Evolution of the inner accretion flow and the white-dwarf spin pulse during the 2023 outburst in GK Persei
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arXiv
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| Natura: | Preprint |
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2025
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| author | Kimura, Mariko Hayashi, Takayuki Wada, Yuuki Iwakiri, Wataru Sako, Shigeyuki Veresvarska, Martina Scaringi, Simone Castro-Segura, Noel Knigge, Christian Gendreau, Keith C. Arzoumanian, Zaven |
| author_facet | Kimura, Mariko Hayashi, Takayuki Wada, Yuuki Iwakiri, Wataru Sako, Shigeyuki Veresvarska, Martina Scaringi, Simone Castro-Segura, Noel Knigge, Christian Gendreau, Keith C. Arzoumanian, Zaven |
| contents | We present our X-ray and optical observations performed by NICER, NuSTAR, and Tomo-e Gozen during the 2023 outburst in the intermediate polar GK Persei. The X-ray spectrum consisted of three components: blackbody emission of several tens of eVs from the irradiated white-dwarf surface, a source possibly including several emission lines around 1 keV, and multi-temperature bremsstrahlung emission from the accretion column. The 351.3-s white-dwarf spin pulse was detected in X-rays, and the observable X-ray flux from the column drastically decreased at the off-pulse phase, which suggests that the absorption of the column by the accreting gas called the curtain was the major cause of the pulse. As the system became brighter in optical, the column became fainter, the pulse amplitude became higher, and the energy dependence of pulses became weaker at $<$8~keV. These phenomena could be explained by the column's more pronounced absorption by the denser curtain as mass accretion rates increased. The blackbody and line fluxes rapidly decreased at the optical decline, which suggests the expansion of the innermost disk edge with decreasing accretion rates. The electron scattering or the column geometry may be associated with almost no energy dependence of high-energy pulses. The irradiated vertically-thick structure at the disk may generate optical QPOs with a period of $\sim$5700 s. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_21313 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Evolution of the inner accretion flow and the white-dwarf spin pulse during the 2023 outburst in GK Persei Kimura, Mariko Hayashi, Takayuki Wada, Yuuki Iwakiri, Wataru Sako, Shigeyuki Veresvarska, Martina Scaringi, Simone Castro-Segura, Noel Knigge, Christian Gendreau, Keith C. Arzoumanian, Zaven High Energy Astrophysical Phenomena We present our X-ray and optical observations performed by NICER, NuSTAR, and Tomo-e Gozen during the 2023 outburst in the intermediate polar GK Persei. The X-ray spectrum consisted of three components: blackbody emission of several tens of eVs from the irradiated white-dwarf surface, a source possibly including several emission lines around 1 keV, and multi-temperature bremsstrahlung emission from the accretion column. The 351.3-s white-dwarf spin pulse was detected in X-rays, and the observable X-ray flux from the column drastically decreased at the off-pulse phase, which suggests that the absorption of the column by the accreting gas called the curtain was the major cause of the pulse. As the system became brighter in optical, the column became fainter, the pulse amplitude became higher, and the energy dependence of pulses became weaker at $<$8~keV. These phenomena could be explained by the column's more pronounced absorption by the denser curtain as mass accretion rates increased. The blackbody and line fluxes rapidly decreased at the optical decline, which suggests the expansion of the innermost disk edge with decreasing accretion rates. The electron scattering or the column geometry may be associated with almost no energy dependence of high-energy pulses. The irradiated vertically-thick structure at the disk may generate optical QPOs with a period of $\sim$5700 s. |
| title | Evolution of the inner accretion flow and the white-dwarf spin pulse during the 2023 outburst in GK Persei |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2504.21313 |