dc.contributor | Inst Astrofis Andalucia CSIC | |
dc.contributor | Sorbonne Univ | |
dc.contributor | Romanian Acad | |
dc.contributor | Inst Astrofis Canarias IAC | |
dc.contributor | Lab Interinst E Astron LIneA | |
dc.contributor | INCT E Universo | |
dc.contributor | Universidade Estadual Paulista (UNESP) | |
dc.contributor | Observ Nacl MCTI | |
dc.contributor | Universidade Federal do Rio de Janeiro (UFRJ) | |
dc.contributor | Inst Polytech Sci | |
dc.contributor | UPMC Univ Paris 06 | |
dc.contributor | Fed Univ Technol Parana UTFPR Curitiba | |
dc.contributor | Univ Cent Florida | |
dc.contributor | ISTEK Belde Observ | |
dc.contributor | Univ Ege | |
dc.contributor | Univ Bucharest | |
dc.contributor | Ataturk Univ | |
dc.contributor | Akdeniz Univ | |
dc.contributor | TUBITAK Natl Observ | |
dc.contributor | Tel Aviv Univ | |
dc.contributor | Erciyes Univ | |
dc.contributor | Weizmann Inst Sci | |
dc.contributor | Astron Observ Amiral Vasile Urseanu Bucharest | |
dc.contributor | Cukurova Univ | |
dc.contributor | Ege Univ | |
dc.contributor | Astron Observ Victor Anestin Bacau | |
dc.contributor | Astroclubul Bucuresti | |
dc.contributor | Stardust Observ | |
dc.contributor | St George Observ | |
dc.contributor | Ia Cu Stele | |
dc.contributor | Stardreams Observ | |
dc.contributor | ROASTERR 1 Observ | |
dc.contributor | Galati Astron Observ | |
dc.contributor | Tiraspol State Univ | |
dc.contributor | Asociatia Astroclubul Quasar | |
dc.contributor | Barlad Observ | |
dc.contributor | Kharkov Natl Univ | |
dc.contributor | Natl Space Facil Control & Test Ctr | |
dc.contributor | Natl & Kapodistrian Univ Athens | |
dc.contributor | II Mechnikov Natl Univ | |
dc.contributor | Eotvos Lorand Res Network ELKH | |
dc.contributor | Eotvos Lorand Univ | |
dc.contributor | Canakkale Onsekiz Mart Univ | |
dc.contributor | Ulupinar Observ | |
dc.contributor | Northolt Branch Observ | |
dc.contributor | Agrupacio Astron Sabadell | |
dc.contributor | Int Occultat Timing Assoc European Sect IOTA ES | |
dc.contributor | Almalex Observ | |
dc.contributor | Ellinogermaniki Agogi Observ | |
dc.contributor | Ondokuz Mayis Univ Observ | |
dc.contributor | Uzhgorod Natl Univ | |
dc.contributor | Adam Mickiewicz Univ | |
dc.contributor | Pedag Univ | |
dc.contributor | Inonu Univ | |
dc.contributor | Vilnius Univ | |
dc.contributor | Univ Zielona Gora | |
dc.date.accessioned | 2022-11-30T13:41:26Z | |
dc.date.accessioned | 2022-12-20T14:49:15Z | |
dc.date.available | 2022-11-30T13:41:26Z | |
dc.date.available | 2022-12-20T14:49:15Z | |
dc.date.created | 2022-11-30T13:41:26Z | |
dc.date.issued | 2022-08-19 | |
dc.identifier | Astronomy & Astrophysics. Les Ulis Cedex A: Edp Sciences S A, v. 664, 18 p., 2022. | |
dc.identifier | 0004-6361 | |
dc.identifier | http://hdl.handle.net/11449/237669 | |
dc.identifier | 10.1051/0004-6361/202141546 | |
dc.identifier | WOS:000841954000001 | |
dc.identifier.uri | https://repositorioslatinoamericanos.uchile.cl/handle/2250/5417725 | |
dc.description.abstract | Context. As part of our international program aimed at obtaining accurate physical properties of trans-Neptunian objects (TNOs), we predicted a stellar occultation by the TNO (38628) Huya of the star Gaia DR2 4352760586390566400 (m(G) = 11.5 mag) on March 18, 2019. After an extensive observational campaign geared at obtaining the astrometric data, we updated the prediction and found it favorable to central Europe. Therefore, we mobilized half a hundred of professional and amateur astronomers in this region and the occultation was finally detected by 21 telescopes located at 18 sites in Europe and Asia. This places the Huya event among the best ever observed stellar occultation by a TNO in terms of the number of chords. Aims. The aim of our work is to determine an accurate size, shape, and geometric albedo for the TNO (38628) Huya by using the observations obtained from a multi-chord stellar occultation. We also aim to provide constraints on the density and other internal properties of this TNO. Methods. The 21 positive detections of the occultation by Huya allowed us to obtain well-separated chords which permitted us to fit an ellipse for the limb of the body at the moment of the occultation (i.e., the instantaneous limb) with kilometric accuracy. Results. The projected semi-major and minor axes of the best ellipse fit obtained using the occultation data are (a ', b ') = (217.6 +/- 3.5 km, 194.1 +/- 6.1 km) with a position angle for the minor axis of P ' = 55.2 degrees +/- 9.1. From this fit, the projected area-equivalent diameter is 411.0 +/- 7.3 km. This diameter is compatible with the equivalent diameter for Huya obtained from radiometric techniques (D = 406 +/- 16 km). From this instantaneous limb, we obtained the geometric albedo for Huya (p(V) = 0.079 +/- 0.004) and we explored possible three-dimensional shapes and constraints to the mass density for this TNO. We did not detect the satellite of Huya through this occultation, but the presence of rings or debris around Huya was constrained using the occultation data. We also derived an upper limit for a putative Pluto-like global atmosphere of about p(surf) = 10 nbar. | |
dc.language | eng | |
dc.publisher | Edp Sciences S A | |
dc.relation | Astronomy & Astrophysics | |
dc.source | Web of Science | |
dc.subject | Kuiper belt objects | |
dc.subject | Individual | |
dc.subject | Huya | |
dc.subject | Methods | |
dc.subject | Observational | |
dc.subject | Techniques | |
dc.subject | Photometric | |
dc.title | Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation | |
dc.type | Artículos de revistas | |