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.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
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 |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
aa44637-22.pdf | Pdf editoriale | 1.46 MB | Adobe PDF | View/Open |
Page view(s)
44
checked on Sep 11, 2024
Download(s)
17
checked on Sep 11, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.