分野別の学術論文翻訳例を紹介。医学・生命科学、物理・工学、人文系等の各翻訳・校正サンプル

ログイン
英文校正のエディテージ 論文の「伝える力」を最大限に発揮する
英文校正、論文翻訳、論文投稿サポート
お見積り・ご注文・お問い合せ 03-6868-3348 平日・祝日 9:30~24:0012:30~21:30
(論文投稿支援のみ 月~金 11:00~22:00)
GW中の祝日も全て通常営業

物理学の和英翻訳サンプル
物理科学・工学チームが対応する日英翻訳・英文校正

物理学の和英翻訳/サービスレベル別翻訳サンプル

物理学系のサンプルをサービスレベル別にご用意しました。各々のサービスの日英翻訳・英文校正プロセスで原稿がどのように仕上がっていくかご確認ください。

原子核物理分野との研究連携では、原子核物理側から、宇宙現象を理解するための基礎物理を天文・宇宙物理分野に提供することが重要となる。なかでも今後 10 年から 20 年を俯瞰した際に重要なのは、元素合成に関与する不安定核の諸性質と反応、及び高密度核物質の状態方程式の 2 点である。

元素合成については、星の進化に大きく影響する不定性の大きな核反応の精密化等が必要であると同時に、r-過程とよばれる元素合成過程の解明が焦点となる。r-過程とは、ウランや金など、鉄より重い元素のほぼ半分を合成し、ヒトや生物の生命維持に必須な元素を生み出す重要な物理過程であるが、どこで、どのように起きているのかわかっていない。

この r-過程に関与する、極端に中性子過剰な原子核の質量、半減期、核構造、中性子捕獲反応について、理研 RI ビームファクトリー(RIBF)において世界で初めて実験が敢行される。今後取得が見込まれる原子核データは大量である。

 高密度核物質の状態方程式については、RIBF において標準核密度の 2-3 倍程度までの情報が得られる。それ以上の密度については J-PARC において、中性子星中心部に存在が示唆されている中間子凝縮に関わるハイパー核の情報が得られる。これらを統合して、高密度核物質の状態方程式の理解が格段に進むと期待される。状態方程式の理解は、超新星爆発のメカニズムや中性子星の内部構造に密接に関係する。さらに重力波検出計画において第一の重力波源と想定されている、中性子星連星が合体する際の重力波放出にも、直接的な影響をもつ。

In performing collaborative research with the field of nuclear physics, it is important that fundamental physics knowledge from nuclear physics are provided to the fields of astronomy and astrophysics for the purpose of understanding cosmic phenomena. Within this, taking a broad view of the next 10 to 20 years, two points will be important. These are the various properties and reactions of unstable nuclei related to nucleosynthesis and equations of state for high density nuclear materials.

Regarding nucleosynthesis, while it is necessary to gain a refined understanding of nuclear reactions with high uncertainty that have a large effect on the evolution of stars, clarifying the nucleosynthetic process known as the r-process will be the focal point. The r-process is an important physical process that creates almost half of the elements heavier than iron, such as uranium, gold, and many others. These elements are important to the maintenance of human life and other living things, but where and how it occurs are still not understood.

The first experiments in the world on aspects of the r-process, such as the mass, half-life, nucleic structure, and neutron capture reactions of extremely neutron-rich nuclei will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding equations of state for high density nuclear materials, information about nuclei of two to three times standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which is suggested to exist in the center of neutron stars, is obtained in J-PARC. By integrating these, it is expected that our understanding of equations of state for high density nuclear materials will be dramatically advanced. An understanding of equations of state is intimately related to the mechanisms involved in supernova and the internal structure of neutron stars. Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, an event which has been positioned as the foremost source of gravitational waves in the gravitational wave detection plan.

In performing collaborative research with the field of nuclear physics, it is important that information about fundamental physics knowledge from nuclear physics areis provided to the fields of astronomy and astrophysics for the purpose of understanding cosmic phenomena. Within this, takingTaking a broad view of the next 10 to 20 years, two points will pieces of such information are expected to be important.of particular importance. These are, first, the various properties and reactions of unstable nuclei related to nucleosynthesis and, second, equations of state for high density nuclear materialsmatter.

Regarding nucleosynthesis, while it is necessary to gain a refined understanding of high uncertainty nuclear reactions with high uncertainty that have a largesignificant effect on the evolution of stars, clarifying the nucleosynthetic process known as the r-process will be the focal point. The r-process is an important physical process that creates almostabout half of the elements heavier than iron, such as uranium, gold, and many others. These elements are important to the maintenance of human life and other living things, but where and how itthis process occurs areis still not understood.

The first experiments in the world on aspects of the r-process, such as the mass, half-life, nucleicnuclear structure, and neutron capture reactions of extremely neutron-rich nuclei will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding equations of state for high density nuclear materialsmatter, information about nuclei of two to three times standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which ishave been suggested to exist in the center of neutron stars, iswill be obtained inat J-PARC. By integrating these, it is expected thatWe expect our understanding of equations of state for high density nuclear materials willmatter to be dramatically advanced by integrating these two sets of data. An understanding of equations of state is intimately related to the mechanisms involved in supernova and, as well as the internal structure of neutron stars. Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, an event which has been positioned as the foremost source of gravitational waves in the gravitational wave detection plan.

For In cperforming collaborative research with in the field of nuclear physics,,  it is important that information about fundamental nuclear physics information should be provided is provided to researchers from the fields of astronomy and astrophysics for the purpose of understanding cosmic phenomena. Taking Based on a broad view of the next 10 to 20 years, two pieces of such information are expected to be of particular importance. These are, first, the various properties and reactions of unstable nuclei related to nucleosynthesis, and, second, the equations of state for high high-density nuclear matter—are of particular importance.

To understand Regarding nucleosynthesis, while it is necessary to gain a refined understanding of high uncertainty nuclear reactions that have a significant effect on the evolution of stars is necessary; however, it is very important to clarifying the nucleosynthetic process known as the r-process will be the focal point.  The r-process is an important physical process that creates about half of the elements heavier than iron, such as uranium, gold, and many others. These elements areDespite the importancet of these elementsto  to the maintenance of human life and other living things, but where and how this process occurs is still not understood.

 The first experiments in the world on the aspects of the r-process, such as the mass, half-life, nuclear structure, and neutron capture reactions of extremely neutron-rich nuclei will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding For the equations equations of state for high high-density nuclear matter, information about the nuclei of two to three times the standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which have been suggested to exist in the center center of neutron stars, will be obtained at J-PARC. We expect our understanding of equations of state for high high-density nuclear matter to be dramatically advanced by integrating these two sets of data.

An Uunderstanding of the equations of state is intimately closely related to the mechanisms involved in a supernova, as well as the internal structure of neutron stars. Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, which is an event which has been positioned as considered to be the foremost source of gravitational waves in the gravitational wave detection plan.

For In cperforming collaborative research with in the field of nuclear physics,,  it is important that information about fundamental nuclear physics information should be provided is provided to researchers from the fields of astronomy and astrophysics for to facilitate the purpose of understanding of cosmic phenomena. Taking Based on a broad view of the next 10 to 20 years, two pieces of such information are expected to be of particular importance. These are, first, the various properties and reactions of unstable nuclei related to nucleosynthesis, and, second, the equations of state for high high-density nuclear matter—are of particular importance.

To understand Regarding nucleosynthesis, while it is necessary to gain a refined understanding of high- uncertainty nuclear reactions that have a significant effect on the evolution of stars is necessary; however, it is also very important to clarifying the nucleosynthetic process known as the r-process will be the focal point.  The r-process is an important physical process that creates about half of the elements heavier than iron, such as uranium, gold, and many others. These elements are Despite the importancet of these elements to to the maintenance of human life and other living things, but where and how this process occurs is still not understood.

 The first experiments in the world on the different aspects of the r-process, such as the mass, half-life, nuclear structure, and neutron capture reactions of extremely neutron-rich nuclei, will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding For the equations equations of state for high high-density nuclear matter, information about the nuclei of two to three times the standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which have been suggested to exist in the center center of neutron stars, will be obtained at J-PARC. We expect our understanding of the equations of state for high high-density nuclear matter to be dramatically advanced by integrating these two sets of data.

An Uunderstanding of the equations of state is intimately closely related to the mechanisms involved in a supernova, as well as the internal structure of neutron stars. Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, which is an event which has been positioned as considered to be the foremost source of gravitational waves in the gravitational wave detection plan.

原子核物理分野との研究連携では、原子核物理側から、宇宙現象を理解するための基礎物理を天文・宇宙物理分野に提供することが重要となる。なかでも今後 10 年から 20 年を俯瞰した際に重要なのは、元素合成に関与する不安定核の諸性質と反応、及び高密度核物質の状態方程式の 2 点である。

元素合成については、星の進化に大きく影響する不定性の大きな核反応の精密化等が必要であると同時に、r-過程とよばれる元素合成過程の解明が焦点となる。r-過程とは、ウランや金など、鉄より重い元素のほぼ半分を合成し、ヒトや生物の生命維持に必須な元素を生み出す重要な物理過程であるが、どこで、どのように起きているのかわかっていない。

この r-過程に関与する、極端に中性子過剰な原子核の質量、半減期、核構造、中性子捕獲反応について、理研 RI ビームファクトリー(RIBF)において世界で初めて実験が敢行される。今後取得が見込まれる原子核データは大量である。

 高密度核物質の状態方程式については、RIBF において標準核密度の 2-3 倍程度までの情報が得られる。それ以上の密度については J-PARC において、中性子星中心部に存在が示唆されている中間子凝縮に関わるハイパー核の情報が得られる。これらを統合して、高密度核物質の状態方程式の理解が格段に進むと期待される。状態方程式の理解は、超新星爆発のメカニズムや中性子星の内部構造に密接に関係する。さらに重力波検出計画において第一の重力波源と想定されている、中性子星連星が合体する際の重力波放出にも、直接的な影響をもつ。

In performing collaborative research with the field of nuclear physics, it is important that fundamental physics knowledge from nuclear physics are provided to the fields of astronomy and astrophysics for the purpose of understanding cosmic phenomena. Within this, taking a broad view of the next 10 to 20 years, two points will be important. These are the various properties and reactions of unstable nuclei related to nucleosynthesis and equations of state for high density nuclear materials.

Regarding nucleosynthesis, while it is necessary to gain a refined understanding of nuclear reactions with high uncertainty that have a large effect on the evolution of stars, clarifying the nucleosynthetic process known as the r-process will be the focal point. The r-process is an important physical process that creates almost half of the elements heavier than iron, such as uranium, gold, and many others. These elements are important to the maintenance of human life and other living things, but where and how it occurs are still not understood.

The first experiments in the world on aspects of the r-process, such as the mass, half-life, nucleic structure, and neutron capture reactions of extremely neutron-rich nuclei will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding equations of state for high density nuclear materials, information about nuclei of two to three times standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which is suggested to exist in the center of neutron stars, is obtained in J-PARC. By integrating these, it is expected that our understanding of equations of state for high density nuclear materials will be dramatically advanced. An understanding of equations of state is intimately related to the mechanisms involved in supernova and the internal structure of neutron stars. Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, an event which has been positioned as the foremost source of gravitational waves in the gravitational wave detection plan.

In performing collaborative research with the field of nuclear physics, it is important that information about fundamental physics knowledge from nuclear physics areis provided to the fields of astronomy and astrophysics for the purpose of understanding cosmic phenomena. Within this, takingTaking a broad view of the next 10 to 20 years, two points will pieces of such information are expected to be important.of particular importance. These are, first, the various properties and reactions of unstable nuclei related to nucleosynthesis and, second, equations of state for high density nuclear materialsmatter.

Regarding nucleosynthesis, while it is necessary to gain a refined understanding of high uncertainty nuclear reactions with high uncertainty that have a largesignificant effect on the evolution of stars, clarifying the nucleosynthetic process known as the r-process will be the focal point. The r-process is an important physical process that creates almostabout half of the elements heavier than iron, such as uranium, gold, and many others. These elements are important to the maintenance of human life and other living things, but where and how itthis process occurs areis still not understood.

The first experiments in the world on aspects of the r-process, such as the mass, half-life, nucleicnuclear structure, and neutron capture reactions of extremely neutron-rich nuclei will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding equations of state for high density nuclear materialsmatter, information about nuclei of two to three times standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which ishave been suggested to exist in the center of neutron stars, iswill be obtained inat J-PARC. By integrating these, it is expected thatWe expect our understanding of equations of state for high density nuclear materials willmatter to be dramatically advanced by integrating these two sets of data. An understanding of equations of state is intimately related to the mechanisms involved in supernova and, as well as the internal structure of neutron stars. Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, an event which has been positioned as the foremost source of gravitational waves in the gravitational wave detection plan.

In When performing collaborative research with in the field of nuclear physics, it is important that to provide information about fundamental nuclear physics is provided to researchers from the fields of astronomy and astrophysics for the purpose of understanding cosmic phenomena. Taking Based on a broad view of the next 10 to 20 years, two pieces of such information are expected to be of particular importance. These are, first, : the various properties and reactions of unstable nuclei related to nucleosynthesis, and, second, the equations of state for high high-density nuclear matter.

ARegarding nucleosynthesis, while lthough it is necessary to gain a refined understanding of high uncertainty nuclear reactions that have a significant effect on the evolution of stars to understand nucleosynthesis, clarifying the nucleosynthetic process known as the r-process will be the is the focal point. The r-process is an important physical process that creates about half of the elements heavier than iron, such as uranium, gold, and many others. These elements are important to for sustaining the maintenance of human life and other living things, but where and how this process occurs is still not understood.

 

The first experiments in the world on the aspects of the r-process, such as the mass, half-life, nuclear structure, and neutron capture reactions of extremely neutron-rich nuclei will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding For the equations of state for high high-density nuclear matter, information about the nuclei of two to three times the standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which have been suggested to exist in the center center of neutron stars, will be obtained at J-PARC. We expect our understanding of equations of state for high high-density nuclear matter to be dramatically advanced by integrating these two sets of data. An understanding of the equations of state is intimately related to the mechanisms involved in a supernova, as well as the internal structure of neutron stars.

Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, which is an event which has been positioned as the foremost source of gravitational waves in the gravitational wave detection plan.

In When performing collaborative research with in the field of nuclear physics, it is important that to provide information about fundamental nuclear physics is provided to researchers from the fields of astronomy and astrophysics for the purpose of understanding cosmic phenomena. Taking Based on a broad view of the next 10 to 20 years, two pieces of such information are expected to be of particular importance. These are, first, : the various properties and reactions of unstable nuclei related to nucleosynthesis, and, second, the equations of state for high high-density nuclear matter.

ARegarding nucleosynthesis, while lthough it is necessary to gain a refined understanding of high high-uncertainty nuclear reactions that have a significant effect on the evolution of stars to understand nucleosynthesis, clarifying the nucleosynthetic process known as the r-process will be the is the focal point. The r-process is an important physical process that creates about half of the elements heavier than iron, such as uranium, gold, and many others. These elements are important to for sustaining the maintenance of human life and other living things, but where and how this process occurs is still not understood.

 

The first experiments in the world on the aspects of the r-process, such as the mass, half-life, nuclear structure, and neutron capture reactions of extremely neutron-rich nuclei, will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding For the equations of state for high high-density nuclear matter, information about the nuclei of two to three times the standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which have been suggested to exist in the center center of neutron stars, will be obtained at J-PARC. We expect our understanding of the equations of state for high high-density nuclear matter to be dramatically advanced by integrating these two sets of data. An understanding of the equations of state is intimately related to the mechanisms involved in a supernova, as well as the internal structure of neutron stars.

Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, which is an event which has been positioned as the foremost source of gravitational waves in the gravitational wave detection plan.

原子核物理分野との研究連携では、原子核物理側から、宇宙現象を理解するための基礎物理を天文・宇宙物理分野に提供することが重要となる。なかでも今後 10 年から 20 年を俯瞰した際に重要なのは、元素合成に関与する不安定核の諸性質と反応、及び高密度核物質の状態方程式の 2 点である。

元素合成については、星の進化に大きく影響する不定性の大きな核反応の精密化等が必要であると同時に、r-過程とよばれる元素合成過程の解明が焦点となる。r-過程とは、ウランや金など、鉄より重い元素のほぼ半分を合成し、ヒトや生物の生命維持に必須な元素を生み出す重要な物理過程であるが、どこで、どのように起きているのかわかっていない。

この r-過程に関与する、極端に中性子過剰な原子核の質量、半減期、核構造、中性子捕獲反応について、理研 RI ビームファクトリー(RIBF)において世界で初めて実験が敢行される。今後取得が見込まれる原子核データは大量である。

 高密度核物質の状態方程式については、RIBF において標準核密度の 2-3 倍程度までの情報が得られる。それ以上の密度については J-PARC において、中性子星中心部に存在が示唆されている中間子凝縮に関わるハイパー核の情報が得られる。これらを統合して、高密度核物質の状態方程式の理解が格段に進むと期待される。状態方程式の理解は、超新星爆発のメカニズムや中性子星の内部構造に密接に関係する。さらに重力波検出計画において第一の重力波源と想定されている、中性子星連星が合体する際の重力波放出にも、直接的な影響をもつ。

In performing collaborative research with the field of nuclear physics, it is important that fundamental physics knowledge from nuclear physics are provided to the fields of astronomy and astrophysics for the purpose of understanding cosmic phenomena. Within this, taking a broad view of the next 10 to 20 years, two points will be important. These are the various properties and reactions of unstable nuclei related to nucleosynthesis and equations of state for high density nuclear materials.

Regarding nucleosynthesis, while it is necessary to gain a refined understanding of nuclear reactions with high uncertainty that have a large effect on the evolution of stars, clarifying the nucleosynthetic process known as the r-process will be the focal point. The r-process is an important physical process that creates almost half of the elements heavier than iron, such as uranium, gold, and many others. These elements are important to the maintenance of human life and other living things, but where and how it occurs are still not understood.

The first experiments in the world on aspects of the r-process, such as the mass, half-life, nucleic structure, and neutron capture reactions of extremely neutron-rich nuclei will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding equations of state for high density nuclear materials, information about nuclei of two to three times standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which is suggested to exist in the center of neutron stars, is obtained in J-PARC. By integrating these, it is expected that our understanding of equations of state for high density nuclear materials will be dramatically advanced. An understanding of equations of state is intimately related to the mechanisms involved in supernova and the internal structure of neutron stars. Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, an event which has been positioned as the foremost source of gravitational waves in the gravitational wave detection plan.

In performing collaborative research with the field of nuclear physics, it is important that information about fundamental physics knowledge from nuclear physics areis provided to the fields of astronomy and astrophysics for the purpose of understanding cosmic phenomena. Within this, takingTaking a broad view of the next 10 to 20 years, two points will pieces of such information are expected to be important.of particular importance. These are, first, the various properties and reactions of unstable nuclei related to nucleosynthesis and, second, equations of state for high density nuclear materialsmatter.

Regarding nucleosynthesis, while it is necessary to gain a refined understanding of high uncertainty nuclear reactions with high uncertainty that have a largesignificant effect on the evolution of stars, clarifying the nucleosynthetic process known as the r-process will be the focal point. The r-process is an important physical process that creates almostabout half of the elements heavier than iron, such as uranium, gold, and many others. These elements are important to the maintenance of human life and other living things, but where and how itthis process occurs areis still not understood.

The first experiments in the world on aspects of the r-process, such as the mass, half-life, nucleicnuclear structure, and neutron capture reactions of extremely neutron-rich nuclei will be performed at the Riken RI Beam Factory (RIBF). A large amount of nuclear data is expected to be obtained.

Regarding equations of state for high density nuclear materialsmatter, information about nuclei of two to three times standard density can be obtained at the RIBF. For higher densities, information on hypernuclei related to meson condensation, which ishave been suggested to exist in the center of neutron stars, iswill be obtained inat J-PARC. By integrating these, it is expected thatWe expect our understanding of equations of state for high density nuclear materials willmatter to be dramatically advanced by integrating these two sets of data. An understanding of equations of state is intimately related to the mechanisms involved in supernova and, as well as the internal structure of neutron stars. Furthermore, these equations directly affect the emission of gravitational waves when binary neutron stars merge, an event which has been positioned as the foremost source of gravitational waves in the gravitational wave detection plan.

医学・医療分野

物理科学・工学分野

生命科学分野

人文社会学分野

ビジネス・経済学分野

和英翻訳でよくある質問

日英翻訳3サービスの特長
プレミアム学術翻訳

お客様が翻訳内容をチェックし、変更や修正を何度でも指示できるコラボ翻訳に論理に踏み込むプレミアム英文校正(365日無料無制限再校正付)が付いた翻訳サービス。


スタンダード学術翻訳

翻訳からスタンダード英文校正までノンストップで行う標準サービス。スタンダード英文校正では、投稿先ジャーナルのフォーマットに無料で調整します。


ベーシック翻訳

日英翻訳後の英文校正が不要な方向けのリーズナブルな翻訳サービス。ノーマルスピードとハイスピードプランから選べます。

エディテージの英文校正者はどのような人たちですか?
エディテージの英文校正者は、4つの能力評価テストによる厳しい選抜により選ばれた、学術論文校正のプロです。博士号・修士号取得者、医師、 生命科学分野の英文校正の国家資格であるBELS認定取得者、学術論文出版の経験者など、学歴、研究経験または校正能力において優れた者 のみを採用しています。39%のスタッフは実際、校正者になる前に以前研究に携わっていました。その分野の優れた知識と経験、英語力を持ち、 アカデミック・コミュニケーションに情熱を持つ校正スタッフでチーム構成されています。

学術翻訳に関するその他の質問はこちらから >>