{"title":"新星爆发物理学:1.2 M⊙和 1.3 M⊙白矮星上带有光学厚风的经典新星爆发理论模型","authors":"Mariko Kato, Hideyuki Saio, Izumi Hachisu","doi":"10.1093/pasj/psae038","DOIUrl":null,"url":null,"abstract":"We present time-dependent nova outburst models with optically thick winds for 1.2 and 1.35$\\, M_{\\odot }$ white dwarfs (WDs) with a mass-accretion rate of $5 \\times 10^{-9}\\, M_{\\odot }$ yr−1 and for a 1.3$\\, M_{\\odot }$ WD with $2 \\times 10^{-9}\\, M_{\\odot }$ yr−1. The X-ray flash occurs 11 d before the optical peak of the 1.2$\\, M_{\\odot }$ WD and 2.5 d before the peak of the 1.3$\\, M_{\\odot }$ WD. The wind mass-loss rate of the 1.2$\\, M_{\\odot }$ WD (1.3$\\, M_{\\odot }$ WD) reaches a peak of $6.4 \\times 10^{-5}\\, M_{\\odot }$ yr−1 ($7.4 \\times 10^{-5}\\, M_{\\odot }$ yr−1) at the epoch of the maximum photospheric expansion with the lowest photospheric temperature of log Tph (K) = 4.33 (4.35). The nuclear energy generated during the outburst is lost in the form of radiation (61% for the 1.2$\\, M_{\\odot }$ WD; 47% for the 1.3$\\, M_{\\odot }$ WD), gravitational energy of ejecta (39%; 52%), and kinetic energy of the wind (0.28%; 0.29%). We found an empirical relation for fast novae between the time to optical maximum from the outburst tpeak and the expansion timescale τexp. With this relation, we are able to predict the time to optical maximum tpeak from the ignition model (at t = 0) without following a time-consuming nova wind evolution.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":null,"pages":null},"PeriodicalIF":2.2000,"publicationDate":"2024-05-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Physics of nova outbursts: Theoretical models of classical nova outbursts with optically thick winds on 1.2 M⊙ and 1.3 M⊙ white dwarfs\",\"authors\":\"Mariko Kato, Hideyuki Saio, Izumi Hachisu\",\"doi\":\"10.1093/pasj/psae038\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"We present time-dependent nova outburst models with optically thick winds for 1.2 and 1.35$\\\\, M_{\\\\odot }$ white dwarfs (WDs) with a mass-accretion rate of $5 \\\\times 10^{-9}\\\\, M_{\\\\odot }$ yr−1 and for a 1.3$\\\\, M_{\\\\odot }$ WD with $2 \\\\times 10^{-9}\\\\, M_{\\\\odot }$ yr−1. The X-ray flash occurs 11 d before the optical peak of the 1.2$\\\\, M_{\\\\odot }$ WD and 2.5 d before the peak of the 1.3$\\\\, M_{\\\\odot }$ WD. The wind mass-loss rate of the 1.2$\\\\, M_{\\\\odot }$ WD (1.3$\\\\, M_{\\\\odot }$ WD) reaches a peak of $6.4 \\\\times 10^{-5}\\\\, M_{\\\\odot }$ yr−1 ($7.4 \\\\times 10^{-5}\\\\, M_{\\\\odot }$ yr−1) at the epoch of the maximum photospheric expansion with the lowest photospheric temperature of log Tph (K) = 4.33 (4.35). The nuclear energy generated during the outburst is lost in the form of radiation (61% for the 1.2$\\\\, M_{\\\\odot }$ WD; 47% for the 1.3$\\\\, M_{\\\\odot }$ WD), gravitational energy of ejecta (39%; 52%), and kinetic energy of the wind (0.28%; 0.29%). We found an empirical relation for fast novae between the time to optical maximum from the outburst tpeak and the expansion timescale τexp. With this relation, we are able to predict the time to optical maximum tpeak from the ignition model (at t = 0) without following a time-consuming nova wind evolution.\",\"PeriodicalId\":20733,\"journal\":{\"name\":\"Publications of the Astronomical Society of Japan\",\"volume\":null,\"pages\":null},\"PeriodicalIF\":2.2000,\"publicationDate\":\"2024-05-09\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Publications of the Astronomical Society of Japan\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://doi.org/10.1093/pasj/psae038\",\"RegionNum\":4,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q2\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Publications of the Astronomical Society of Japan","FirstCategoryId":"101","ListUrlMain":"https://doi.org/10.1093/pasj/psae038","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
Physics of nova outbursts: Theoretical models of classical nova outbursts with optically thick winds on 1.2 M⊙ and 1.3 M⊙ white dwarfs
We present time-dependent nova outburst models with optically thick winds for 1.2 and 1.35$\, M_{\odot }$ white dwarfs (WDs) with a mass-accretion rate of $5 \times 10^{-9}\, M_{\odot }$ yr−1 and for a 1.3$\, M_{\odot }$ WD with $2 \times 10^{-9}\, M_{\odot }$ yr−1. The X-ray flash occurs 11 d before the optical peak of the 1.2$\, M_{\odot }$ WD and 2.5 d before the peak of the 1.3$\, M_{\odot }$ WD. The wind mass-loss rate of the 1.2$\, M_{\odot }$ WD (1.3$\, M_{\odot }$ WD) reaches a peak of $6.4 \times 10^{-5}\, M_{\odot }$ yr−1 ($7.4 \times 10^{-5}\, M_{\odot }$ yr−1) at the epoch of the maximum photospheric expansion with the lowest photospheric temperature of log Tph (K) = 4.33 (4.35). The nuclear energy generated during the outburst is lost in the form of radiation (61% for the 1.2$\, M_{\odot }$ WD; 47% for the 1.3$\, M_{\odot }$ WD), gravitational energy of ejecta (39%; 52%), and kinetic energy of the wind (0.28%; 0.29%). We found an empirical relation for fast novae between the time to optical maximum from the outburst tpeak and the expansion timescale τexp. With this relation, we are able to predict the time to optical maximum tpeak from the ignition model (at t = 0) without following a time-consuming nova wind evolution.
期刊介绍:
Publications of the Astronomical Society of Japan (PASJ) publishes the results of original research in all aspects of astronomy, astrophysics, and fields closely related to them.