.

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The solar system is populated with, other than planets, a wide variety of minor bodies, the majority of which are represented by asteroids. Most of their orbits are comprised of those between Mars and Jupiter, thus forming a population named Main Belt. However, some asteroids can run on trajectories that come close to, or even intersect, the orbit of the Earth. These objects are known as Near Earth Asteroids (NEAs) or Near Earth Objects (NEOs) and may entail a risk of collision with our planet. Predicting the occurrence of such collisions as early as possible is the task of Impact Monitoring (

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Shevchenko, Ivan I. "On the Lyapunov exponents of the asteroidal motion subject to resonances and encounters." Proceedings of the International Astronomical Union 2, S236 (2006): 15–30. http://dx.doi.org/10.1017/s174392130700302x.

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AbstractIn theoretical as well as practical issues of the asteroidal hazard problem, it is important to be able to assess the degree of predictability of the orbital motion of asteroids. Some asteroids move in a virtually predictable way, others do not. The characteristic time of predictability of any motion is nothing but the Lyapunov time (the reciprocal of the maximum Lyapunov exponent) of the motion. In this report, a method of analytical estimation of the maximum Lyapunov exponents of the orbital motion of asteroids is described in application for two settings of the problem. Namely, the

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Aikman, G. Christopher L., David D. Balam, and Jeremy B. Tatum. "The minor planet (3316) Herzberg." Canadian Journal of Physics 72, no. 11-12 (1994): 743–46. http://dx.doi.org/10.1139/p94-097.

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We describe the history of the minor planet (3316) Herzberg, and present a new precise orbit for the object from all available observations, including new observations of our own obtained specially for the purpose of this commemorative issue, applying perturbations from all the major planets.

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Dunham, David W. "Asteroid and Cometary Occultations." International Astronomical Union Colloquium 98 (1988): 147–48. http://dx.doi.org/10.1017/s0252921100092551.

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Occultations of stars by minor planets and comets can be used to determine the diameter of the occulting body. With photoelectric equipment, it might also be possible to measure the diameter of the occulted star or to resolve close binary systems at the same time.On 1983 May 29, (2) Pallas occulted the 4.7-mag. star 1 Vulpeculae. A star this bright is occulted by one of the four largest asteroids only once every 60 years. Timings were sent by 130 observers in Florida, Louisiana, Texas, Arizona, Sonora, and Baja California, making it the best-observed asteroidal occultation to date. Asteroidal

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Sephton, Mark A. "Organic matter in carbonaceous meteorites: past, present and future research." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 363, no. 1837 (2005): 2729–42. http://dx.doi.org/10.1098/rsta.2005.1670.

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Carbonaceous meteorites are fragments of ancient asteroids that have remained relatively unprocessed since the formation of the Solar System. These carbon-rich objects provide a record of prebiotic chemical evolution and a window on the early Solar System. Many compound classes are present reflecting a rich organic chemical environment during the formation of the planets. Recent theories suggest that similar extraterrestrial organic mixtures may have acted as the starting materials for life on Earth.

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Scott, Edward R. D., and Horton E. Newsom. "Planetary Compositions - Clues from Meteorites and Asteroids." Zeitschrift für Naturforschung A 44, no. 10 (1989): 924–34. http://dx.doi.org/10.1515/zna-1989-1005.

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Abstract We review the chemical and mineralogical properties of primitive meteorites and chemical data for the Sun, Comet Halley and interplanetary dust particles. Regardless of where meteorites formed, concentrations of rock-forming elements in solar nebular solids could not have varied simply with distance from the Sun. Thus compositional differences between neighboring planets and the chemical and mineralogical diversity of chondritic asteroids may have been caused by local variations in the compositions of planetesimals, rather than transport of planetesimals over large heliocentric dis t

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Kiss, L. L., Gy Szabó, and K. Sárneczky. "CCD photometry and new models of 5 minor planets." Astronomy and Astrophysics Supplement Series 140, no. 1 (1999): 21–28. http://dx.doi.org/10.1051/aas:1999115.

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Vaduvescu, O., L. Hudin, T. Mocnik, et al. "280 one-opposition near-Earth asteroids recovered by the EURONEAR with the Isaac Newton Telescope." Astronomy & Astrophysics 609 (January 2018): A105. http://dx.doi.org/10.1051/0004-6361/201731844.

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Context. One-opposition near-Earth asteroids (NEAs) are growing in number, and they must be recovered to prevent loss and mismatch risk, and to improve their orbits, as they are likely to be too faint for detection in shallow surveys at future apparitions. Aims. We aimed to recover more than half of the one-opposition NEAs recommended for observations by the Minor Planet Center (MPC) using the Isaac Newton Telescope (INT) in soft-override mode and some fractions of available D-nights. During about 130 h in total between 2013 and 2016, we targeted 368 NEAs, among which 56 potentially hazardous

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Hallis, L. J. "D/H ratios of the inner Solar System." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, no. 2094 (2017): 20150390. http://dx.doi.org/10.1098/rsta.2015.0390.

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The original hydrogen isotope (D/H) ratios of different planetary bodies may indicate where each body formed in the Solar System. However, geological and atmospheric processes can alter these ratios through time. Over the past few decades, D/H ratios in meteorites from Vesta and Mars, as well as from S- and C-type asteroids, have been measured. The aim of this article is to bring together all previously published data from these bodies, as well as the Earth, in order to determine the original D/H ratio for each of these inner Solar System planetary bodies. Once all secondary processes have bee

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Downing, C. A., B. Ahmady, C. R. A. Catlow, and N. H. de Leeuw. "The interaction of hydrogen with the {010} surfaces of Mg and Fe olivine as models for interstellar dust grains: a density functional theory study." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 371, no. 1994 (2013): 20110592. http://dx.doi.org/10.1098/rsta.2011.0592.

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There is no consensus as yet to account for the significant presence of water on the terrestrial planets, but suggested sources include direct hydrogen adsorption from the parent molecular cloud after the planets’ formation, and delivery of hydrous material via comets or asteroids external to the zone of the terrestrial planets. Alternatively, a more recent idea is that water may have directly adsorbed onto the interstellar dust grains involved in planetary formation. In this work, we use electronic structure calculations based on the density functional theory to investigate and compare the bu

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Cellino, Alberto, Dominique Bockelée-Morvan, Walter F. Huebner, et al. "COMMISSION 15: PHYSICAL STUDIES OF COMETS AND MINOR PLANETS." Proceedings of the International Astronomical Union 6, T27B (2010): 168–72. http://dx.doi.org/10.1017/s1743921310004941.

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This report of the business meeting of Commission 15 at the 2009 IAU GA is based on notes provided by Walter Huebner, past president, and on the minutes taken by Daniel Boice, secretary of Commission 15 in the triennium 2006 to 2009, with additional notes from the current secretary, Daniel Hestroffer. The business meeting was split into two sessions, the first held on 5 August and the second held on 11 August. This report presents the minutes of the two Commission 15 business-meeting sessions held during General Assembly XXVII.

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Huebner, Walter F., Alberto Cellino, Edward F. Tedesco, et al. "COMMISSION 15: PHYSICAL STUDY OF COMETS AND MINOR PLANETS." Proceedings of the International Astronomical Union 3, T26B (2007): 128–30. http://dx.doi.org/10.1017/s174392130802379x.

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This report of the business meeting at the 2006 IAU GA is based on notes provided by Edward Tedesco, past president, and on the minutes taken by Petrus Jenniskens, secretary of Commission 15 in the triennium 2003 to 2006, with additional notes from the current secretary of Commission 15, Daniel Boice. For political reasons the incoming President, Walter Huebner, was unable to attend the General Assembly.

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van Kooten, Elishevah M. M. E., Frédéric Moynier, and Arnaud Agranier. "A unifying model for the accretion of chondrules and matrix." Proceedings of the National Academy of Sciences 116, no. 38 (2019): 18860–66. http://dx.doi.org/10.1073/pnas.1907592116.

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The so far unique role of our Solar System in the universe regarding its capacity for life raises fundamental questions about its formation history relative to exoplanetary systems. Central in this research is the accretion of asteroids and planets from a gas-rich circumstellar disk and the final distribution of their mass around the Sun. The key building blocks of the planets may be represented by chondrules, the main constituents of chondritic meteorites, which in turn are primitive fragments of planetary bodies. Chondrule formation mechanisms, as well as their subsequent storage and transpo

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Tichý, Miloš. "Klet Observatory – European Contribution to Detecting and Tracking of Near Earth Objects." Geoinformatics FCE CTU 7 (December 29, 2011): 107–16. http://dx.doi.org/10.14311/gi.7.9.

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Near Earth Object (NEO) research is an expanding field of astronomy. Is is important for solar system science and also for protecting human society from asteroid and comet hazard. A near-Earth object (NEO) can be defined as an asteroid or comet that has a possibility of making an approach to the Earth, or possibly even collide with it. The discovery rate of current NEO surveys reflects progressive improvement in a number of technical areas. An integral part of NEO discovery is astrometric follow-up fundamental for precise orbit computation and for the reasonable judging of future close encount

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Fox, J. L. "Models for aurora and airglow emissions from other planetary atmospheres." Canadian Journal of Physics 64, no. 12 (1986): 1631–56. http://dx.doi.org/10.1139/p86-288.

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Models for aurora and airglow emissions from planetary atmospheres other than the Earth are surveyed, with emphasis on accomplishments of the last seven years. The goals of modeling the terrestrial planets and modeling the outer planets are very different. Because less is known about the atmospheres of the outer planets, models of their luminosity seek to provide information about the basic structure of the atmospheres and to identify the major production mechanisms. Models of the terrestrial planets have recently begun to address more complex questions about the abundances of trace and minor

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Krons, Aivars. "VISUALIZATION IN ASTRONOMY AT GENERAL SCHOOL." GAMTAMOKSLINIS UGDYMAS / NATURAL SCIENCE EDUCATION 6, no. 2 (2009): 31–37. http://dx.doi.org/10.48127/gu-nse/09.6.31a.

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This is an International Year of Astronomy (IYA 2009) when we pay great attention to astronomy education. The International Year of Astronomy is a year-long celebration of astronomy, taking place in 2009 to coincide with the 400th anniversary of the first recorded astronomical observations with a telescope by Galileo Galilei. Author presents a modern approach to teaching astronomy and planetary sciences, centered on visual images and simulations of planetary objects. The basic idea is to take the students to other celestial objects as tourists, and to teach science through the observations of

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de la Fuente Marcos, C., and R. de la Fuente Marcos. "Waiting to make an impact: a probable excess of near-Earth asteroids in 2018 LA-like orbits." Astronomy & Astrophysics 621 (January 2019): A137. http://dx.doi.org/10.1051/0004-6361/201834313.

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Context. The discovery and tracking of 2018 LA marks only the third instance in history that the parent body of a fireball has been identified before its eventual disintegration in our atmosphere. The subsequent recovery of meteorites from 2018 LA was only the second time materials from outer space that reached the ground could be linked with certitude to a particular minor body. However, meteoroids like 2018 LA and its forerunners, 2008 TC3 and 2014 AA, are perhaps fragments of larger members of the near-Earth object (NEO) population. As the processes leading to the production of such fragmen

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Kipreos, Yung, and Inseok Song. "An Unbiased Mineral Compositional Analysis Technique for Circumstellar Disks." American Journal of Undergraduate Research 18, no. 2 (2021): 13–27. http://dx.doi.org/10.33697/ajur.2021.043.

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A circumstellar disk that surrounds a star is composed of gas, dust, and rocky objects that are in orbit around it. Around infant stars, this disk can act as a source of material that can be used to form planetesimals, which can then accrete more material and form into planets. Studying the mineral composition of these disks can provide insight into the processes that created our solar system. The purpose of this paper is to analyze the mineral composition of these disks by using a newly created python package, Min-CaLM. This package determines the relative mineral abundance within a disk by u

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Gai, Mario, Alberto Vecchiato, Alessandro Sozzetti, Sebastiano Ligori, and Mario G. Lattanzi. "Gravitation Astrometric Measurement Experiment (GAME)." Proceedings of the International Astronomical Union 6, S276 (2010): 535–36. http://dx.doi.org/10.1017/s1743921311021119.

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AbstractGAME (Gravitation Astrometric Measurement Experiment) is a mission concept based on astronomical techniques for high precision measurements of interest to Fundamental Physics and cosmology, in particular the γ and β parameters of the Parameterized Post-Newtonian formulation of gravitation theories extending the General Relativity.High precision astrometry also provides the light deflection induced by the quadrupole moment of Jupiter and Saturn, and, by high precision determination of the orbits of Mercury and high elongation asteroids, the PPN parameter β.The astrometric and photometri

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