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Dissertations / Theses on the topic 'Minor planets, asteroids: general'

Author: Grafiati

Published: 4 June 2021

Last updated: 16 February 2022

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1

Thirouin, A., N. Moskovitz, R. P. Binzel, et al. "THE MISSION ACCESSIBLE NEAR-EARTH OBJECTS SURVEY (MANOS): FIRST PHOTOMETRIC RESULTS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622441.

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The Mission Accessible Near-Earth Objects Survey aims to physically characterize sub-km near-Earth objects (NEOs). We report the first photometric results from the survey that began in 2013 August. Photometric observations were performed using 1-4 m class telescopes around the world. We present rotational periods and light curve amplitudes for 86 sub-km NEOs, though in some cases only lower limits are provided. Our main goal is to obtain light curves for small NEOs (typically, sub-km objects) and estimate their rotational periods, light curve amplitudes, and shapes. These properties are used f

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2

Takir, Driss, Vishnu Reddy, Juan A. Sanchez, Michael K. Shepard, and Joshua P. Emery. "DETECTION OF WATER AND/OR HYDROXYL ON ASTEROID (16) Psyche." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622751.

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In order to search for evidence of hydration on M-type asteroid (16) Psyche, we observed this object in the 3 mu m spectral region using the long-wavelength cross-dispersed (LXD: 1.9-4.2 mu m) mode of the SpeX spectrograph/imager at the NASA Infrared Telescope Facility. Our observations show that Psyche exhibits a 3 mu m absorption feature, attributed to water or hydroxyl. The 3 m absorption feature is consistent with the hydration features found on the surfaces of water-rich asteroids, attributed to OH- and/or H2O-bearing phases (phyllosilicates). The detection of a 3 mu m hydration absorptio

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3

Nathues, A., T. Platz, M. Hoffmann, et al. "Oxo Crater on (1) Ceres: Geological History and the Role of Water-ice." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625818.

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Dwarf planet Ceres (empty set similar to 940 km) is the largest object in the main asteroid belt. Investigations suggest that Ceres is a thermally evolved, volatile-rich body with potential geological activity, a body that was never completely molten, but one that possibly partially differentiated into a rocky core and an ice-rich mantle, and may contain remnant internal liquid water. Thermal alteration and the infall of exogenic material contribute to producing a (dark) carbonaceous chondritic-like surface containing ammoniated phyllosilicates. Here we report imaging and spectroscopic analyse

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4

Jewitt, David, Jessica Agarwal, Harold Weaver, Max Mutchler, Jing Li, and Stephen Larson. "HUBBLE SPACE TELESCOPE OBSERVATIONS OF ACTIVE ASTEROID 324P/La SAGRA." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621499.

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Hubble Space Telescope observations of active asteroid 324P/La Sagra near perihelion show continued mass loss consistent with the sublimation of near-surface ice. Isophotes of the coma measured from a vantage point below the orbital plane are best matched by steady emission of particles having a nominal size. of. a similar to 100 mu m. The inferred rate of mass loss, dM(d)/dt similar to 0.2 kg s(-1), can be supplied by sublimation of water ice in thermal equilibrium with sunlight from an area as small as 930 m(2), corresponding to about 0.2% of the nucleus surface. Observations taken from a va

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5

Jewitt, David, Jessica Agarwal, Jing Li, Harold Weaver, Max Mutchler, and Stephen Larson. "Anatomy of an Asteroid Breakup: The Case of P/2013 R3." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624051.

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We present an analysis of new and published data on P/2013 R3, the first asteroid detected while disintegrating. Thirteen discrete components are measured in the interval between UT 2013 October 01 and 2014 February 13. We determine a mean, pair-wise velocity dispersion among these components of Delta nu = 0.33. +/- 0.03 ms(-1) and find that their separation times are staggered over an interval of similar to 5 months. Dust enveloping the system has, in the first observations, a cross-section of. similar to 30 km(2) but fades monotonically at a rate consistent with the action of radiation press

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6

Trilling, D. E., F. Valdes, L. Allen, et al. "The Size Distribution of Near-Earth Objects Larger Than 10 m." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626044.

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We analyzed data from the first year of a survey for Near-Earth Objects (NEOs) that we are carrying out with the Dark Energy Camera (DECam) on the 4 m Blanco telescope at the Cerro Tololo Inter-American Observatory. We implanted synthetic NEOs into the data stream to derive our nightly detection efficiency as a function of magnitude and rate of motion. Using these measured efficiencies and the solar system absolute magnitudes derived by the Minor Planet Center for the 1377. measurements of 235. unique NEOs detected, we directly derive, for the first time from a single observational data set, t

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7

Sanchez, Juan A., Vishnu Reddy, Michael K. Shepard, et al. "DETECTION OF ROTATIONAL SPECTRAL VARIATION ON THE M-TYPE ASTEROID (16) PSYCHE." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622750.

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The asteroid (16) Psyche is of scientific interest because it contains similar to 1% of the total mass of the asteroid belt and is thought to be the remnant metallic core of a protoplanet. Radar observations have indicated the significant presence of metal on the surface with a small percentage of silicates. Prior ground-based observations showed rotational variations in the near-infrared (NIR) spectra and radar albedo of this asteroid. However, no comprehensive study that combines multi-wavelength data has been conducted so far. Here we present rotationally resolved NIR spectra (0.7-2.5 mu m)

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8

Engelhardt, Toni, Robert Jedicke, Peter Vereš, et al. "An Observational Upper Limit on the Interstellar Number Density of Asteroids and Comets." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623256.

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We derived 90% confidence limits (CLs) on the interstellar number density (rho(CL)(IS)) of interstellar objects (ISOs; comets and asteroids) as a function of the slope of their size-frequency distribution (SFD) and limiting absolute magnitude. To account for gravitational focusing, we first generated a quasi-realistic ISO population to similar to 750 au from the Sun and propagated it forward in time to generate a steady state population of ISOs with heliocentric distance <50 au. We then simulated the detection of the synthetic ISOs using pointing data for each image and average detection effic

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9

Reddy, Vishnu, Juan A. Sanchez, William F. Bottke, et al. "PHYSICAL CHARACTERIZATION OF ∼2 m DIAMETER NEAR-EARTH ASTEROID 2015 TC25: A POSSIBLE BOULDER FROM E-TYPE ASTEROID (44) NYSA." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622440.

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Small near-Earth asteroids (NEAs) (< 20 m) are interesting, because they are progenitors for meteorites in our terrestrial collection. The physical characteristics of these small NEAs are crucial to our understanding of the effectiveness of our atmosphere in filtering low-strength impactors. In the past, the characterization of small NEAs has been a challenge, because of the difficulty in detecting them prior to close Earth flyby. In this study, we physically characterized the 2 m diameter NEA 2015 TC25 using ground-based optical, near-infrared and radar assets during a close flyby of the Eart

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10

Rozo, E., and T. Abbott. "The Dark Energy Survey: more than dark energy – an overview." OXFORD UNIV PRESS, 2016. http://hdl.handle.net/10150/621432.

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This overview paper describes the legacy prospect and discovery potential of the Dark Energy Survey (DES) beyond cosmological studies, illustrating it with examples from the DES early data. DES is using a wide-field camera (DECam) on the 4 m Blanco Telescope in Chile to image 5000 sq deg of the sky in five filters (grizY). By its completion, the survey is expected to have generated a catalogue of 300 million galaxies with photometric redshifts and 100 million stars. In addition, a time-domain survey search over 27 sq deg is expected to yield a sample of thousands of Type Ia supernovae and othe

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11

JeongAhn, Youngmin, and Renu Malhotra. "Simplified Derivation of the Collision Probability of Two Objects in Independent Keplerian Orbits." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624717.

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Many topics in planetary studies demand an estimate of the collision probability of two objects moving on nearly Keplerian orbits. In the classic works of Opik and Wetherill, the collision probability was derived by linearizing the motion near the collision points, and there is now a vast amount of literature using their method. We present here a simpler and more physically motivated derivation for non-tangential collisions in Keplerian orbits, as well as for tangential collisions that were not previously considered. Our formulas have the added advantage of being manifestly symmetric in the pa

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12

Wang, Xianyu, and Renu Malhotra. "Mean Motion Resonances at High Eccentricities: The 2:1 and the 3:2 Interior Resonances." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624905.

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Mean motion resonances (MMRs) play an important role in the formation and evolution of planetary systems and have significantly influenced the orbital properties and distribution of planets and minor planets in the solar system and in. exoplanetary systems. Most previous theoretical analyses have focused on the low- to moderate-eccentricity regime, but with new discoveries of high-eccentricity resonant minor planets and even exoplanets, there is increasing motivation to examine MMRs in the high-eccentricity regime. Here we report on a study of the high-eccentricity regime of MMRs in the circul

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13

Hallakoun, N., (许偲艺) S. Xu, D. Maoz, et al. "Once in a blue moon: detection of ‘bluing' during debris transits in the white dwarf WD 1145+017." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/625505.

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The first transiting planetesimal orbiting a white dwarf was recently detected in K2 data of WD 1145+017 and has been followed up intensively. The multiple, long and variable transits suggest the transiting objects are dust clouds, probably produced by a disintegrating asteroid. In addition, the system contains circumstellar gas, evident by broad absorption lines, mostly in the u' band, and a dust disc, indicated by an infrared excess. Here we present the first detection of a change in colour of WD 1145+017 during transits, using simultaneous multiband fast-photometry ULTRACAM measurements ove

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14

Ferreira, Joao. "Occultations stellaires. Une nouvelle approche grâce à la mission Gaia." Thesis, Université Côte d'Azur, 2020. http://www.theses.fr/2020COAZ4084.

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Les astéroïdes participent à la compréhension de plusieurs problèmes clés liés à la science du système solaire et à l’environnement spatial de notre planète, tels que les conditions du système solaire lors de sa formation, l’apport d’eau et de molécules organiques sur la Terre, le danger potentiel des astéroïdes proches de la Terre et leur rôle dans l’influence du climat de la Terre.Les occultations stellaires sont une occasion unique d’obtenir du sol une astrométrie astéroïde très précise, proche de la performance de Gaia, ainsi que des formes pour les astéroïdes. Lorsqu’un astéroïde cache la

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15

Hollis, Andrew John. "Studies into the rotational history of the minor planets." [N.p.], 1995. http://ethos.bl.uk/.

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16

Hollis, Andrew John. "Studies into the rotational history of the minor planets." Thesis, Open University, 1996. http://oro.open.ac.uk/57633/.

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17

Karlsson, Ola. "A Study of Jupiter Trojans." Doctoral thesis, Uppsala universitet, Institutionen för fysik och astronomi, 2012. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-172151.

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Jupiter Trojan asteroid dynamics have been studied for a long time but it is only within the last decades that the known population has become large enough to make other studies meaningful. In four articles I have been scratching the surface of the unknown Trojan knowledge space. Paper I presents photometric observations confirming a larger variety in surface redness for the smaller Trojans compared to the larger ones, in line with the groups in the outer main asteroid belt. However, the largest Trojans are significantly redder compared to the largest Cybele and Hilda asteroids. Paper II is an

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18

Mommert, M., D. E. Trilling, D. Borth, et al. "FIRST RESULTS FROM THE RAPID-RESPONSE SPECTROPHOTOMETRIC CHARACTERIZATION OF NEAR-EARTH OBJECTS USING UKIRT." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/614713.

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Using the Wide Field Camera for the United Kingdom Infrared Telescope (UKIRT), we measure the near-infrared colors of near-Earth objects (NEOs) in order to put constraints on their taxonomic classifications. The rapid-response character of our observations allows us to observe NEOs when they are close to the Earth and bright. Here we present near-infrared color measurements of 86 NEOs, most of which were observed within a few days of their discovery, allowing us to characterize NEOs with diameters of only a few meters. Using machine-learning methods, we compare our measurements to existing ast

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19

Schorghofer, Norbert, Shane Byrne, Margaret E. Landis, et al. "The Putative Cerean Exosphere." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626261.

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The ice-rich crust of dwarf planet 1 Ceres is the source of a tenuous water exosphere, and the behavior of this putative exosphere is investigated with model calculations. Outgassing water molecules seasonally condense around the winter pole in an optically thin layer. This seasonal cap reaches an estimated mass of at least 2 x 10(3) kg, and the aphelion summer pole may even retain water throughout summer. If this reservoir is suddenly released by a solar energetic particle event, it would form a denser transient water exosphere. Our model calculations also explore species other than H2O. Ligh

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20

JeongAhn, (Chung) Youngmin. "Orbital Distribution of Minor Planets in the Inner Solar System and their Impact Fluxes on the Earth, the Moon and Mars." Diss., The University of Arizona, 2015. http://hdl.handle.net/10150/579034.

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The planet crossing asteroids in the inner solar system have strongly chaotic orbits and the distributions of their angular elements (longitude of ascending node, Ω; argument of perihelion, ω; and longitude of perihelion, ϖ) are often regarded as uniform random. In the last decade, the known population of these minor planets has increased by more than a factor of four, providing a sufficiently large dataset for statistical analysis of their distribution. By choosing the observationally complete set of bright objects, we quantified the level of intrinsic non-uniformities of the angular elements

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