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 |
|