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111. Mass of (11) Parthenope
ID:
ivo://CDS.VizieR/J/A+A/320/652
Title:
Mass of (11) Parthenope
Short Name:
J/A+A/320/652
Date:
21 Oct 2021
Publisher:
CDS
Description:
The asteroid observations made with the automatic meridian circle at Bordeaux observatory from 1985 to 1994, and which have recently become available, are presented. The residuals of these observations obtained using the orbital elements published in the ``Ephemerides of Minor Planets for 1996'' are analysed. An anomaly for the asteroid (17) Thetis was found, indicating a current close encounter between this asteroid and (4) Vesta. Such an encounter will allow very interesting determinations of the mass of Vesta to be made in the future. Lastly, our determination of the mass of (11) Parthenope is discussed, which was based on its perturbations on the orbit of Thetis. The result obtained, (2.58+/-0.10)x10^-12^M{sun}, appears significant.
112. M4AST
ID:
ivo://padc.obspm.planeto/m4ast/q/epn_core
Title:
M4AST
Short Name:
M4AST
Date:
16 Jul 2024 13:55:03
Publisher:
Paris Astronomical Data Centre - IMCCE
Description:
compiled database for asteroid spectra in the visible and NIR regions
113. Meteor showers new parent bodies
ID:
ivo://CDS.VizieR/J/A+A/622/A84
Title:
Meteor showers new parent bodies
Short Name:
J/A+A/622/A84
Date:
21 Oct 2021
Publisher:
CDS
Description:
Several new meteor showers are added to the International Astronomical Union (IAU) list of meteor showers every year. Given the multiplication of video meteor measurements new parent bodies are to be found in addition to new showers. Such an endeavor is usually performed by comparing orbital elements, using a high threshold single-linking Dsh-criterion. However, questions remain about the accuracy of the method and the veracity of the newly associated parent bodies. Our goal is to find the presence of new parent bodies in a statistical meaningful way. A search for parent bodies was performed among SonotaCo and EDMOND databases. The association of asteroids with meteors was based on different methods, discussed and compared below. In addition, a thorough statistical test was performed in order to investigate the possible random associations. A list of potential new parent bodies associated with at least 50 meteors is found. A statistical test was used to show whether the group of meteor orbits and the asteroid is a random coincidence or not. Out of 54 potential new parent bodies, only three new parent bodies are not excluded by the statistical test: 2014 BN14, 2015 TX24 and 2015 QT3, with a probability of chance occurrence of 37, 10 and 13%, respectively. This shows the need for rigorous method when searching for the existence of meteor showers and parent bodies. Ideally, such a test (or even better, tests) should be conducted in order to confirm (or not) the current IAU list of meteor showers. Similarly, all meteor orbit data in our databases should ideally be revisited using the latest methods providing a better estimate of the real uncertainty and accuracy of the derived orbits.
114. Meteor stream activity. II.
ID:
ivo://CDS.VizieR/J/A+A/295/206
Title:
Meteor stream activity. II.
Short Name:
J/A+A/295/206
Date:
21 Oct 2021
Publisher:
CDS
Description:
In the past two centuries, alert amateur and professional meteor astronomers have documented 35 outbursts of 17 individual meteor streams well enough to allow the construction of a homogeneous set of activity curves. These curves add to similar profiles of the annual streams in a previous paper (Paper I, See Cat. <J/A+A/287/990>). The activity curves, expressed in terms of Zenith Hourly Rates (ZHR), have a shape that is usually well described by: ZHR=ZHR(max)10^(-B|{lambda}_{sun }_-{lambda_{sun}_(max)}|)^. The steepness of the slopes varies from an exponent of B=7 to B=220 per degree of solar longitude, with a typical value of B=30.
115. Mg-rich olivines with electron microscopy
ID:
ivo://CDS.VizieR/J/ApJ/831/197
Title:
Mg-rich olivines with electron microscopy
Short Name:
J/ApJ/831/197
Date:
21 Oct 2021
Publisher:
CDS
Description:
Antarctica micrometeorites (~1200) and cosmic spherules (~5000) from deep sea sediments are studied using electron microscopy to identify Mg-rich olivine grains in order to determine the nature of the particle precursors. Mg-rich olivine (FeO<5wt%) in micrometeorites suffers insignificant chemical modification during its history and is a well-preserved phase. We examine 420 forsterite grains enclosed in 162 micrometeorites of different types-unmelted, scoriaceous, and porphyritic-in this study. Forsterites in micrometeorites of different types are crystallized during their formation in solar nebula; their closest analogues are chondrule components of CV-type chondrites or volatile rich CM chondrites. The forsteritic olivines are suggested to have originated from a cluster of closely related carbonaceous asteroids that have Mg-rich olivines in the narrow range of CaO (0.1-0.3wt%), Al_2_O_3_ (0.0-0.3wt%), MnO (0.0-0.3wt%), and Cr_2_O_3_ (0.1-0.7wt%). Numerical simulations carried out with the Chemical Ablation Model (CABMOD; Vondrak+ 2008ACP.....8.7015V) enable us to define the physical conditions of atmospheric entry that preserve the original compositions of the Mg-rich olivines in these particles. The chemical compositions of relict olivines affirm the role of heating at peak temperatures and the cooling rates of the micrometeorites. This modeling approach provides a foundation for understanding the ablation of the particles and the circumstances in which the relict grains tend to survive.
116. Minor Planet Center - Asteroid Orbital Data
ID:
ivo://org.gavo.dc/mpc/q/import
Title:
Minor Planet Center - Asteroid Orbital Data
Date:
03 Jul 2024 11:48:02
Publisher:
The GAVO DC team
Description:
Complete Asteroid Data from the Minor Planet Center (MPC), updated once per month. The MPC operates at the Smithsonian Astrophysical Observatory under the auspices of Division III of the International Astronomical Union (IAU). The MPC Orbit database contains orbital elements of minor planets that have been published in the Minor Planet Circulars, the Minor Planet Orbit Supplement and the Minor Planet Electronic Circulars.
117. Mission Accessible Near-Earth Objects Survey
ID:
ivo://CDS.VizieR/J/AJ/152/163
Title:
Mission Accessible Near-Earth Objects Survey
Short Name:
J/AJ/152/163
Date:
21 Oct 2021
Publisher:
CDS
Description:
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 1-4m 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 for a statistical study to constrain overall properties of the NEO population. A weak correlation seems to indicate that smaller objects are more spherical than larger ones. We also report seven NEOs that are fully characterized (light curve and visible spectra) as the most suitable candidates for a future human or robotic mission. Viable mission targets are objects fully characterized, with {Delta}v^NHATS^{<=}12km/s, and a rotational period P>1hr. Assuming a similar rate of object characterization as reported in this paper, approximately 1230 NEOs need to be characterized in order to find 100 viable mission targets.
118. mm-dm-sized meteoroids spectral & orbital survey
ID:
ivo://CDS.VizieR/J/A+A/629/A71
Title:
mm-dm-sized meteoroids spectral & orbital survey
Short Name:
J/A+A/629/A71
Date:
21 Oct 2021
Publisher:
CDS
Description:
We investigate the spectra, material properties and orbital distribution of mid-sized meteoroids. Our study aims to distinguish characteristics of different size populations of meteoroids and reveal the heterogeneity of identified meteoroid streams. The emission spectra and multi-station meteor trajectories were collected within the AMOS network observations. The sample is based on 202 meteors of -1 to -14 magnitude, corresponding to meteoroids of mm-dm in size. Overall increase of Na content compared to the population of mm-sized meteoroids was detected, reflecting weaker effects of space weathering processes on larger meteoroids. We report on very low ratio of pure iron meteoroids and the discovery of a new spectral group of Fe-rich meteors. The majority of meteoroids on asteroidal orbits were found to be chondritic. Thermal processes causing Na depletion and physical processes resulting in Na-rich spectra are described and linked to characteristically increased material strengths. Numerous major and minor shower meteors were identified in our sample, revealing various degrees of heterogeneity within Halley-type, ecliptical and sungrazing meteoroid streams.
119. MOOJa catalogs for Solar System Objects
ID:
ivo://CDS.VizieR/J/A+A/655/A47
Title:
MOOJa catalogs for Solar System Objects
Short Name:
J/A+A/655/A47
Date:
22 Feb 2022
Publisher:
CDS
Description:
The Javalambre Photometric Local Universe Survey (J-PLUS) is an observational campaign that aims to obtain photometry in 12 ultraviolet-visible filters (0.3-1um) over ~8500deg^2^ of the sky observable from Javalambre (Teruel, Spain). Due to its characteristics and observation strategy, this survey will allow a great number of Solar System small bodies to be analyzed, and with improved spectrophotometric resolution with respect to previous large-area photometric surveys in optical wavelengths. The main goal of the present work is to present the first catalog of magnitudes and colors of minor bodies of the Solar System compiled using the first data release (DR1) of the J-PLUS observational campaign: the Moving Objects Observed from Javalambre (MOOJa) catalog. Using the compiled photometric data we obtained very-low-resolution reflectance (photo)spectra of the asteroids. We first used a {sigma}-clipping algorithm in order to remove outliers and clean the data. We then devised a method to select the optimal solar colors in the J-PLUS photometric system. These solar colors were computed using two different approaches: on one hand, we used different spectra of the Sun convolved with the filter transmissions of the J-PLUS system, and on the other, we selected a group of solar-type stars in the J-PLUS DR1 according to their computed stellar parameters. Finally, we used the solar colors to obtain the reflectance spectra of the asteroids. We present photometric data in the J-PLUS filters for a total of 3122 minor bodies (3666 before outlier removal), and we discuss the main issues with the data, as well as some guidelines to solve them.
120. Near-Earth asteroid (1917) Cuyo opt. and IR obs.
ID:
ivo://CDS.VizieR/J/A+A/627/A172
Title:
Near-Earth asteroid (1917) Cuyo opt. and IR obs.
Short Name:
J/A+A/627/A172
Date:
21 Oct 2021
Publisher:
CDS
Description:
The near-Earth asteroid (1917) Cuyo was subject to radar and light curve observations during a close approach in 1989, and observed up until 2008. It was selected as one of our ESO Large Programme targets, aimed at observational detections of the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect through long-term light curve monitoring and physical modelling of near-Earth asteroids. We aim to constrain the physical properties of Cuyo: shape, spin-state, and spectroscopic & thermophysical properties of the surface. We acquired photometric light curves of Cuyo spanning the period between 2010 and 2013, which we combined with published light curves from 1989-2008. Our thermal-infrared observations were obtained in 2011. Rotationally resolved optical spectroscopy data were acquired in 2011 and combined with all available published spectra to investigate any surface material variegation. We developed a convex light-curve-inversion shape of Cuyo that suggests the presence of an equatorial ridge, typical for an evolved system close to shedding mass due to fast rotation. We determine limits of YORP strength through light-curve-based spin-state modelling, including both negative and positive acceleration values, between -0.7x10^-8^rad/day^2^ and 1.7x10^-8^rad/day^2^. Thermo-physical modelling with the ATPM provides constraints on the geometric albedo, pV=0.24+/-0.07, the effective diameter Deff=3.15+/-0.08km, the thermal inertia =44+/-9J/m^2^/s^1/2^/K, and a roughness fraction of 0.52+/-0.26. This enabled a YORP strength prediction of (-6.39+/-0.96)x10^-10^rad/day^2^. We also see evidence of surface compositional variation. The low value of YORP predicted by means of thermophysical analysis, consistent with the results of the light curve study, might be due to the self-limiting properties of rotational YORP, possibly involving movement of sub-surface and surface material. This may also be consistent with the surface compositional variation that we see. The physical model of Cuyo can be used to investigate cohesive forces as a way to explain why some targets survive rotation rates faster than the fission limit.