＜＜＜「@」を「__AT__」に置き換えています＞＞＞ Date: Mon, 29 Jun 2026 15:13:57 +0900 To: sg-l__AT__yukawa.kyoto-u.ac.jp Subject: [Sg-l:10478] 学術変革領域「量子物質」国際レクチャー：銀河化学進化 From: Nobuya Nishimura (Sg-l 経由)Sg-l の皆さま、 工学院大学の西村です。 下記にありますように、今年１０月に国立天文台（三鷹）におきまして、 銀河化学進化に関する国際レクチャーを開催いたします。 これは、学術変革領域「精密数値計算が切り拓く宇宙の量子物質科学」 による国際レクチャーシリーズの一環です。 講師：小林 千晶（Hertfordshire 大学） 場所：国立天文台（三鷹） ※ベストエフォートでのZoom参加も準備 日程：2026年10月29日、30日 詳細は、本メール末尾の案内、および、ウェブサイトをご覧ください。 https://indico2.riken.jp/e/gce2026 皆様、特に学生や若手研究者の皆さま、奮ってご参加ください。 世話人： 青木 和光（国立天文台） 岡田 寛子（国立天文台） 西村 俊二（理化学研究所） 西村 信哉（工学院大） =========================================================== Dear all, We are pleased to announce a two-day international lecture on "Galactic Chemical Evolution" by Prof. C. Kobayashi (University of Hertfordshire). This lecture is part of the international lecture series sponsored by the JSPS KAKENHI Transformative Research Areas (A) project, "Quantum Matter Science in the Universe Opened Up by Precise Numerical Calculations". We welcome a broad audience, including PhD students, early-career researchers, and non-specialists interested in stellar nucleosynthesis and galactic chemical evolution. For more details and the latest information, please visit: https://indico2.riken.jp/e/gce2026 Date: 29–30 Oct. 2026 Venue: Mitaka Campus, National Astronomical Observatory of Japan (NAOJ) * On-site participation is encouraged, but online participation via Zoom will also be available for registrants. Please note that online access via Zoom will be provided on a best-effort basis Registration deadline: 21 Oct. 2026 (JST) Lecturer: Chiaki Kobayashi (University of Hertfordsire) Tile: Galactic Chemical Evolution Abstract: During the Big Bang, only light elements such as hydrogen and helium were produced. Carbon and heavier elements (called metals in astronomy) are created inside stars and are ejected when they die. Iron-peak and neutron-capture elements are further produced by binaries - Type Ia supernovae and neutron star mergers, respectively. These elements are distributed into the interstellar medium, and new stars formed from this gas contain elements produced by previous generations of stars. Therefore, stars are fossils that retain the history of their host galaxy. Detailed elemental abundances of individual stars in the Milky Way have been extremely useful for constraining stellar nucleosynthesis and the origin of elements. Not only metallicities but also elemental abundance ratios evolve in galaxies, which can be used to constrain stellar astrophysics and galaxy evolution. In our zoom-in simulation of a Milky Way type galaxy, the basic structures of the Galaxy and their stellar populations are reproduced very well; the bulge formed by the assembly of small gas-rich galaxies at high-redshifts has old and high-alpha stellar populations, while the disk formed inside-out with a longer timescale has younger and lower-alpha stellar populations due to the delayed enrichment from Type Ia supernovae, which results in the bimodal distribution of the alpha-to-iron ratios observed in the Milky Way Galaxy and M31 Andromeda Galaxy. For the elements heavier than iron, it is not possible to reproduce observations with neutron star mergers only and the contributions from magneto-rotational supernovae is required. In large-scale cosmological simulations, including feedback from active galactic nuclei that originate the first stars, chemical and dynamical properties of various types of galaxies are fairly well reproduced. Metallicity is higher in more massive galaxies (leading to the mass-metallicity relation), and at the centre of galaxies (causing metallicity radial gradients), broadly following elemental abundance trends expected by nuclear astrophysics. With the James Webb Space Telescope, unexpected elemental-abundance ratios (namely high N/O) are detected for very high redshift star-forming galaxies, which can be explained with Wolf-Rayet stars under intermittent star formation. Comparing various elemental abundances (CNO, Ne, and Ar) to the galactic chemical evolution models, it will be possible to confirm the dominant enrichment source as well as constraining galaxy formation processes across Cosmic Time. Tentative program: 29 Oct. 10:00-11:30 Lecture 1: Galactic Chemical Evolution Basics 13:30-15:00 Lecture 2: The Galactics Archaeology - Milky Way and it's satellites 30 Oct. 10:00-11:30 Lecture 3: Extra-galactics Archaeology - JWST galaxies and cosmic chemical enrichment ========================================================== -- Nobuya Nishimura Academic Support Center, Kogakuin University e-mail (research): nobuya__AT__cc.kogakuin.ac.jp Visiting researcher: - Center for Nuclear Study (CNS), The University of Tokyo - RIKEN Pioneering Research Institute (RIKEN PRI), RIKEN %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% Date: Fri, 25 Sep 2026 22:00:34 +0900 To: sg-l__AT__yukawa.kyoto-u.ac.jp Subject: [Sg-l:10648] 【リマインド】学術変革領域「量子物質」国際レクチャー：銀河化学進化 From: Nobuya Nishimura (Sg-l 経由) sg-l ML の皆さま、 工学院大の西村です。 参加登録締め切りまで１ヶ月ほどになりましたので、 再度ご案内させていただきます。 分野を問わず、学生や若手研究者の皆さまの参加を歓迎します。 詳細は、本メール末尾の案内、および、ウェブサイトをご覧ください。 https://indico2.riken.jp/e/gce2026 なお、10月30日（講義2日目）の午後には、小林さんによる 国立天文台の談話会が計画されています。講義に続いて 最新の話題を聴講するよい機会になると思います。 具体的な実施内容は、今後の談話会についての案内等をお待ちください。 https://sites.google.com/site/naojdanwakai/ 世話人： 青木 和光（国立天文台） 岡田 寛子（国立天文台） 西村 俊二（理化学研究所） 西村 信哉（工学院大） ===================================== Sg-l の皆さま、 工学院大学の西村です。 下記にありますように、今年１０月に国立天文台（三鷹）におきまして、 銀河化学進化に関する国際レクチャーを開催いたします。 これは、学術変革領域「精密数値計算が切り拓く宇宙の量子物質科学」 による国際レクチャーシリーズの一環です。 講師：小林 千晶（Hertfordshire 大学） 場所：国立天文台（三鷹） ※ベストエフォートでのZoom参加も準備 日程：2026年10月29日、30日 詳細は、本メール末尾の案内、および、ウェブサイトをご覧ください。 https://indico2.riken.jp/e/gce2026 皆様、特に学生や若手研究者の皆さま、奮ってご参加ください。 世話人： 青木 和光（国立天文台） 岡田 寛子（国立天文台） 西村 俊二（理化学研究所） 西村 信哉（工学院大） =========================================================== Dear all, We are pleased to announce a two-day international lecture on "Galactic Chemical Evolution" by Prof. C. Kobayashi (University of Hertfordshire). This lecture is part of the international lecture series sponsored by the JSPS KAKENHI Transformative Research Areas (A) project, "Quantum Matter Science in the Universe Opened Up by Precise Numerical Calculations". We welcome a broad audience, including PhD students, early-career researchers, and non-specialists interested in stellar nucleosynthesis and galactic chemical evolution. For more details and the latest information, please visit: https://indico2.riken.jp/e/gce2026 Date: 29–30 Oct. 2026 Venue: Mitaka Campus, National Astronomical Observatory of Japan (NAOJ) * On-site participation is encouraged, but online participation via Zoom will also be available for registrants. Please note that online access via Zoom will be provided on a best-effort basis Registration deadline: 21 Oct. 2026 (JST) Lecturer: Chiaki Kobayashi (University of Hertfordsire) Tile: Galactic Chemical Evolution Abstract: During the Big Bang, only light elements such as hydrogen and helium were produced. Carbon and heavier elements (called metals in astronomy) are created inside stars and are ejected when they die. Iron-peak and neutron-capture elements are further produced by binaries - Type Ia supernovae and neutron star mergers, respectively. These elements are distributed into the interstellar medium, and new stars formed from this gas contain elements produced by previous generations of stars. Therefore, stars are fossils that retain the history of their host galaxy. Detailed elemental abundances of individual stars in the Milky Way have been extremely useful for constraining stellar nucleosynthesis and the origin of elements. Not only metallicities but also elemental abundance ratios evolve in galaxies, which can be used to constrain stellar astrophysics and galaxy evolution. In our zoom-in simulation of a Milky Way type galaxy, the basic structures of the Galaxy and their stellar populations are reproduced very well; the bulge formed by the assembly of small gas-rich galaxies at high-redshifts has old and high-alpha stellar populations, while the disk formed inside-out with a longer timescale has younger and lower-alpha stellar populations due to the delayed enrichment from Type Ia supernovae, which results in the bimodal distribution of the alpha-to-iron ratios observed in the Milky Way Galaxy and M31 Andromeda Galaxy. For the elements heavier than iron, it is not possible to reproduce observations with neutron star mergers only and the contributions from magneto-rotational supernovae is required. In large-scale cosmological simulations, including feedback from active galactic nuclei that originate the first stars, chemical and dynamical properties of v arious types of galaxies are fairly well reproduced. Metallicity is higher in more massive galaxies (leading to the mass-metallicity relation), and at the centre of galaxies (causing metallicity radial gradients), broadly following elemental abundance trends expected by nuclear astrophysics. With the James Webb Space Telescope, unexpected elemental-abundance ratios (namely high N/O) are detected for very high redshift star-forming galaxies, which can be explained with Wolf-Rayet stars under intermittent star formation. Comparing various elemental abundances (CNO, Ne, and Ar) to the galactic chemical evolution models, it will be possible to confirm the dominant enrichment source as well as constraining galaxy formation processes across Cosmic Time. Tentative program: 29 Oct. 10:00-11:30 Lecture 1: Galactic Chemical Evolution Basics 13:30-15:00 Lecture 2: The Galactics Archaeology - Milky Way and it's satellites 30 Oct. 10:00-11:30 Lecture 3: Extra-galactics Archaeology - JWST galaxies and cosmic chemical enrichment ==========================================================