dc.date.accessioned | 2020-05-22T19:04:06Z | |
dc.date.available | 2020-05-22T19:04:06Z | |
dc.date.created | 2020-01-27T15:31:48Z | |
dc.date.issued | 2019 | |
dc.identifier.citation | Jewitt, David Luu, Jane . Initial Characterization of Interstellar Comet 2I/2019 Q4 (Borisov). Astrophysical Journal Letters. 2019, 886(2) | |
dc.identifier.uri | http://hdl.handle.net/10852/76111 | |
dc.description.abstract | We present initial observations of the interstellar body 2I/(2019 Q4) Borisov taken to determine its nature prior to the perihelion in 2019 December. Images from the Nordic Optical Telescope show a prominent, morphologically stable dust coma and tail. The dust cross-section within 15,000 km of the nucleus averages 130 km2 (assuming geometric albedo 0.1) and increases by about 1% per day. If sustained, this rate indicates that the comet has been active for ~100 days prior to the observations. Cometary activity thus started in 2019 June, at which time C/Borisov was at ~4.5 au from the Sun, a typical distance for the onset of water ice sublimation in comets. The dust optical colors, B − V = 0.80 ± 0.05, V − R = 0.47 ± 0.03 and R− I = 0.49 ± 0.05, are identical to those of a sample of (solar system) long-period comets. The colors are similar to those of 1I/(2017 U1) 'Oumuamua, indicating a lack of the ultrared matter that is common in the Kuiper Belt, on both interstellar objects. The effective size of the dust particles is estimated as $\overline{a}$ = 100 μm, based on the length of the dust tail and the 100 day lifetime. With this size, the ejected dust mass is of order 1.3 × 107 kg and the current dust mass loss rate ~2 kg s−1. We set an upper limit to the nucleus radius using photometry at r n ≤3.8 km (again for albedo 0.1) and we use a statistical argument to show that the nucleus must be much smaller, likely a few hundred meters in radius. | en_US |
dc.language | EN | |
dc.publisher | Institute of Physics Publishing Ltd. | |
dc.title | Initial Characterization of Interstellar Comet 2I/2019 Q4 (Borisov) | en_US |
dc.type | Journal article | en_US |
dc.creator.author | Jewitt, David | |
dc.creator.author | Luu, Jane | |
cristin.unitcode | 185,15,22,40 | |
cristin.unitname | Senter for Jordens utvikling og dynamikk | |
cristin.ispublished | true | |
cristin.fulltext | original | |
cristin.qualitycode | 2 | |
dc.identifier.cristin | 1783341 | |
dc.identifier.bibliographiccitation | info:ofi/fmt:kev:mtx:ctx&ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astrophysical Journal Letters&rft.volume=886&rft.spage=&rft.date=2019 | |
dc.identifier.jtitle | Astrophysical Journal Letters | |
dc.identifier.volume | 886 | |
dc.identifier.issue | 2 | |
dc.identifier.pagecount | 6 | |
dc.identifier.doi | https://doi.org/10.3847/2041-8213/ab530b | |
dc.identifier.urn | URN:NBN:no-79210 | |
dc.type.document | Tidsskriftartikkel | en_US |
dc.type.peerreviewed | Peer reviewed | |
dc.source.issn | 2041-8205 | |
dc.identifier.fulltext | Fulltext https://www.duo.uio.no/bitstream/handle/10852/76111/1/Jewitt_2019_ApJL_886_L29.pdf | |
dc.type.version | PublishedVersion | |
cristin.articleid | L29 | |