Modeling X-ray reflection spectra from returning radiation: application to 4U 1630$-$47
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arXiv
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| Autori principali: | , , , , , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2026
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| _version_ | 1866915743416713216 |
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| author | Kourmpetis, Kostas Riaz, Shafqat Liu, Honghui Mirzaev, Temurbek Bambi, Cosimo Das, Debtroy Jiang, Jiachen Kokkotas, Kostas D. Santangelo, Andrea |
| author_facet | Kourmpetis, Kostas Riaz, Shafqat Liu, Honghui Mirzaev, Temurbek Bambi, Cosimo Das, Debtroy Jiang, Jiachen Kokkotas, Kostas D. Santangelo, Andrea |
| contents | Returning radiation is thought to play a key role in disk illumination of black hole X-ray binaries in the high-soft state, yet it has not been fully incorporated into XSPEC reflection models. We present a new table model for reflection spectroscopy that, for the first time, self-consistently accounts for the returning radiation. To isolate this effect, we adopt the standard disk-corona configuration but disable the corona, allowing the reflection spectrum to be produced solely by self-irradiation of the disk. Applying our model to the black hole X-ray binary 4U 1630$-$47, we report a rapidly spinning black hole ($a_* \sim 0.99$), a disk inclination of $i \sim 53^\circ$, a mass accretion rate of $\dot{M}_{\rm BH} \sim 15\% \, {\rm \dot{M}_{Edd}}$, and an electron density of $n_{\rm e} \sim 10^{21} \,\mathrm{cm^{-3}}$ to reproduce the observed reflection features. The model also yields a source distance of $D\sim 8.2 \, {\rm kpc}$, slightly below the commonly adopted value of $10 \, {\rm kpc}$ in the literature. Compared to the widely used relxillNS, our model naturally produces a harder high-energy reflection spectrum, fitting the data without invoking a Comptonized component. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2601_14860 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Modeling X-ray reflection spectra from returning radiation: application to 4U 1630$-$47 Kourmpetis, Kostas Riaz, Shafqat Liu, Honghui Mirzaev, Temurbek Bambi, Cosimo Das, Debtroy Jiang, Jiachen Kokkotas, Kostas D. Santangelo, Andrea High Energy Astrophysical Phenomena Returning radiation is thought to play a key role in disk illumination of black hole X-ray binaries in the high-soft state, yet it has not been fully incorporated into XSPEC reflection models. We present a new table model for reflection spectroscopy that, for the first time, self-consistently accounts for the returning radiation. To isolate this effect, we adopt the standard disk-corona configuration but disable the corona, allowing the reflection spectrum to be produced solely by self-irradiation of the disk. Applying our model to the black hole X-ray binary 4U 1630$-$47, we report a rapidly spinning black hole ($a_* \sim 0.99$), a disk inclination of $i \sim 53^\circ$, a mass accretion rate of $\dot{M}_{\rm BH} \sim 15\% \, {\rm \dot{M}_{Edd}}$, and an electron density of $n_{\rm e} \sim 10^{21} \,\mathrm{cm^{-3}}$ to reproduce the observed reflection features. The model also yields a source distance of $D\sim 8.2 \, {\rm kpc}$, slightly below the commonly adopted value of $10 \, {\rm kpc}$ in the literature. Compared to the widely used relxillNS, our model naturally produces a harder high-energy reflection spectrum, fitting the data without invoking a Comptonized component. |
| title | Modeling X-ray reflection spectra from returning radiation: application to 4U 1630$-$47 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2601.14860 |