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dc.contributor.author | Martínez-Chicharro M. | |
dc.contributor.author | Grinberg V. | |
dc.contributor.author | Torrejón J.M. | |
dc.contributor.author | Schulz N. | |
dc.contributor.author | Oskinova L. | |
dc.contributor.author | Nowak M. | |
dc.contributor.author | Fürst F. | |
dc.contributor.author | Hell N. | |
dc.contributor.author | Hainich R. | |
dc.date.accessioned | 2022-02-09T20:31:54Z | |
dc.date.available | 2022-02-09T20:31:54Z | |
dc.date.issued | 2021 | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.uri | https://dspace.kpfu.ru/xmlui/handle/net/168797 | |
dc.description.abstract | We present an analysis of the first observation of the iconic high-mass X-ray binary 4U 1700-37 with the Chandra High-Energy Transmission Gratings (HETGs) during an X-ray eclipse. The goal of the observation was to study the structure/physical conditions in the clumpy stellar wind through high-resolution spectroscopy. We find the following: (a) Emission-line brightness from K-shell transitions, corresponding to near-neutral species, directly correlates with continuum illumination. However, these lines do not greatly diminish during eclipse. This is readily explained if fluorescence K α emission comes from the bulk of the wind. (b) The highly ionized Fe xxv and Fe xxvi Ly α diminish during eclipse. Thus, they must be produced in the vicinity of the compact object where log ζ > 3. (c) To describe the emission-line spectrum, the sum of two self-consistent photoionization models with low ionization (log ζ ∼-1) and high ionization (log ζ ∼2.4) is required. From their emission measures, the clump-to-interclump density ratio can be estimated to be nc/ni ∼300. To fit the complex He-like Si xiii profile, the plasma requires a broadening with vbulk ∼840 km s-1. Reproducing the observed r ≈ f line fluxes requires the addition of a third collisionally ionized plasma. (d) Emission-line widths appear unresolved at the HETG resolution with the exception of silicon. There is no clear radial segregation between (quasi-)neutral and ionized species, consistent with cold wind clumps interspersed in a hot rarefied interclump medium. | |
dc.relation.ispartofseries | Monthly Notices of the Royal Astronomical Society | |
dc.subject | stars: individual 4U 1700-37 | |
dc.subject | stars: massive | |
dc.subject | X-rays: binaries | |
dc.title | High-resolution X-ray spectroscopy of supergiant HMXB 4U 1700-37 during the compact object eclipse | |
dc.type | Article | |
dc.relation.ispartofseries-issue | 4 | |
dc.relation.ispartofseries-volume | 501 | |
dc.collection | Публикации сотрудников КФУ | |
dc.relation.startpage | 5646 | |
dc.source.id | SCOPUS00358711-2021-501-4-SID85100781426 |