Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/27295
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Posselt, B. | en_US |
dc.contributor.author | Pavlov, G. G. | en_US |
dc.contributor.author | Slane, P. O. | en_US |
dc.contributor.author | Romani, R. | en_US |
dc.contributor.author | BUCCIANTINI, NICCOLO' | en_US |
dc.contributor.author | Bykov, A. M. | en_US |
dc.contributor.author | Kargaltsev, O. | en_US |
dc.contributor.author | Weisskopf, M. C. | en_US |
dc.contributor.author | Ng, C.-Y. | en_US |
dc.date.accessioned | 2020-09-10T15:06:03Z | - |
dc.date.available | 2020-09-10T15:06:03Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27295 | - |
dc.description.abstract | We report on six new Chandra observations of the Geminga pulsar wind nebula (PWN). The PWN consists of three distinct elongated structures—two ≈ 0.2{d}250 pc long lateral tails and a segmented axial tail of ≈ 0.05{d}250 pc length, where {d}250=d/(250 {pc}). The photon indices of the power-law spectra of the lateral tails, {{Γ }}≈ 1, are significantly harder than those of the pulsar ({{Γ }}≈ 1.5) and the axial tail ({{Γ }}≈ 1.6). There is no significant diffuse X-ray emission between the lateral tails—the ratio of the X-ray surface brightness between the south tail and this sky area is at least 12. The lateral tails apparently connect directly to the pulsar and show indications of moving footpoints. The axial tail comprises time-variable emission blobs. However, there is no evidence for constant or decelerated outward motion of these blobs. Different physical models are consistent with the observed morphology and spectra of the Geminga PWN. In one scenario, the lateral tails could represent an azimuthally asymmetric shell whose hard emission is caused by the Fermi acceleration mechanism of colliding winds. In another scenario, the lateral tails could be luminous, bent polar outflows, while the blobs in the axial tail could represent a crushed torus. In a resemblance to planetary magnetotails, the blobs of the axial tail might also represent short-lived plasmoids, which are formed by magnetic field reconnection in the relativistic plasma of the pulsar wind tail. | en_US |
dc.language.iso | eng | en_US |
dc.title | Geminga’s Puzzling Pulsar Wind Nebula | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/835/1/66 | en_US |
dc.identifier.scopus | 2-s2.0-85011277942 | en_US |
dc.identifier.isi | 000393455400066 | en_US |
dc.identifier.url | https://arxiv.org/abs/1611.03496 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/835/1/66 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 835 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 66 | 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 | USA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017ApJ...835...66P | 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.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0002-8848-1392 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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Posselt_2017_ApJ_835_66(1).pdf | Pdf editoriale | 2.74 MB | Adobe PDF | View/Open |
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