X-ray and gamma-ray study for 2023 nova eruption of V1716 Sco
| Autor: | Wang, H. -H., Yan, H. -D., Takata, J., Lin, L. C. -C. |
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| Rok vydání: | 2024 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| Popis: | We report the results of X-ray and gamma-ray analyses of the nova V1716 Sco taken by Swift, NICER, NuSTAR and F ermi-LAT. We have detected gamma-ray emission at a significant level exceeding 8 {\sigma} in daily bins starting the day after the optical eruption. The gamma-ray emission, characterized by a Test Statistic (TS) value more than four, persisted for approximately 40 days. Notably, harder X-ray emission were observed by NuSTAR as the start of gamma-ray emission, which is the fourth classical nova that gamma-ray emission is concurrent with harder X-ray emission from NuSTAR data. V1716 Sco is one of rare samples that clearly shows a hard X-ray emission (1-10 keV bands) in the Swift-XRT data concurrently with gamma-ray emission of Fermi-LAT data, and its light curve in 1.0-10.0 keV bands had a peak at about 20 days after the optical eruption. The X-ray spectrum was initially fitted by a model of thermal plasma emission, and entered a supersoft phase with additional blackbody (BB) component emerged around about 40 days after the optical eruption. NICER data taken in supersoft source phase revealed a quasi-periodic oscillation with a period of 79.10+-1.98 seconds, and the peak phase of the folded light curve varied with time. Moreover, V1716 Sco is the another example that the emission radius in supersoft source phase is significantly larger than the radius of white dwarf, and a simple BB emission model may not be applicable since the luminosity exceeds significantly Eddington limit. Comment: 16 pages,13 figures,submitted to AAS Journals. arXiv admin note: text overlap with arXiv:2404.08409 |
| Databáze: | arXiv |
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