Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/29874
Campo DC | Valore | Lingua |
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dc.contributor.author | Panasenco, Olga | en_US |
dc.contributor.author | VELLI, MARCO | en_US |
dc.contributor.author | D'AMICIS, RAFFAELLA | en_US |
dc.contributor.author | Shi, Chen | en_US |
dc.contributor.author | Réville, Victor | en_US |
dc.contributor.author | Bale, Stuart D. | en_US |
dc.contributor.author | Badman, Samuel T. | en_US |
dc.contributor.author | Kasper, Justin | en_US |
dc.contributor.author | Korreck, Kelly | en_US |
dc.contributor.author | Bonnell, J. W. | en_US |
dc.contributor.author | Wit, Dudok de Thierry | en_US |
dc.contributor.author | Goetz, Keith | en_US |
dc.contributor.author | Harvey, Peter R. | en_US |
dc.contributor.author | MacDowall, Robert J. | en_US |
dc.contributor.author | Malaspina, David M. | en_US |
dc.contributor.author | Pulupa, Marc | en_US |
dc.contributor.author | Case, Anthony W. | en_US |
dc.contributor.author | Larson, Davin | en_US |
dc.contributor.author | Livi, Roberto | en_US |
dc.contributor.author | Stevens, Michael | en_US |
dc.contributor.author | Whittlesey, Phyllis | en_US |
dc.date.accessioned | 2021-01-20T13:17:25Z | - |
dc.date.available | 2021-01-20T13:17:25Z | - |
dc.date.issued | 2020 | en_US |
dc.identifier.issn | 0067-0049 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29874 | - |
dc.description.abstract | The magnetic field measurements of the FIELDS instrument on the Parker Solar Probe (PSP) have shown intensities, throughout its first solar encounter, that require a very low source surface (SS) height ( ${R}_{\mathrm{SS}}\leqslant 1.8\,{R}_{\odot }$ ) to be reconciled with magnetic field measurements at the Sun via potential field extrapolation (PFSS). However, during PSP's second encounter, the situation went back to a more classic SS height ( ${R}_{\mathrm{SS}}\leqslant 2.5\,{R}_{\odot }$ ). Here we use high-resolution observations of the photospheric magnetic field (Solar Dynamics Observatory/Helioseismic and Magnetic Imager) to calculate neutral lines and boundaries of the open field regions for SS heights from 1.2 to 2.5 R<SUB>☉</SUB> using an evolving PFSS model and the measured solar wind speed to trace the source of the wind observed by PSP to the low corona and photosphere. We adjust R<SUB>SS</SUB> to get the best match for the field polarity over the period 2018 October-November and 2019 March-April, finding that the best fit for the observed magnetic field polarity inversions requires a nonspherical SS. The geometry of the coronal hole boundaries for different R<SUB>SS</SUB> is tested using the PSP perihelion passes, 3D PFSS models, and LASCO/C2 observations. We investigate the sources of stronger-than-average magnetic fields and times of Alfvénic fast and slow wind. Only some of the strongly Alfvénic slow wind streams seen by PSP survive and are observed at 1 au: the origins and peculiar topology of the background in which they propagate is discussed. | en_US |
dc.language.iso | eng | en_US |
dc.title | Exploring Solar Wind Origins and Connecting Plasma Flows from the Parker Solar Probe to 1 au: Nonspherical Source Surface and Alfvénic Fluctuations | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4365/ab61f4 | en_US |
dc.identifier.scopus | 2-s2.0-85087164439 | en_US |
dc.identifier.isi | 000537499300003 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4365/ab61f4 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 246 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.numberofpages | 15 | en_US |
dc.relation.article | 54 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 21 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | USA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2020ApJS..246...54P | 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 | en_US |
dc.description.apc | sì | 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.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | embargo_20710101 | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.orcid | 0000-0003-2647-117X | - |
crisitem.journal.journalissn | 0067-0049 | - |
crisitem.journal.ance | E016254 | - |
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Panasenco_2020_ApJS_246_54.pdf | Pdf editoriale | 14.8 MB | Adobe PDF | Embargoed until 1 gennaio 2071 |
panasenco_apjs_preprint.pdf | preprint | 24.17 MB | Adobe PDF | Visualizza/apri |
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