Swift unveils the orbital period of IGR J18214-1318
| Autor: | Giancarlo Cusumano, A. Segreto, Antonino D'Ai, V. La Parola, M. Del Santo |
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| Rok vydání: | 2020 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics 010308 nuclear & particles physics Astrophysics::High Energy Astrophysical Phenomena media_common.quotation_subject FOS: Physical sciences Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Star (graph theory) Type (model theory) Orbital period 01 natural sciences Neutron star Space and Planetary Science Observatory 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics Absorption (logic) Eccentricity (behavior) Astrophysics - High Energy Astrophysical Phenomena 010303 astronomy & astrophysics media_common Eclipse |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 498:2750-2756 |
| ISSN: | 1365-2966 0035-8711 |
| Popis: | We analysed 13 years of the Neil Gehrels Swift Observatory survey data collected on the High Mass X-ray Binary IGR J18214-1318. Performing the timing analysis we detected a periodic signal of 5.42 d. From the companion star characteristics we derived an average orbital separation of $\sim 41 \rm R_{\odot}\simeq 2 R_{\star}$. The spectral type of the companion star (O9) and the tight orbital separation suggest that IGR~J18214-1318 is a wind accreting source with eccentricity lower than 0.17. The intensity profile folded at the orbital period shows a deep minimum compatible with an eclipse of the source by the companion star. In addition, we report on the broad-band 0.6--100 keV spectrum using data from XMM-Newton, NuSTAR, and Swift, applying self-consistent physical models. We find that the spectrum is well fitted either by a pure thermal Comptonization component, or, assuming that the source is a neutron star accreting above the critical regime, by a combined thermal and bulk-motion Comptonization model. In both cases, the presence of a local neutral absorption (possibly related to the thick wind of the companion star) is required. Comment: 7 pages, 7 figures. Accepted by MNRAS on 2020-08-17 |
| Databáze: | OpenAIRE |
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