Light-curve analysis of the classical nova YZ Ret: revisit with fully self-consistent nova outburst models
Abstract
YZ Ret is a well observed nova from the first detection of an X-ray flash phase in classical novae until the end of a supersoft X-ray source phase. We have reanalyzed multiwavelength light curves of YZ Ret over the total duration of the outburst. Our fully self-consistent nova outburst model, a 1.25 M⊙ white dwarf (WD) and a mass accretion rate of 1× 10−9 M⊙ yr−1 on to the WD, reasonably reproduced V/g light curves as well as the very early X-ray flash and late supersoft X-ray light curves. This model explains the emergence epoch of the GeV gamma-ray emission because a shock naturally arises far outside the nova (WD) photosphere just after the optical maximum. In our model, before optical maximum, later ejected matter has a smaller velocity than that of earlier ejecta and therefore the ejecta expands while, after optical maximum, later ejected matter has a larger velocity than that of earlier ejecta and collision with the earlier ejecta makes a shock.
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BibTeX
@misc{hachisu2026lightcurve,
title = {{Light-curve analysis of the classical nova YZ Ret: revisit with fully self-consistent nova outburst models}},
author = {Izumi Hachisu and Mariko Kato},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.27029},
eprint = {2609.27029},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.27029},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Light-curve analysis of the classical nova YZ Ret: revisit with fully self-consistent nova outburst models
AU - Izumi Hachisu
AU - Mariko Kato
PY - 2026
DA - 2026/09/22
PB - arXiv
DO - 10.48550/arxiv.2609.27029
UR - https://arxiv.org/abs/2609.27029
AB - YZ Ret is a well observed nova from the first detection of an X-ray flash phase in classical novae until the end of a supersoft X-ray source phase. We have reanalyzed multiwavelength light curves of YZ Ret over the total duration of the outburst. Our fully self-consistent nova outburst model, a 1.25 M_⊙ white dwarf (WD) and a mass accretion rate of 1× 10^−9 M_⊙ yr^−1 on to the WD, reasonably reproduced V/g light curves as well as the very early X-ray flash and late supersoft X-ray light curves. This model explains the emergence epoch of the GeV gamma-ray emission because a shock naturally arises far outside the nova (WD) photosphere just after the optical maximum. In our model, before optical maximum, later ejected matter has a smaller velocity than that of earlier ejecta and therefore the ejecta expands while, after optical maximum, later ejected matter has a larger velocity than that of earlier ejecta and collision with the earlier ejecta makes a shock.
ER -