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.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
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 |
Page view(s)
28
checked on Mar 28, 2024
Download(s)
10
checked on Mar 28, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.