A multiwavelength light curve analysis of the classical nova V392 Per: Optical contribution from an irradiated accretion disk during the nova wind phase
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arXiv
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| Natura: | Preprint |
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2025
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| _version_ | 1866912278557753344 |
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| author | Hachisu, Izumi Kato, Mariko |
| author_facet | Hachisu, Izumi Kato, Mariko |
| contents | The classical nova V392 Per 2018 is characterized by a very fast optical decline, long binary orbital period of 3.23 days, detection of GeV gamma rays, and almost identical decay trends of $B$, $V$, and $I_{\rm C}$ light curves. The last feature is unique because most novae develop strong emission lines in the nebular phase and these lines contribute especially to the $B$ and $V$ bands and make large differences between the $BV$ and $I_{\rm C}$ light curves. This unique feature can be understood if the optical flux is dominated by continuum until the late phase of the nova outburst. Such continuum radiation is emitted by a bright accretion disk irradiated by a hydrogen burning white dwarf (WD) and viscous heating disk with high mass-accretion rate after the hydrogen burning ended. We present a comprehensive nova outburst model that reproduces all of these light curves. We determined the WD mass to be $M_{\rm WD}=1.35$ - $1.37 ~M_\odot$ and the distance modulus in the $V$ band to be $(m-M)_V=14.6 \pm 0.2$; the distance is $d= 3.45\pm 0.5$ kpc for the reddening of $E(B-V)=0.62$. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2503_13384 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A multiwavelength light curve analysis of the classical nova V392 Per: Optical contribution from an irradiated accretion disk during the nova wind phase Hachisu, Izumi Kato, Mariko High Energy Astrophysical Phenomena Solar and Stellar Astrophysics The classical nova V392 Per 2018 is characterized by a very fast optical decline, long binary orbital period of 3.23 days, detection of GeV gamma rays, and almost identical decay trends of $B$, $V$, and $I_{\rm C}$ light curves. The last feature is unique because most novae develop strong emission lines in the nebular phase and these lines contribute especially to the $B$ and $V$ bands and make large differences between the $BV$ and $I_{\rm C}$ light curves. This unique feature can be understood if the optical flux is dominated by continuum until the late phase of the nova outburst. Such continuum radiation is emitted by a bright accretion disk irradiated by a hydrogen burning white dwarf (WD) and viscous heating disk with high mass-accretion rate after the hydrogen burning ended. We present a comprehensive nova outburst model that reproduces all of these light curves. We determined the WD mass to be $M_{\rm WD}=1.35$ - $1.37 ~M_\odot$ and the distance modulus in the $V$ band to be $(m-M)_V=14.6 \pm 0.2$; the distance is $d= 3.45\pm 0.5$ kpc for the reddening of $E(B-V)=0.62$. |
| title | A multiwavelength light curve analysis of the classical nova V392 Per: Optical contribution from an irradiated accretion disk during the nova wind phase |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2503.13384 |