Gaia Data Release 3 contains accurate photometric observations of more than 150,000 asteroids covering a time interval of 34 months. With a total of about 3,000,000 measurements, a typical number of observations per asteroid ranges from a few to several tens. We aimed to reconstruct the spin states and shapes of asteroids from this dataset. We computed the viewing and illumination geometry for each individual observation and used the light curve inversion method to find the best-fit asteroid model, which was parameterized by the sidereal rotation period, the spin axis direction, and a low-resolution convex shape. To find the best-fit model, we ran the inversion for tens of thousands of trial periods on interval 2-10,000 h, with tens of initial pole directions. To find the correct rotation period, we also used a triaxial ellipsoid model for the shape approximation. In most cases the number of data points was insufficient to uniquely determine the rotation period. However, for about 8600 asteroids we were able to determine the spin state uniquely together with a low-resolution convex shape model. This large sample of new asteroid models enables us to study the spin distribution in the asteroid population. The distribution of spins confirms previous findings that (i) small asteroids have poles clustered toward ecliptic poles, likely because of the YORP-induced spin evolution, (ii) asteroid migration due to the Yarkovsky effect depends on the spin orientation, and (iii) members of asteroid families have the sense of rotation correlated with their proper semimajor axis: over the age of the family, orbits of prograde rotators evolved, due to the Yarkovsky effect, to larger semimajor axes, while those of retrograde rotators drifted in the opposite direction. 

/pdf/reconstruction-of-asteroid-spin-states-from-gaia-dr3-2coszjsc.pdf

Reconstruction of asteroid spin states from Gaia DR3 photometry

We present a database of the absolute magnitudes of asteroids named the Kharkiv Asteroid Absolute Magnitude Database (KhAAMD). The database includes a homogeneous set of the absolute magnitudes for about 400 asteroids in the new HG 1 G 2 magnitude system. We performed a comparative analysis of the asteroid absolute magnitudes between the Kharkiv database and other main magnitude databases (MPC, Pan-STARRS, ATLAS, PTF, and Gaia). We show that the Pan-STARRS absolute magnitude dataset has no systematic deviations and is the most suitable for the determination of diameters and albedos of asteroids. For the MPC dataset, there is a linear trend of overestimating the absolute magnitudes of bright objects and underestimating the magnitudes of faint asteroids. The ATLAS dataset has both a systematic overestimation of asteroid magnitudes and a linear trend. We propose equations that can be used to correct for systematic errors in the MPC and the ATLAS magnitude datasets. There are possible systematic deviations of about 0.1 mag for the Gaia and PTF databases but there are insu ﬃ cient data overlapping with our data for a deﬁnitive analysis.

Kharkiv database of asteroid absolute magnitudes: Comparative analysis with other datasets

ABSTRACT We investigate the photometric properties of 35 well-observed asteroids using dense ground-based and sparse ATLAS survey data. Focusing on two-colour photometric phase functions, derived using inverse methods, we explore the wavelength dependence. Our study reveals distinct (G1, G2) domains for cyan and orange filters, especially among some S-complex asteroids. For other asteroids, substantial uncertainties prevail, or their distributions of phase curve parameters overlap, precluding definitive conclusions on wavelength dependence. Notably, for S-complex objects, the effect appears systematic, characterized by lower G2 values in the cyan filter. The effect can be explained by considering the known geometric albedo correlation: higher albedo corresponds to flatter, whereas lower albedo corresponds to steeper phase curves. In the case of equal albedo, asteroids with red spectral slopes have a more pronounced opposition effect in red and asteroids with blue spectral slopes in blue filters. We explore the variation of slope differences of orange and cyan phase curves with phase angle. For most asteroids, the largest nominal variation is observed at phase angles &amp;lt; 10°. This suggests that the phase colouring for the orange–cyan colour slope is more pronounced at small phase angles. Through meticulous analysis of the opposition effect amplitudes, we also pinpoint preferred rotational pole solutions. We identify inconsistencies between phase curve parameters and spectral types in specific cases. The shape- and geometry-corrected phase curves signify an important advancement in studying asteroid photometric behaviour and may offer a deeper understanding of surface and regolith properties previously obscured by these effects, such as surface roughness. 

Phase curve wavelength dependency as revealed by shape- and geometry- corrected asteroid phase curves

Optical observations of the potentially hazardous asteroid (4660) Nereus at opposition 2021


 The shapes of asteroid phase curves are influenced by the physical properties of asteroid surfaces. The variation of an asteroid’s brightness as a function of the solar phase angle can tell us about surface properties such as grain size distribution, roughness, porosity, and composition. Phase curves are traditionally derived from photometric observations at visible wavelengths, but phase curves using infrared data can also provide useful information about an asteroid surface. Using photometric observations centered near ∼3.4 μm from the W1 band of the Near-Earth Object Wide-field Infrared Survey Explorer mission, we construct thermally and rotationally corrected infrared phase curves for a sample of main-belt asteroids, which includes asteroids observed by the AKARI satellite, as well as subsets of the Themis and Flora dynamical families. We calculate the linear slope of the phase curves as a measure of their shape and compare W1 phase slopes to band depths of absorption features associated with hydrated materials, spectral slopes, visible albedos, W1 albedos, and diameters. We observe a steepening of the W1 phase slope of C-type asteroids with increasing 2.7 μm band depth but little correlation between the phase slope and 3 μm band depth or 3 μm spectral slope. The C-types in our sample exhibit steeper average W1 phase slopes than M- or S-types, similar to visible-light phase slopes. We also observe steeper W1 phase slopes for smaller-diameter objects within the Themis family and explore comparisons to Jupiter-family comets in phase slope versus albedo space.

3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry

The amount of sparse asteroid photometry being gathered by both space- and ground-based surv e ys is growing exponentially. This large volume of data poses a computational challenge owing to both the large amount of information to be processed and the new methods needed to combine data from different sources (e.g. obtained by different techniques, in different bands, and having different random and systematic errors). The main goal of this work is to develop an algorithm capable of merging sparse and dense data sets, both relative and differential, in preparation for asteroid observations originating from, for example, Gaia , TESS , ATLAS, LSST, K2 , VISTA, and many other sources. We present a no v el method to obtain asteroid phase curves by combining sparse photometry and differential ground-based photometry. In the traditional approach, the latter cannot be used for phase curves. Merging those two data types allows for the extraction of phase-curve information for a growing number of objects. Our method is validated for 26 sample asteroids observed by the Gaia mission.

/pdf/asteroid-phase-curves-using-sparse-gaia-dr2-data-and-psfqiwa6.pdf

Asteroid phase curves using sparse Gaia DR2 data and differential dense light curves


 We present research program and project for high-resolution
 wavelength-dispersive spectrometer dedicated to low-energy X-ray
 spectroscopy at the electron cooler of the CRYRING@ESR storage ring,
 which is a part of the international Facility for Antiproton and Ion
 Research (FAIR) currently being built in Darmstadt. Due to the
 unique shape of the electorn-ion recombination X-ray source,
 resulting from the overlapping of the electron and ion beams in the
 electron cooler, the spectrometer can work in the specific
 asymmetric von Hamos (AvH) geometry. In order to completely
 eliminate the influence of Doppler effect on the measured X-ray
 energies, two asymmetric von Hamos spectrometers will be installed
 next to the dipole magnets on both sides of the electron cooler to
 detect blue/red (0°/180°) shifted X-rays, e.g. emitted in the radiative recombination (RR) process. The
 X-ray-tracing Monte-Carlo simulations show that the proposed AvH
 spectrometer will allow to determine with sub-meV precision, the
 low-energy X-rays (5–10 keV) emitted from stored bare or
 few-electron heavy ions interacting with cooling electrons. This
 experimental precision will enable accurate studies of the quantum
 electrodynamics (QED) effects in mid-Z H- and He-like ions.

pdf/a-high-resolution-asymmetric-von-hamos-spectrometer-for-low-1vm3u725rx.pdf

A high-resolution asymmetric von Hamos spectrometer for low-energy X-ray spectroscopy at the CRYRING@ESR electron cooler

Heavy-ion collisions are a unique tool to test the behaviour of matter in extreme conditions. The momentum correlations of charm and bottom hadrons have been considered for testing heavy quarks' thermalisation in the hot, dense medium produced by the collisions. In addition to these back-to-back correlations due to the quark-anti-quark pair creation dynamics, there are other important sources of momentum correlations, which allow us to explore the rich physics of heavy-ion collisions further. Here we show significant momentum correlations even in the thermalisation of charm quarks in the expanding medium, and this effect can be measured in collisions at sufficiently low energies. The momentum correlations depend on the correlations in the configuration space, more specifically, on the spatial separation between charm and anti-charm hadrons emission points. The pair production locality and spatial diffusion of the charm quarks give the latter. Using an example of central Pb+Pb collisions at the CERN SPS energies, we show that future measurements of the azimuthal correlations of charm and anti-charm hadrons should allow us to distinguish between different assumptions on their spatial correlations. This provides a unique window into a poorly understood sector of particle production at high-energy densities. The measurements can help to constrain the diffusion of charm quarks and verify assumptions concerning production locality of a charm and ant-charm quark pair.

pdf/production-locality-and-spatial-diffusion-of-heavy-flavour-2fg13p4i.pdf

Production locality and spatial diffusion of heavy flavour at high energy densities

Handle everyday research tasks with reliable, citation-backed results

Your personal Research Agent to handle research tasks with citation-backed results

Popular Tasks used by Researchers

How can I help with your research?

Meet SciSpace

Get more enhanced response by uploading the PDFs you want me to reference.

No relevant PDFs in your library

SciSpace is the AI research assistant for academics. Run systematic literature reviews on 280M+ papers, and write papers with cited sources. Trusted by 1M+ students, PhDs & researchers.

SciSpace | AI for Research

Analyze PDFs

Code & Manuscripts

Funding & Grants

Literature & Patents

Medical & Clinical Data

Systematic Review

Visualize & Present

Web & Data

Build a Google Scholar-like website for your research.

Build a website

Create charts and images for your research

Create a Chart

Write a paper for submission to a journal

Draft a manuscript

Patent Search

Design eye-catching scientific posters in minutes.

Scientific Poster Generation

Systematic Literature Review

One task is running at the moment. Your messages will be shown right after.

Drag and drop or click here to browse

Loved by <highlight>1 million+</highlight> researchers

Extract a list of specific topics and their sources from unstructured text

Topics

Compare and analyze relevant papers that matches with your search

Papers

Get insights from PDFs and bookmarked papers from your library

My library

Recent searches

Try searching for:

Catch AI-generated content in scholarly and non-scholarly content

{ai} Detector

Ai Writer

Get PDF Summaries, highlighted text explanations 

Chat with PDF

Effortlessly create in-text citations and bibliographies in APA and 2,500 other formats

Citation generator

Get explanations, summaries, and answers on academic papers

Ease up your research workflow with {scispace}'s cohort of exciting AI tools

Elevate your academic writing skills and convey your ideas the way you want

Paraphraser

Explore our range of reading and writing tools

Your file is being prepared and should be ready in a few minutes. If it's a large file, it might take a bit longer. You can close this window, and we'll email you the file when it's done.

You have reached a maximum limit of <strong>{limit}</strong> columns in the table. Remove at least <strong>1</strong> column to add or create another one.

Kielce

Author Tools

Chat about Author

Papers

Asteroid phase curves using sparse Gaia DR2 data and differential dense light curves

A high-resolution asymmetric von Hamos spectrometer for low-energy X-ray spectroscopy at the CRYRING@ESR electron cooler

Production locality and spatial diffusion of heavy flavour at high energy densities