Exploring equation of state for neutron star analyzing gravitational wave data from binary neutron star mergers

探索中子星的状态方程，分析双中子星合并的引力波数据

• 批准号: 21K03548
• 负责人: 成川 達也
• 金额: $ 1.25万
• 依托单位: The University of Tokyo
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (C)
• 财政年份: 2021
• 资助国家: 日本
• 起止时间: 2021-04-01 至 2024-03-31
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-21K03548/
• 关键词: ポスト・ニュートニアン近似; 連星中性子星合体; 重力波天文学; 重力波データ解析; 中性子星; 高密度状態方程式; 連星中性子星

本研究の目的である(A): 重力波波形モデルの開発と実イベント解析への応用を行った.ポスト・ニュートニアン (PN) 近似は理論的に堅くかつコンパクト連星合体のインスパイラル期を正確に記述するため, 重力波データ解析に使われている. Henry, et al. (2020) によって, PN近似による重力波波形の断熱的潮汐効果パートがアップデートされた. 我々は以前, この波形を解析に便利なように潮汐変形率パラメータの関数として書き直した.書き直した波形を連星中性子星合体の解析に適用した. GW170817とGW190425の再解析を行い, アップデート前と後の波形による潮汐変形率の推定の差異は非常に小さいことを確認した. 潮汐効果項の各PN次数項の効果を調べ, 潮汐変形率の推定に関して位相進化と無矛盾な結果を得た. つまり, 半整数次項は負符号の潮汐変形効果を与えるため, 推定される潮汐変形率の中央値は整数次項の推定に比べて大きな値となる. また, 数値相対論較正モデルと比較し, 潮汐変形率は少し小さく見積もられるが, 有意性は主張できないことをベイズ因子を用いて示した. そして, 中性子星の状態方程式モデルの制限としてコンパクトネスが大きいモデルが選択されることを示した. 点粒子モデルの比較を行い, 潮汐変形率の推定に差異は無く, モデルの有意性も主張できないことを示した. これらの結果を科学論文としてまとめ, 提出, 受理, 出版された.また, この波形モデルをLIGO-Virgo-KAGRA Collaborationの共通解析パイプラインであるLALSuiteの波形部分であるLALSimulationに実装し, レヴューされ, 一般に公開される版として組み込まれた.

The purpose of this study is to analyze and analyze the gravity waveform. In the approximate theory of PN, there is a correct record of the period of the combination of stars, the analysis of gravity waves, the analysis of gravity waves, the analysis of gravity waves. Henry, et al. (2020) the PN approximation is due to the tidal effect of the broken gravity waveforms. In the past, we used to analyze the waveforms for convenience, tide, shape, shape and shape. The analysis of the neutral sub-star combination of the direct wave shape and the neutral sub-star. GW170817 GW190425 then parses the line, the front and rear waveforms, the tidal shape rate, the presumptive difference, the very small error, the confirmation. There are significant differences in the number of PN for each tidal event, and the tidal shape rate is presumed to be the result of phase evolution and contradiction. It is presumed that the shape rate of the tide is larger than that of the whole number of times, and the probability of the shape of the tide is larger than that of the whole number of times. The shape of the tide is small, the shape of the tide is small, The equation of the status of the neutral sub-star is limited by the limit of the equation. The number of point particles is higher than that of the point particles, the tidal shape rate is presumed to be clean, and the point particles are intentional. According to the results of the scientific literature, it is proposed, accepted, and published. In the common analysis of the waveforms, the waveforms, the LIGO-Virgo-KAGRA Collaboration waveforms, the waveforms, the LALSuite waveforms, the LALSimulation waveforms, the waveforms.

项目成果

GRB-targeted analyses on O3 GEO-KAGRA

O3 GEO-KAGRA 的 GRB 目标分析

• 发表时间: 2021
• 作者: Ren Tsuda;Shinya Tomizawa Ryotaku Suzuki;Tatsuhiro Naka;成川達也
• 通讯作者: 成川達也

The Current Status and Future Prospects of KAGRA, the Large-Scale Cryogenic Gravitational Wave Telescope Built in the Kamioka Underground

• DOI: 10.3390/galaxies10030063
• 发表时间: 2022-06-01
• 期刊: GALAXIES
• 影响因子: 2.5
• 作者: Abe, Homare;Akutsu, Tomotada;Zhao, Yuhang
• 通讯作者: Zhao, Yuhang

Observation of Gravitational Waves from Two Neutron Star-Black Hole Coalescences

• DOI: 10.3847/2041-8213/ac082e
• 发表时间: 2021-07-01
• 期刊: ASTROPHYSICAL JOURNAL LETTERS
• 影响因子: 7.9
• 作者: Abbott, R.;Abbott, T. D.;Zweizig, J.
• 通讯作者: Zweizig, J.

ポスト・ニュートニアン波形を用いた連星中性子星信号の詳細解析

使用后牛顿波形详细分析双中子星信号

• 发表时间: 2023
• 作者: M. Tahir;G. Abbas;Kazuharu Bamba and M. R. Shahzad;成川達也
• 通讯作者: 成川達也

All-sky search for gravitational wave emission from scalar boson clouds around spinning black holes in LIGO O3 data

• DOI: 10.1103/physrevd.105.102001
• 发表时间: 2021-11
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Gosselin;R. Gouaty;D. Gould;S. Goyal;B. Grace;A. Grado;V. Graham;M. Granata;V. Granata;A. Grant;S. Gras;P. Grassia;C. Gray;R. Gray;G. Greco;A. Green;R. Green;A. Gretarsson;E. Gretarsson;D. Griffith;W. Griffiths;H. L. Griggs;G. Grignani;A. Grimaldi;E. Grimes;S. Grimm;H. Grote;S. Grunewald;P. Gruning;A. Gruson;D. Guerra;G. Guidi;A. R. Guimaraes;G. Guix'e;H. Gulati;A. Gunny;H.-K. Guo;Y. Guo;Anchal Gupta;Anuradha Gupta;I. Gupta;P. Gupta;S. Gupta;R. Gustafson;F. Guzmán;S. Ha;I. Hadiputrawan;L. Haegel;S. Haino;O. Halim;E. Hall;E. Hamilton;G. Hammond;W. Han;M. Haney;J. Hanks;C. Hanna;M. Hannam;O. Hannuksela;H. Hansen;T. Hansen;J. Hanson;T. Harder;K. Haris;J. Harms;G. Harry;I. Harry;D. Hartwig;K. Hasegawa;B. Haskell;C. Haster;J. S. Hathaway;K. Hattori;K. Haughian;H. Hayakawa;K. Hayama;F. Hayes;J. Healy;A. Heidmann;A. Heidt;M. Heintze;J. Heinze;J. Heinzel;H. Heitmann;F. Hellman;P. Hello;A. Helmling-Cornell;G. Hemming;M. Hendry;I. Heng;E. Hennes;J. Hennig;M. Hennig;C. Henshaw;A. Hernandez;F. 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