English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/189378
Share/Impact:
Statistics
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL
Exportar a otros formatos:

Title

Physical properties of PHA 2014 JO 25 from a worldwide observational campaign

AuthorsAznar, A.; De León, J.; Popescu, M.; Serra-Ricart, M.; Short, P.; Pravec, P.; Vaduvescu, O.; Licandro, J.; Ortiz, José Luis ; Sota Ballano, Alfredo ; Morales, Nicolás ; Lorenzi, V.; Warner, B.; Oey, J.; Groom, R.
KeywordsTechniques: photometric
Techniques: spectroscopic
Minor planets, asteroids: individual: 2014 JO(25)
Issue Date2019
PublisherOxford University Press
CitationMonthly Notices of the Royal Astronomical Society 483: 4820- 4827 (2019)
AbstractThe study of minor planets is motivated both by fundamental science of Solar system origins (some of these bodies contain the most pristine materials from the early ages of the planetary nebula) and by practical reasons concerning space exploration and impact frequency with Earth. Among minor bodies, near-Earth asteroids are a particularly important group: these objects are nearby the Earth's orbit and they represent both resources and hazards to humans. This is the case of 2014 JO 25. The encounter of this potentially hazardous asteroid with the Earth at 0.011 75 au on 2017 April 19 was a good opportunity to study its properties through photometric and spectral analyses. The work we present here has been carried out thanks to a worldwide observational campaign that included time-series photometry and spectroscopy in the visible and near-infrared wavelengths. The optical images for photometric analysis were collected at different phase angles using small telescopes (<0.5 m) and medium telescopes (from 0.6 to 1.5 m). Spectral analysis was performed by 2-4 m telescopes. The light curve of 2014 JO 25 indicates a synodic rotational period of 4.5286 ± 0.0004 h. Although rotational period had been previously obtained by other authors, this work confirms it with a better accuracy. The obtained reflectance spectrum of this asteroid indicates that it belongs to the S-complex and its surface is most likely composed of a mixture of pyroxenes and olivine. From the comparison of its spectrum to those of meteorite samples, as well as from the wavelength position of the first absorption band (close to 0.9 μm), we suggest that this asteroid might contain a large fraction of low-calcium pyroxene and, tentatively, some amounts of metal.© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
Publisher version (URL)http://dx.doi.org/10.1093/mnras/sty3250
URIhttp://hdl.handle.net/10261/189378
Identifiersdoi: 10.1093/mnras/sty3250
issn: 1365-2966
Appears in Collections:(IAA) Artículos
Files in This Item:
File Description SizeFormat 
IAA_2019_sty3250.pdf1,83 MBAdobe PDFThumbnail
View/Open
Show full item record
Review this work
 


WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.