X-Ray Flashes on Helium Novae
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866917772151226368 |
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| author | Kato, Mariko Hachisu, Izumi |
| author_facet | Kato, Mariko Hachisu, Izumi |
| contents | A helium nova occurs on a white dwarf (WD) accreting hydrogen-deficient matter from a helium star companion. When the mass of a helium envelope on the WD reaches a critical value, unstable helium burning ignites to trigger a nova outburst. A bright soft X-ray phase appears in an early outbursting phase of a helium nova before it optically rises toward maximum. Such an X-ray bright phase is called the X-ray flash. We present theoretical light curves of X-ray flashes for 1.0, 1.2, and 1.35 $M_\odot$ helium novae with mass accretion rates of $(1.6-7.5) \times 10^{-7}~M_\odot$ yr$^{-1}$. Long durations of the X-ray flashes (100 days to 10 years) and high X-ray luminosities ($\sim 10^{38}$ erg s$^{-1}$) indicate that X-ray flashes are detectable as a new type of X-ray transients or persistent X-ray sources. An X-ray flash is a precursor of optical brightening, so that the detection of X-ray flashes on helium novae enables us to plan arranged observation for optical pre-maximum phases that have been one of the frontiers of nova study. We found a candidate object of helium-burning X-ray flash from literature on extra-galactic X-ray surveys. This X-ray transient source is consistent with our X-ray flash model of a $1.35 ~M_\odot$ WD. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_02947 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | X-Ray Flashes on Helium Novae Kato, Mariko Hachisu, Izumi Solar and Stellar Astrophysics High Energy Astrophysical Phenomena A helium nova occurs on a white dwarf (WD) accreting hydrogen-deficient matter from a helium star companion. When the mass of a helium envelope on the WD reaches a critical value, unstable helium burning ignites to trigger a nova outburst. A bright soft X-ray phase appears in an early outbursting phase of a helium nova before it optically rises toward maximum. Such an X-ray bright phase is called the X-ray flash. We present theoretical light curves of X-ray flashes for 1.0, 1.2, and 1.35 $M_\odot$ helium novae with mass accretion rates of $(1.6-7.5) \times 10^{-7}~M_\odot$ yr$^{-1}$. Long durations of the X-ray flashes (100 days to 10 years) and high X-ray luminosities ($\sim 10^{38}$ erg s$^{-1}$) indicate that X-ray flashes are detectable as a new type of X-ray transients or persistent X-ray sources. An X-ray flash is a precursor of optical brightening, so that the detection of X-ray flashes on helium novae enables us to plan arranged observation for optical pre-maximum phases that have been one of the frontiers of nova study. We found a candidate object of helium-burning X-ray flash from literature on extra-galactic X-ray surveys. This X-ray transient source is consistent with our X-ray flash model of a $1.35 ~M_\odot$ WD. |
| title | X-Ray Flashes on Helium Novae |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2408.02947 |