千新星at2017gfo中的碲发射谱线

Q1 Earth and Planetary Sciences
Kenta Hotokezaka, Masaomi Tanaka, Daiji Kato, Gediminas Gaigalas
{"title":"千新星at2017gfo中的碲发射谱线","authors":"Kenta Hotokezaka, Masaomi Tanaka, Daiji Kato, Gediminas Gaigalas","doi":"10.1093/mnrasl/slad128","DOIUrl":null,"url":null,"abstract":"ABSTRACT The late-time spectra of the kilonova AT 2017gfo associated with GW170817 exhibit a strong emission line feature at $2.1\\, {\\rm \\mu m}$. The line structure develops with time and there is no blueshifted absorption feature in the spectra, suggesting that this emission line feature is produced by electron collision excitation. We attribute the emission line to a fine structure line of Tellurium (Te) III, which is one of the most abundant elements in the second r-process peak. By using a synthetic spectral modelling including fine structure emission lines with the solar r-process abundance pattern beyond the first r-process peak, i.e. atomic mass numbers A ≳ 88, we demonstrate that [Te iii] $2.10\\, \\rm \\mu m$ is indeed expected to be the strongest emission line in the near infrared region. We estimate that the required mass of Te iii is ∼10−3 M⊙, corresponding to the merger ejecta of 0.05 M⊙, which is in agreement with the mass estimated from the kilonova light curve.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"1 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"2023-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"2","resultStr":"{\"title\":\"Tellurium emission line in kilonova AT 2017gfo\",\"authors\":\"Kenta Hotokezaka, Masaomi Tanaka, Daiji Kato, Gediminas Gaigalas\",\"doi\":\"10.1093/mnrasl/slad128\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"ABSTRACT The late-time spectra of the kilonova AT 2017gfo associated with GW170817 exhibit a strong emission line feature at $2.1\\\\, {\\\\rm \\\\mu m}$. The line structure develops with time and there is no blueshifted absorption feature in the spectra, suggesting that this emission line feature is produced by electron collision excitation. We attribute the emission line to a fine structure line of Tellurium (Te) III, which is one of the most abundant elements in the second r-process peak. By using a synthetic spectral modelling including fine structure emission lines with the solar r-process abundance pattern beyond the first r-process peak, i.e. atomic mass numbers A ≳ 88, we demonstrate that [Te iii] $2.10\\\\, \\\\rm \\\\mu m$ is indeed expected to be the strongest emission line in the near infrared region. We estimate that the required mass of Te iii is ∼10−3 M⊙, corresponding to the merger ejecta of 0.05 M⊙, which is in agreement with the mass estimated from the kilonova light curve.\",\"PeriodicalId\":18951,\"journal\":{\"name\":\"Monthly Notices of the Royal Astronomical Society: Letters\",\"volume\":\"1 1\",\"pages\":\"0\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2023-08-09\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"2\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Monthly Notices of the Royal Astronomical Society: Letters\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1093/mnrasl/slad128\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q1\",\"JCRName\":\"Earth and Planetary Sciences\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Monthly Notices of the Royal Astronomical Society: Letters","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1093/mnrasl/slad128","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q1","JCRName":"Earth and Planetary Sciences","Score":null,"Total":0}
引用次数: 2

摘要

与GW170817相关的千新星AT 2017gfo的晚时光谱在$2.1\,{\rm \mu m}$处表现出强烈的发射谱线特征。谱线结构随时间发展,光谱中没有蓝移吸收特征,表明这种发射谱线特征是由电子碰撞激发产生的。我们将发射线归因于碲(Te) III的精细结构线,它是第二个r过程峰中最丰富的元素之一。通过一个包含太阳r过程丰度模式超过第一个r过程峰(即原子质量数a > 88)的精细结构发射谱线的合成光谱模型,我们证明了[Te iii] $2.10\, \rm \mu m$确实是近红外区域最强的发射谱线。我们估计teiii的所需质量为~ 10−3 M⊙,对应于0.05 M⊙的合并抛射,这与从千新星光曲线估计的质量一致。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Tellurium emission line in kilonova AT 2017gfo
ABSTRACT The late-time spectra of the kilonova AT 2017gfo associated with GW170817 exhibit a strong emission line feature at $2.1\, {\rm \mu m}$. The line structure develops with time and there is no blueshifted absorption feature in the spectra, suggesting that this emission line feature is produced by electron collision excitation. We attribute the emission line to a fine structure line of Tellurium (Te) III, which is one of the most abundant elements in the second r-process peak. By using a synthetic spectral modelling including fine structure emission lines with the solar r-process abundance pattern beyond the first r-process peak, i.e. atomic mass numbers A ≳ 88, we demonstrate that [Te iii] $2.10\, \rm \mu m$ is indeed expected to be the strongest emission line in the near infrared region. We estimate that the required mass of Te iii is ∼10−3 M⊙, corresponding to the merger ejecta of 0.05 M⊙, which is in agreement with the mass estimated from the kilonova light curve.
求助全文
通过发布文献求助,成功后即可免费获取论文全文。 去求助
来源期刊
Monthly Notices of the Royal Astronomical Society: Letters
Monthly Notices of the Royal Astronomical Society: Letters Earth and Planetary Sciences-Space and Planetary Science
CiteScore
8.80
自引率
0.00%
发文量
136
期刊介绍: For papers that merit urgent publication, MNRAS Letters, the online section of Monthly Notices of the Royal Astronomical Society, publishes short, topical and significant research in all fields of astronomy. Letters should be self-contained and describe the results of an original study whose rapid publication might be expected to have a significant influence on the subsequent development of research in the associated subject area. The 5-page limit must be respected. Authors are required to state their reasons for seeking publication in the form of a Letter when submitting their manuscript.
×
引用
GB/T 7714-2015
复制
MLA
复制
APA
复制
导出至
BibTeX EndNote RefMan NoteFirst NoteExpress
×
提示
您的信息不完整,为了账户安全,请先补充。
现在去补充
×
提示
您因"违规操作"
具体请查看互助需知
我知道了
×
提示
确定
请完成安全验证×
copy
已复制链接
快去分享给好友吧!
我知道了
右上角分享
点击右上角分享
0
联系我们:info@booksci.cn Book学术提供免费学术资源搜索服务,方便国内外学者检索中英文文献。致力于提供最便捷和优质的服务体验。 Copyright © 2023 布克学术 All rights reserved.
京ICP备2023020795号-1
ghs 京公网安备 11010802042870号
Book学术文献互助
Book学术文献互助群
群 号:481959085
Book学术官方微信