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http://hdl.handle.net/2289/7929Full metadata record
| DC Field | Value | Language |
|---|---|---|
| dc.contributor.author | Dutta, Anirban | - |
| dc.contributor.author | Rana, Vikram | - |
| dc.date.accessioned | 2022-04-28T05:51:33Z | - |
| dc.date.available | 2022-04-28T05:51:33Z | - |
| dc.date.issued | 2022-04 | - |
| dc.identifier.citation | Monthly Notices of the Royal Astronomical Society, 2022, Vol. 511, p4981 | en_US |
| dc.identifier.issn | 0035-8711 | - |
| dc.identifier.issn | 1365-2966 (Online) | - |
| dc.identifier.uri | http://hdl.handle.net/2289/7929 | - |
| dc.description | Restricted Access. An open-access version is available at arXiv.org (one of the alternative locations) | en_US |
| dc.description.abstract | We present a simultaneous broad-band analysis of X-ray data obtained with the XMM–Newton and the Nuclear Spectroscopic Telescope Array (NuSTAR) for the asynchronous polar source, CD Ind. The spin-folded light curve in the soft 0.3–3.0 keV band shows a single broad hump-like structure superimposed with occasional narrow dips, indicating a single-pole accretion model with a complex intrinsic absorber. Lack of strong modulation in the folded light curve above 3 keV reveals that emission from the corresponding zone of the post-shock region (PSR) remains in view throughout the spin phase. The broad-band spectrum is modelled with a three-component absorbed plasma emission model and absorbed isobaric cooling flow model, both of which fit the data well with similar statistical significance. The presence of a partial covering absorber is evident in the spectra with equivalent column density ∼7×1022cm−2 and a covering fraction of ~25 per cent. Strong ionized oxygen Kα line emission is detected in the spectra. We notice spectral variability during the spin phase 0.75–1.05, when there is a considerable increase in the column density of the overall absorber (from ∼1×1020cm−2 to ∼9×1020cm−2). We required at least three plasma temperatures to describe the multitemperature nature of the PSR. The shock temperature ∼43.3+3.8−3.4 keV, represented by the upper temperature of the cooling flow model, implies a white dwarf mass of ∼0.87+0.04−0.03M⊙. The iron Kα line complex show strong He-like and weak neutral fluorescence lines. We could not unambiguously detect the presence of Compton reflection in the spectra, which is probably very small and signifies a tall shock height. | en_US |
| dc.language.iso | en | en_US |
| dc.publisher | Oxford University Press on behalf of the Royal Astronomical Society | en_US |
| dc.relation.uri | A broad-band X-ray study of the asynchronous polar CD Ind | en_US |
| dc.relation.uri | https://arxiv.org/abs/2201.12334 | en_US |
| dc.relation.uri | https://doi.org/10.1093/mnras/stac296 | en_US |
| dc.rights | 2022 The Author(s) | en_US |
| dc.subject | accretion | en_US |
| dc.subject | accretion discs | en_US |
| dc.subject | stars: individual: EUVE J2115–58.6 | en_US |
| dc.subject | stars: individual: RX J2115.7–5840 | en_US |
| dc.subject | novae | en_US |
| dc.subject | cataclysmic variables | en_US |
| dc.subject | white dwarfs | en_US |
| dc.title | A broad-band X-ray study of the asynchronous polar CD Ind | en_US |
| dc.type | Article | en_US |
| Appears in Collections: | Research Papers (A&A) | |
Files in This Item:
| File | Description | Size | Format | |
|---|---|---|---|---|
| 2022_MNRAS_511_p4981.pdf Restricted Access | Restricted Access | 1.02 MB | Adobe PDF | View/Open Request a copy |
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