Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/32047
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Bulla, M. | en_US |
dc.contributor.author | Kyutoku, K. | en_US |
dc.contributor.author | Tanaka, M. | en_US |
dc.contributor.author | COVINO, Stefano | en_US |
dc.contributor.author | Bruten, J. R. | en_US |
dc.contributor.author | Matsumoto, T. | en_US |
dc.contributor.author | Maund, J. R. | en_US |
dc.contributor.author | TESTA, Vincenzo | en_US |
dc.contributor.author | Wiersema, K. | en_US |
dc.date.accessioned | 2022-03-29T13:48:16Z | - |
dc.date.available | 2022-03-29T13:48:16Z | - |
dc.date.issued | 2021 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32047 | - |
dc.description.abstract | We predict linear polarization for a radioactively-powered kilonova following the merger of a black hole and a neutron star. Specifically, we perform 3-D Monte Carlo radiative transfer simulations for two different models, both featuring a lanthanide-rich dynamical ejecta component from numerical-relativity simulations while only one including an additional lanthanide-free disk wind component. We calculate polarization spectra for nine different orientations at 1.5, 2.5 and 3.5 d after the merger and in the $0.1-2\,\mu$m wavelength range. We find that both models are polarized at a detectable level 1.5 d after the merger while show negligible levels thereafter. The polarization spectra of the two models are significantly different. The model lacking a disk wind shows no polarization in the optical, while a signal increasing at longer wavelengths and reaching $\sim1\%-6\%$ at $2\,\mu$m depending on the orientation. The model with a disk-wind component, instead, features a characteristic "double-peak" polarization spectrum with one peak in the optical and the other in the infrared. Polarimetric observations of future events will shed light on the debated neutron richness of the disk-wind component. The detection of optical polarization would unambiguously reveal the presence of a lanthanide-free disk-wind component, while polarization increasing from zero in the optical to a peak in the infrared would suggest a lanthanide-rich composition for the whole ejecta. Future polarimetric campaigns should prioritize observations in the first $\sim48$ hours and in the $0.5-2\,\mu$m range, where polarization is strongest, but also explore shorter wavelengths/later times where no signal is expected from the kilonova and the interstellar polarization can be safely estimated. | en_US |
dc.language.iso | eng | en_US |
dc.title | Polarized kilonovae from black hole-neutron star mergers | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/staa3796 | en_US |
dc.identifier.scopus | 2-s2.0-85100248606 | en_US |
dc.identifier.url | http://arxiv.org/abs/2009.07279v2 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/501/2/1891/6030051?login=true | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 501 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 1891 | en_US |
dc.relation.lastpage | 1899 | en_US |
dc.relation.numberofpages | 9 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 9 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | JPN | en_US |
dc.contributor.country | SWE | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2021MNRAS.501.1891B | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_11 Relativistic astrophysics | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0001-9078-5507 | - |
crisitem.author.orcid | 0000-0003-1033-1340 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
staa3796.pdf | Pdf editoriale | 1.84 MB | Adobe PDF | View/Open |
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