Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/33969
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Illiano, G. | en_US |
dc.contributor.author | PAPITTO, ALESSANDRO | en_US |
dc.contributor.author | AMBROSINO, Filippo | en_US |
dc.contributor.author | Miraval Zanon, A. | en_US |
dc.contributor.author | Coti Zelati, F. | en_US |
dc.contributor.author | STELLA, Luigi | en_US |
dc.contributor.author | ZAMPIERI, Luca | en_US |
dc.contributor.author | Burtovoi, A. | en_US |
dc.contributor.author | CAMPANA, Sergio | en_US |
dc.contributor.author | CASELLA, Piergiorgio | en_US |
dc.contributor.author | Cecconi, M. | en_US |
dc.contributor.author | DE MARTINO, Domitilla | en_US |
dc.contributor.author | Fiori, M. | en_US |
dc.contributor.author | Ghedina, A. | en_US |
dc.contributor.author | Gonzales, M. | en_US |
dc.contributor.author | Hernandez Diaz, M. | en_US |
dc.contributor.author | ISRAEL, Gian Luca | en_US |
dc.contributor.author | LEONE, Francesco | en_US |
dc.contributor.author | Naletto, G. | en_US |
dc.contributor.author | Perez Ventura, H. | en_US |
dc.contributor.author | Riverol, C. | en_US |
dc.contributor.author | Riverol, L. | en_US |
dc.contributor.author | Torres, D. F. | en_US |
dc.contributor.author | Turchetta, M. | en_US |
dc.date.accessioned | 2023-03-03T10:41:43Z | - |
dc.date.available | 2023-03-03T10:41:43Z | - |
dc.date.issued | 2023 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/33969 | - |
dc.description.abstract | Context. PSR J1023+0038 is the first millisecond pulsar that was ever observed as an optical and UV pulsar. So far, it is the only optical transitional millisecond pulsar. The rotation- and accretion-powered emission mechanisms hardly individually explain the observed characteristics of optical pulsations. A synergistic model, combining these standard emission processes, was proposed to explain the origin of the X-ray/UV/optical pulsations. <BR /> Aims: We study the phase lag between the pulses in the optical and X-ray bands to gain insight into the physical mechanisms that cause it. <BR /> Methods: We performed a detailed timing analysis of simultaneous or quasi-simultaneous observations in the X-ray band, acquired with the XMM-Newton and NICER satellites, and in the optical band, with the fast photometers SiFAP2 (mounted at the 3.6 m Telescopio Nazionale Galileo) and Aqueye+ (mounted at the 1.8 m Copernicus Telescope). We estimated the time lag of the optical pulsation with respect to that in the X-rays by modeling the folded pulse profiles with two harmonic components. <BR /> Results: Optical pulses lag the X-ray pulses by ∼150 μs in observations acquired with instruments (NICER and Aqueye+) whose absolute timing uncertainty is much smaller than the measured lag. We also show that the phase lag between optical and X-ray pulsations lies in a limited range of values, δϕ ∈ (0 − 0.15), which is maintained over timescales of about five years. This indicates that both pulsations originate from the same region, and it supports the hypothesis of a common emission mechanism. Our results are interpreted in the shock-driven mini pulsar nebula scenario. This scenario suggests that optical and X-ray pulses are produced by synchrotron emission from the shock that formed within a few light cylinder radii away (∼100 km) from the pulsar, where its striped wind encounters the accretion disk inflow. | en_US |
dc.language.iso | eng | en_US |
dc.title | Investigating the origin of optical and X-ray pulsations of the transitional millisecond pulsar PSR J1023+0038 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/202244637 | en_US |
dc.identifier.scopus | 2-s2.0-85145772307 | en_US |
dc.identifier.url | http://arxiv.org/abs/2211.12975v1 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/pdf/2023/01/aa44637-22.pdf | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 669 | en_US |
dc.relation.firstpage | A26 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2023A&A...669A..26I | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering | 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 | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.orcid | 0000-0001-6289-7413 | - |
crisitem.author.orcid | 0000-0001-7915-996X | - |
crisitem.author.orcid | 0000-0002-0018-1687 | - |
crisitem.author.orcid | 0000-0002-6516-1329 | - |
crisitem.author.orcid | 0000-0001-6278-1576 | - |
crisitem.author.orcid | 0000-0002-0752-3301 | - |
crisitem.author.orcid | 0000-0002-5069-4202 | - |
crisitem.author.orcid | 0000-0001-5480-6438 | - |
crisitem.author.orcid | 0000-0001-7626-3788 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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aa44637-22.pdf | Pdf editoriale | 1.46 MB | Adobe PDF | View/Open |
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