Progress in Astronomy 天文学进展 (twxjz-new)

@book{pia:1,
  author    = {W. J. 卡夫曼},
  title     = {行星和卫星},
  translator= {马星垣 and 王鸿阳},
  address   = {北京},
  publisher = {科学出版社},
  year      = {1987},
  pages     = {88-89}
}

@book{pia:2,
  editor    = {G. A. Wilkin and S. Stevens-Rayburn},
  title     = {Library and Information Services in Astronomy},
  address   = {Washington},
  publisher = {USNO},
  year      = {1989},
  pages     = {10-11}
}

@incollection{pia:3,
  author    = {H. A. Abt},
  title     = {Unknown},
  booktitle = {Library and Information Services in Astronomy},
  editor    = {G. A. Wilkin and S. Stevens-Rayburn},
  address   = {Washington},
  publisher = {USNO},
  year      = {1989},
  pages     = {37-38}
}

@article{pia:4,
  author  = {熊大闰 and 邓李才},
  title   = {Unknown},
  journal = {天文学报},
  year    = {2002},
  volume  = {43},
  pages   = {12--19}
}

@article{pia:5,
  author       = {J. M. Bardeen and J. R. Bond and N. Kaiser and others},
  title        = {Unknown},
  journal      = {Astrophysical Journal},
  shortjournal = {ApJ},
  year         = {1986},
  volume       = {304},
  pages        = {15-22}
}

@phdthesis{pia:6,
  author  = {R. B. Cairn},
  title   = {Unknown},
  school  = {University of California},
  address = {Berkley},
  year    = {1965},
  pages   = {156-157}
}

@phdthesis{pia:7,
  author  = {卢仙文},
  title   = {Unknown},
  school  = {中国科学院上海天文台},
  address = {上海},
  year    = {1998},
  pages   = {43-44}
}

@techreport{pia:8,
  author      = {S. Larson and I. Sekanina},
  title       = {Unknown},
  institution = {JPL},
  series      = {International Halley Watch Newsletters},
  number      = {5},
  address     = {California},
  year        = {1984},
  pages       = {32-33}
}

@letter{pia:9,
  author       = {H. W. Epps},
  howpublished = {Private communication},
  year         = {1989},
  date         = {1989-09-30}
}

@letter{pia:10,
  author       = {林元章},
  howpublished = {私人通信},
  year         = {1992},
  date         = {1992-10-09}
}



@misc{pia:12,
  title         = {Where are the young pulsars?},
  author        = {Arnon Dar},
  year          = {1999},
  eprint        = {astro-ph/9911473},
  archivePrefix = {arXiv},
  primaryClass  = {astro-ph},
  url           = {https://arxiv.org/abs/astro-ph/9911473},
}

}

@article{RodriguezE2000,
  author = {Rodr{\'i}guez, E. and L{\'o}pez-Gonz{\'a}lez, M. J. and L{\'o}pez de Coca, P.},
  title = {},
  journal = {Astronomy and Astrophysics Supplement Series},
  volume = {144},
  pages = {469},
  year = {2000}
}

@article{Lee2008,
  author = {Lee, Y. H. and Kim, S. S. and Shin, J. and others},
  title = {},
  journal = {Publications of the Astronomical Society of Japan},
  volume = {60},
  pages = {551},
  year = {2008}
}

@misc{yang2021cataloguedoublemodehighamplitude,
      title={A catalogue of double-mode high amplitude $\delta$ Scuti stars in the Galaxy and their statistical properties}, 
      author={Tao-Zhi Yang and Zhao-Yu Zuo and Xin-Yue Wang and Xiao-Ya Sun and Rui-Xuan Tang},
      year={2021},
      eprint={2110.13594},
      archivePrefix={arXiv},
      primaryClass={astro-ph.SR},
      url={https://arxiv.org/abs/2110.13594}, 
}

@article{Bowman2021,
  author = {Bowman, D. M. and Hermans, J. and Daszy{\'n}ska-Daszkiewicz, J. and others},
  title = {},
  journal = {Monthly Notices of the Royal Astronomical Society},
  volume = {504},
  number = {3},
  pages = {4039},
  year = {2021}
}

@article{Yang2022,
  author = {Yang, T. Z. and Zuo, Z. Y. and Sun, X. Y. and others},
  title = {},
  journal = {The Astrophysical Journal},
  volume = {936},
  number = {1},
  pages = {48},
  year = {2022}
}

@article{Lv2022a,
  author = {Lv, C. and Esamdin, A. and Pascual-Granado, J. and others},
  title = {},
  journal = {The Astronomical Journal},
  volume = {164},
  number = {5},
  pages = {218},
  year = {2022}
}

@article{Poretti2011,
  author = {Poretti, E. and Rainer, M. and Weiss, W. W. and others},
  title = {},
  journal = {Astronomy and Astrophysics},
  volume = {528},
  pages = {A147},
  year = {2011}
}


@article{Xue2020,
  author = {Xue, H. F. and Niu, J. S.},
  title = {},
  journal = {The Astrophysical Journal},
  volume = {904},
  number = {1},
  pages = {5},
  year = {2020}
}


@inproceedings{Pamyatnykh2000,
  author = {Pamyatnykh, A. A.},
  title = {Delta Scuti and Related Stars},
  booktitle = {Delta Scuti and Related Stars},
  editor = {Breger, M. and Montgomery, M.},
  series = {Astronomical Society of the Pacific Conference Series},
  volume = {210},
  pages = {215},
  year = {2000},
  address = {San Francisco}
}



@book{Aerts2010,
  author = {Aerts, C. and Christensen-Dalsgaard, J. and Kurtz, D. W.},
  title = {Asteroseismology},
  publisher = {Springer},
  year = {2010},
  address = {Heidelberg},
  pages = {1}
}

@article{Ricker2015,
  author = {Ricker, G. R. and Winn, J. N. and Vanderspek, R. and others},
  title = {},
  journal = {Journal of Astronomical Telescopes, Instruments, and Systems},
  volume = {1},
  pages = {014003},
  year = {2015}
}

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%====================================================================
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%====================================================================
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          % Astronomical Journal
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          % Astrophysical Journal
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          % Infoormation Bulletin on Variable Stars
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%============================================================
% Chinese astronomical affiliates:
%============================================================
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% !TeX program = xelatex
%% 技术支持：latexstudio
%% Website <www.latexstudio.net>
%% Email <[email protected]>

\documentclass{twxjz-new}
% 文档选项
% [en] 英文文档
% [cn] 中文文档


\begin{document}

%%  for Editor
\Volume{43}{2}
\PublishDate{2025}{6}
\setcounter{page}{1}
\SerialNumber{2025.02.XX}


\LabelNumber{P145.2}
\IDCode{A}
\date{YYYY-MM-DD}{YYYY-MM-DD}
\support{国家重点研发计划-政府间国际科技创新合作项（2022XXXXXX）}
\corremail{作者名，[email protected]}


\title{Your paper}

\author{作者1\inst{1,2}，作者2\inst{2}}

\institute{\centering（1. 中国科学院大学~~ 天文与空间科学学院，北京~~ 100049； \quad 2. 中国科学院~~ 上海天文台，上海 ~~ 200030）}

\titlemark{作者1，等：文章中文题目}

\maketitle
\begin{abstract}
褐矮星是亚恒星天体，内核没有稳定的氢燃烧，其质量一般在13至75倍木星质量之间。本质上，褐矮星的内核物理演化过程不同于行星和恒星，观测上我们根据褐矮星不同于行星和恒星的测光和光谱特征来区别证认它们。
\keywords{L、T、Y矮星；褐矮星；极冷矮星；谱指数 }
\end{abstract}

\section{引言}

褐矮星的质量小于恒星的质量下限而大于行星质量上限，其内核没有稳定的氢燃烧。褐矮星的概念
首次由Kumar\upcite{kum1963}于1963年提出。他对低质量星体的数值模拟表明，若质量小于某一阈值，其内核的温度将不能达到维持稳定氢聚变反应需要的温度，
因此不会像恒星一样进入主序阶段。

\subsection{L、T 矮星的光学波段光谱特征与分类}

图~\ref{fig2} 展示早型L到晚型T的光学波段光谱：M矮星中特别显著的VO 和TiO吸收线到中
型L开始减弱消失，而中性的NaI和KI吸收线变得非常强，金属氢化物MgH、CaOH、CrH和FeH的吸收线相比早型L矮星也有所增强；到了晚型L和早型T矮星，
水分子的吸收线增强，中性碱金属的吸收线依然很强，金属氢化物的吸收线则大大地减弱；对于晚型T 矮星，KI和NaI的吸收线因达到饱和而变得非常宽，
水分子线也很强，是主要的吸收体，这些吸收线使得7000~\AA
处光谱的流量很低。根据Kirkpatrick等人\upcite{sau1996}2005年的工作，我们将早型L到晚型T 矮星在光学波段的特征吸收线总结在表1中。

\begin{table}[!htp]
\centering
\caption{4个天区和空源的$\bm A$观测日期和天区}
\label{obs_four_sky_field}
\begin{tabular}{ll|ll}
\hline
观测时间 & 观测天区 & 观测时间 & 观测天区 \\
\hline
1995.07.07        & Blank                      $^{\ast}$ & 2003.04.26 --04.30  & F.Leo F.Coma  \\
1996.01.23---01.25  & F.Leo F.1002 F.Coma Blank            & 2004.04.23--04.26  & F.Leo F.Coma  \\
1996.02.07---02.09  & F.Leo F.1002 F.Coma Blank  $^{\ast}$ & 2004.11.16--11.18  & F.836 Blank   \\
1996.07.05---07.07  & Blank                      $^{\ast}$ & 2005.03.11--03.14  & F.Leo F.Coma  \\
\hline
\end{tabular}
\end{table}

\begin{figure}[!htp]
\centering
\includegraphics{picture/spt_n.eps}
\begin{quote}
\zihao{6}注：红色为侦测到的信号强度，黑色线为热噪音与银河盘面噪音的预期值。$250
\sim 270$ MHz的连续区段为海事通讯用的射电频段。
\end{quote}\vspace{-3mm}
\caption{TAROGE射电背景\upcite{sau1996}}
\label{fig2}
\end{figure}

\section{总结与展望}
褐矮星是近50年来兴起的研究领域，自从1963年Kumar第一次在理论上预言褐矮星的存在，该领域在观测和理论上都得到了很大发展\upcite{sau1996}。
褐矮星质量小、星等暗、颜色红(是指光学波段，并不能简单地说质量越小颜色越红。其近红外波段颜色受大气
尘埃、金属丰度等影响，具有独特的星等、颜色，如T矮星J--K颜色较L矮星的偏蓝)，这对褐矮星的观测造成了困难\upcite{sau1996}。

%% use bibitem
\begin{thebibliography}{00}
\bibitem{kum1963} Kumar S S. AXX, 1963, 137: 1121
\bibitem{sau1996} Saumon D, Hubbard W B, Burrows A, et al. AXX, 1996, 460: 993
\end{thebibliography}

%% use bib
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%\bibliographystyle{twxjz}
%\bibliography{test}

\backmatter

\title{The Title of this Paper in English}
\author{XING Ming$^{1,2}$,\quad SHAO Zhengyi$^{2}$}

\institute{(1. School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing
100049, China;\quad  2. Shanghai Astronomical Observatory, Chinese Academy of
Sciences, Shanghai 200030, China)}

\maketitle

\begin{abstract}
Brown dwarfs are substellar objects which have masses in between the most massive planets
and the least massive stars. There are no stable hydrogen fusion in their interiors,
although large mass brown dwarf might have instant hydrogen fusion in their core. All
brown dwarfs have deuterium burning in their interiors. The L, T and Y dwarfs are cooler
than M dwarfs. A small part of late M, most of the L, all of the T and all of the up to
date discovered Y dwarfs are brown dwarfs.
\end{abstract}

\keywords{brown dwarf; L, T, Y dwarf; ultracool dwarf; spectral index}

\end{document}

90 KB — too long to show here. It arrives with the project.