Swift unveils the orbital period of IGR J18214-1318. (arXiv:2009.06500v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Cusumano_G/0/1/0/all/0/1">G. Cusumano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAi_A/0/1/0/all/0/1">A. D'Aì</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Segreto_A/0/1/0/all/0/1">A. Segreto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parola_V/0/1/0/all/0/1">V. La Parola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santo_M/0/1/0/all/0/1">M. Del Santo</a>
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.
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.
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