日本語 English
| 開講年度/ Academic YearAcademic Year |
20252025 |
| 科目設置学部/ CollegeCollege |
理学研究科/Graduate School of ScienceGraduate School of Science |
| 科目コード等/ Course CodeCourse Code |
LA124/LA124LA124 |
| テーマ・サブタイトル等/ Theme・SubtitleTheme・Subtitle |
宇宙論的揺らぎの進化：インフレーションから現在まで/ Evolution of Cosmological Perturbations: From Inflation to the Present |
| 授業形態/ Class FormatClass Format |
対面（全回対面）/Face to face (all classes are face-to-face)Face to face (all classes are face-to-face) |
| 授業形態（補足事項）/ Class Format (Supplementary Items)Class Format (Supplementary Items) |
|
| 授業形式/ Class StyleCampus |
講義/LectureLecture |
| 校地/ CampusCampus |
池袋/IkebukuroIkebukuro |
| 学期/ SemesterSemester |
秋学期他/Fall OthersFall Others |
| 曜日時限・教室/ DayPeriod・RoomDayPeriod・Room |
ログインして教室を表示する（Log in to view the classrooms.） |
| 単位/ CreditsCredits |
22 |
| 科目ナンバリング/ Course NumberCourse Number |
PHY6090 |
| 使用言語/ LanguageLanguage |
日本語/JapaneseJapanese |
| 履修登録方法/ Class Registration MethodClass Registration Method |
科目コード登録/Course Code RegistrationCourse Code Registration |
| 配当年次/ Assigned YearAssigned Year |
配当年次は開講学部のR Guideに掲載している科目表で確認してください。配当年次は開講学部のR Guideに掲載している科目表で確認してください。 |
| 先修規定/ Prerequisite RegulationsPrerequisite Regulations |
|
| 他学部履修可否/ Acceptance of Other CollegesAcceptance of Other Colleges |
履修登録システムの『他学部・他研究科履修不許可科目一覧』で確認してください。 |
| 履修中止可否/ Course CancellationCourse Cancellation |
－（履修中止制度なし/ No system for cancellation) |
| オンライン授業60単位制限対象科目/ Online Classes Subject to 60-Credit Upper LimitOnline Classes Subject to 60-Credit Upper Limit |
|
| 学位授与方針との関連/ Relationship with Degree PolicyRelationship with Degree Policy |
各授業科目は、学部・研究科の定める学位授与方針（DP）や教育課程編成の方針（CP）に基づき、カリキュラム上に配置されています。詳細はカリキュラム・マップで確認することができます。 |
| 備考/ NotesNotes |
集中講義：日程はR Guide「集中講義日程」を確認すること RA124現代物理学特別講義２と合同授業 |
The goal is to study the foundations of cosmological perturbation theory, which provides a systematic description of the evolution of cosmological fluctuations, as well as its modern applications.
This lecture explains the foundations and applications of cosmological perturbation theory, which forms the core of modern cosmology. We will provide an overview of the fundamentals of cosmology based on general relativity, introducing topics such as the inflationary scenario, the generation of primordial fluctuations, structure formation, and gravitational waves. First, a brief review of general relativity and the homogeneous and isotropic universe will be conducted, followed by an introduction to the basic ideas of cosmological perturbation theory. Subsequently, we will discuss how primordial fluctuations generated by inflation grow and are observed as cosmic microwave background radiation and large-scale structures.
In the latter half of the lecture, we will delve into the nonlinearity of primordial fluctuations and nonlinear structure formation from the perspective of nonlinear perturbation theory. Using computational methods such as the in-in formalism and the delta N formalism, participants will learn theoretical techniques for calculating nonlinear primordial fluctuations and intuitive approaches to understanding their generation mechanisms. Finally, we will provide an overview of cutting-edge methods for probing the non-Gaussianity of primordial fluctuations through observations of large-scale structure formation and discuss how the properties of initial fluctuations can be observationally tested.
| 1 | 一様等方宇宙の進化（概観）/Overview of homogeneous and isotropic universe |
| 2 | 宇宙論的摂動論の基礎/ Basis of cosmological perturbation theory |
| 3 | ゲージ変換とゲージ不変量の構成/ Gauge transformations and construction of gauge invariant variables |
| 4 | インフレーションと原始揺らぎ/ Inflation and primordial perturbations |
| 5 | 構造形成 I: 線形摂動論/ Large scale structure formation I: Linear theory |
| 6 | 構造形成 II: 非線形摂動論/ Large scale structure formation II: Non-linear theory |
| 7 | 宇宙背景輻射（進捗状況次第で短縮または省略する可能性もある）/Cosmic microwave background |
| 8 | 重力波/ Gravitational waves |
| 9 | 非線形の原始揺らぎの計算方法 I/ Non-linear analysis of primordial perturbations I |
| 10 | 非線形の原始揺らぎの計算方法 II/ / Non-linear analysis of primordial perturbations II |
| 11 | 原始非ガウス性と宇宙加速器/ Primordial non-Gaussianity and cosmological colliders |
| 12 | 原始重力波/ Primordial gravitational waves |
| 13 | Stochastic approachとeternal inflation/ Stochastic approach and eternal inflation |
| 14 | 構造形成の観測を通じた原始非ガウス性の検証/ Imprint of primordial non-Gaussianity on large scale structure |
板書 /Writing on the Board
スライド（パワーポイント等）の使用 /Slides (PowerPoint, etc.)
上記以外の視聴覚教材の使用 /Audiovisual Materials Other than Those Listed Above
個人発表 /Individual Presentations
グループ発表 /Group Presentations
ディスカッション・ディベート /Discussion/Debate
実技・実習・実験 /Practicum/Experiments/Practical Training
学内の教室外施設の利用 /Use of On-Campus Facilities Outside the Classroom
校外実習・フィールドワーク /Field Work
上記いずれも用いない予定 /None of the above
一般相対性理論の基礎については既に学んでいるものとして講義を進めます。必要な方は事前に予習をしてください。/ The lecture assumes that participants are already familiar with the basics of general relativity. If not, please review the material beforehand.
| 種類 (Kind) | 割合 (%) | 基準 (Criteria) |
|---|---|---|
| 平常点 (In-class Points) | 100 |
複数回の課題(100%) |
| 備考 (Notes) | ||
| 課題は講義中にアナウンスします。(The detail of the assignment will be announced during the lecture.) | ||
なし/None
| No | 著者名 (Author/Editor) | 書籍名 (Title) | 出版社 (Publisher) | 出版年 (Date) | ISBN/ISSN |
|---|---|---|---|---|---|
| 1 | Hideo Kodama, Misao Sasaki | Cosmological Perturbation Theory | Oxford Academic | 1984 | |
| 2 | Steven Weinberg | Cosmology | Oxford University Press | 2008 | |
| その他 (Others) | |||||
| 各章ごとに参考文献が異なるため文献の詳細は講義中にお知らせします。(The detailed information of reference materials will be announced during the lecture.) | |||||
一般相対性理論の基礎については既に学んでいるものとして講義を進めます。/ The lecture assumes that participants are already familiar with the basics of general relativity.
宇宙論的ゆらぎの進化の体系的記述を与える宇宙論的摂動論の基礎および現代の応用について学ぶことを目標とする。
The goal is to study the foundations of cosmological perturbation theory, which provides a systematic description of the evolution of cosmological fluctuations, as well as its modern applications.
本講義では、現代宇宙論の根幹をなしている宇宙論的摂動論の基礎および応用について解説します。一般相対性理論に基づく宇宙論の基礎を概観し、インフレーションシナリオや原始揺らぎの生成、構造形成、重力波などのトピックを紹介します。まず、一様等方宇宙の簡単な復習を行った後、宇宙論的摂動論の基本的なアイデアを紹介します。続いて、インフレーションによって生成された原始揺らぎがどのように成長し、宇宙背景輻射や大規模構造として観測されるかを俯瞰します。
講義の後半では、非線形摂動論の観点から原始揺らぎの非線形性や非線形構造形成について議論します。in-in形式やデルタN形式といった計算手法を通じて、非線形の原始揺らぎの理論的な計算手法を学ぶとともに、その生成機構を直観的に理解する方法を紹介します。最後に、大規模構造形成の観測を通じて原始揺らぎの非ガウス性を探る最先端の手法を概観し、初期揺らぎの性質を観測的に検証する方法を紹介します。
This lecture explains the foundations and applications of cosmological perturbation theory, which forms the core of modern cosmology. We will provide an overview of the fundamentals of cosmology based on general relativity, introducing topics such as the inflationary scenario, the generation of primordial fluctuations, structure formation, and gravitational waves. First, a brief review of general relativity and the homogeneous and isotropic universe will be conducted, followed by an introduction to the basic ideas of cosmological perturbation theory. Subsequently, we will discuss how primordial fluctuations generated by inflation grow and are observed as cosmic microwave background radiation and large-scale structures.
In the latter half of the lecture, we will delve into the nonlinearity of primordial fluctuations and nonlinear structure formation from the perspective of nonlinear perturbation theory. Using computational methods such as the in-in formalism and the delta N formalism, participants will learn theoretical techniques for calculating nonlinear primordial fluctuations and intuitive approaches to understanding their generation mechanisms. Finally, we will provide an overview of cutting-edge methods for probing the non-Gaussianity of primordial fluctuations through observations of large-scale structure formation and discuss how the properties of initial fluctuations can be observationally tested.
| 1 | 一様等方宇宙の進化（概観）/Overview of homogeneous and isotropic universe |
| 2 | 宇宙論的摂動論の基礎/ Basis of cosmological perturbation theory |
| 3 | ゲージ変換とゲージ不変量の構成/ Gauge transformations and construction of gauge invariant variables |
| 4 | インフレーションと原始揺らぎ/ Inflation and primordial perturbations |
| 5 | 構造形成 I: 線形摂動論/ Large scale structure formation I: Linear theory |
| 6 | 構造形成 II: 非線形摂動論/ Large scale structure formation II: Non-linear theory |
| 7 | 宇宙背景輻射（進捗状況次第で短縮または省略する可能性もある）/Cosmic microwave background |
| 8 | 重力波/ Gravitational waves |
| 9 | 非線形の原始揺らぎの計算方法 I/ Non-linear analysis of primordial perturbations I |
| 10 | 非線形の原始揺らぎの計算方法 II/ / Non-linear analysis of primordial perturbations II |
| 11 | 原始非ガウス性と宇宙加速器/ Primordial non-Gaussianity and cosmological colliders |
| 12 | 原始重力波/ Primordial gravitational waves |
| 13 | Stochastic approachとeternal inflation/ Stochastic approach and eternal inflation |
| 14 | 構造形成の観測を通じた原始非ガウス性の検証/ Imprint of primordial non-Gaussianity on large scale structure |
板書 /Writing on the Board
スライド（パワーポイント等）の使用 /Slides (PowerPoint, etc.)
上記以外の視聴覚教材の使用 /Audiovisual Materials Other than Those Listed Above
個人発表 /Individual Presentations
グループ発表 /Group Presentations
ディスカッション・ディベート /Discussion/Debate
実技・実習・実験 /Practicum/Experiments/Practical Training
学内の教室外施設の利用 /Use of On-Campus Facilities Outside the Classroom
校外実習・フィールドワーク /Field Work
上記いずれも用いない予定 /None of the above
一般相対性理論の基礎については既に学んでいるものとして講義を進めます。必要な方は事前に予習をしてください。/ The lecture assumes that participants are already familiar with the basics of general relativity. If not, please review the material beforehand.
| 種類 (Kind) | 割合 (%) | 基準 (Criteria) |
|---|---|---|
| 平常点 (In-class Points) | 100 |
複数回の課題(100%) |
| 備考 (Notes) | ||
| 課題は講義中にアナウンスします。(The detail of the assignment will be announced during the lecture.) | ||
なし/None
| No | 著者名 (Author/Editor) | 書籍名 (Title) | 出版社 (Publisher) | 出版年 (Date) | ISBN/ISSN |
|---|---|---|---|---|---|
| 1 | Hideo Kodama, Misao Sasaki | Cosmological Perturbation Theory | Oxford Academic | 1984 | |
| 2 | Steven Weinberg | Cosmology | Oxford University Press | 2008 | |
| その他 (Others) | |||||
| 各章ごとに参考文献が異なるため文献の詳細は講義中にお知らせします。(The detailed information of reference materials will be announced during the lecture.) | |||||
一般相対性理論の基礎については既に学んでいるものとして講義を進めます。/ The lecture assumes that participants are already familiar with the basics of general relativity.