Astrophysics Research at Liverpool John Moores University

利物浦约翰摩尔斯大学天体物理学研究

• 批准号: ST/J001465/1
• 负责人: Christopher Collins
• 金额: $ 102.47万
• 依托单位: Liverpool John Moores University
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2012
• 资助国家: 英国
• 起止时间: 2012 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FJ001465%2F1
• 关键词: Astrophysics; Research; Liverpool; John; Moores

We will continue to pursue ground-breaking astrophysical research at the forefront of knowledge through both observational work and theoretical modelling. Under the heading of Time-Domain Astrophysics, we will study the explosions of Novae, Supernovae and Gamma-Ray Bursts. We will investigate the fundamental properties of Galactic and extragalactic novae, building on our considerable expertise in this area, and including a detailed investigation of the possibility that these objects are the progenitors of the important Type la Supernovae, which have become known as one of the primary probes of the scale and nature of the Universe. For supernovae that owe their origin to the collapse of the core of a massive star (Core-Collapse Supernovae), we will constrain their progenitors by investigating the environments in which they are found, coupled with detailed analyses of their outbursts. We will investigate the physics of Gamma-Ray Bursts - the most powerful explosions in the Universe. Combining cutting-edge theoretical predictions with novel observational experiments on the world's largest robotic telescopes, we will probe regions of extreme physics to determine the fundamental role of magnetic fields. In addition, we will use multi-frequency observations to determine the nature of the progenitors of these objects and the physics of the interaction of relativistic ejecta with the pre-outburst medium. Furthermore, we will explore new regions of the time domain being opened up in the radio and exploit our proven ability to build fast-track instrumentation to address new science questions.In the area of stellar evolution, we will capitalise on our leading role in some of the most ambitious ground and space-based surveys to determine the ways in which the earliest phases of the formation of stars occur. This will convert the UK's spearheading of these surveys into international leadership in the scientific interpretation of the data. Our research will also build on our expertise in stellar modelling to investigate the structure of stars at the other end of their lives by comparing our models with results from satellites on stellar vibrations.Under the heading of the formation and evolution of galaxies, we will investigate the properties of galaxies on all mass scales from the smallest to the largest. We will use new observations from the most powerful ground and space-based telescopes to study long-standing theoretical problems with the observed numbers of the smallest galaxies, and the rapid build-up of the most massive galaxies, and we will study how the evolution of galaxies is affected by their environment. We will use new instruments and theoretical modelling techniques to study in detail the manner in which gas is driven into the centres of galaxies and channelled onto the supermassive black holes that power the phenomenon of Active Galactic Nuclei, and study the important role that these objects play in the evolution of their host galaxies. Finally, we will use our results to better predict what the next generation of telescopes, such as the James Webb Space Telescope and Square Kilometre Array, will see and determine the best way for these billion-pound facilities to continue to advance our understanding of the Universe.All of our research uses the most advanced ground-based telescopes (such as our own Liverpool Telescope), satellites and data analysis techniques to carry out observations from gamma rays to radio wavelengths. In turn, ARI staff lead many of the new generation surveys with these telescopes. The projects we propose in the above areas are technically demanding and require computer software support to aid the delivery of the science. The structure and organisation of the ARI is designed to deliver internationally excellent research. The ARI is known worldwide for developing and exploiting outreach activities to engage the wider population in STFC science and we aim to enhance these.

我们将继续通过观察工作和理论建模在知识的最前沿进行突破性的天体研究。在时间域天体物理学的标题下，我们将研究Novae，Supernovae和Gamma-Ray爆发的爆炸。我们将基于我们在该领域的大量专业知识的基础上研究银河系和层次外novae的基本特性，并详细研究了这些物体是重要类型La超新星的祖细胞的可能性，这些物体已被称为宇宙规模和性质的主要探针之一。对于它们起源的超新星归因于巨大恒星的核心（核心折叠超新星）的崩溃，我们将通过研究发现它们的环境，再加上其爆发的详细分析来限制其祖细胞。我们将研究伽马射线爆发的物理学 - 宇宙中最有力的爆炸。将最先进的理论预测与世界上最大的机器人望远镜的新观测实验相结合，我们将探测极端物理的区域，以确定磁场的基本作用。此外，我们将使用多频观测来确定这些物体的祖细胞的性质以及相对论喷射与前爆发培养基的相互作用的物理。此外，我们将探索广播中开放的时域的新区域，并利用我们久经考验的能力来构建快速轨道仪器来解决新的科学问题。在恒星进化领域，我们将利用我们在一些最雄心勃勃的地面和基于太空的调查中的领先作用，以确定形成型明星的最早阶段。这将在数​​据的科学解释中将英国对这些调查的率先转换为国际领导。我们的研究还将基于我们在恒星建模方面的专业知识，以通过将我们的模型与恒星振动的卫星的结果进行比较，以研究恒星的结构。在星系的形成和演化的标准下，我们将研究星系在所有质量尺度上的星系性能，从最小的最大。我们将使用来自最强大的地面和空间望远镜的新观察结果来研究长期观察到的最小星系数量的长期理论问题，以及最庞大的星系的快速积聚，我们将研究星系的演变如何受其环境影响。我们将使用新的仪器和理论建模技术详细研究气体被驱动到星系中心并引导到超级质量的黑洞中，从而为主动银河系核的现象提供动力，并研究这些物体在宿主星系进化中起着的重要作用。 Finally, we will use our results to better predict what the next generation of telescopes, such as the James Webb Space Telescope and Square Kilometre Array, will see and determine the best way for these billion-pound facilities to continue to advance our understanding of the Universe.All of our research uses the most advanced ground-based telescopes (such as our own Liverpool Telescope), satellites and data analysis techniques to carry out observations from gamma rays to radio波长。反过来，ARI员工通过这些望远镜领导了许多新一代调查。我们在上述领域提出的项目在技术上是要求的，需要计算机软件支持以帮助提供科学。 ARI的结构和组织旨在提供国际优秀的研究。 ARI以开发和利用外展活动以吸引更广泛的人群参与STFC科学，我们旨在加强这些活动。

项目成果

Cauchy theory for the gravity water waves system with non localized initial data

具有非局域初始数据的重力水波系统的柯西理论

• DOI: 10.48550/arxiv.1305.0457
• 发表时间: 2013
• 期刊: arXiv e-prints
• 作者: Alazard Thomas

Differential cross section for reflected electrons measured by electron mirror method

电子镜法测量反射电子的微分截面

• DOI: 10.1117/1.jnp.9.093096
• 发表时间: 2015
• 期刊: Journal of Nanophotonics
• 影响因子: 1.5
• 作者: Al-Zahy Y

Extreme HBL behavior of Markarian 501 during 2012

• DOI: 10.1051/0004-6361/201833704
• 发表时间: 2018-08
• 期刊: Astronomy & Astrophysics
• 影响因子: 6.5
• 作者: M. L. Ahnen;S. Ansoldi;L. A. Antonelli;C. Arcaro;A. Babi'c;B. Banerjee;P. Bangale;U. D. Almeida;J. Barrio;J. Gonz'alez;W. Bednarek;E. Bernardini;A. Berti;W. Bhattacharyya;O. Blanch;G. Bonnoli;R. Carosi;A. Carosi;A. Chatterjee;S. M. Colak;P. Colin;E. Colombo;J. Contreras;J. Cortina;S. Covino;P. Cumani;P. D. Vela;F. Dazzi;A. Angelis;B. Lotto;M. Delfino;J. Delgado;F. D. Pierro;M. Doert;A. Domínguez;D. D. Prester-D.;M. Doro;D. Glawion;M. Engelkemeier;V. Ramazani;A. Fern'andez-Barral;D. Fidalgo;M. V. Fonseca;L. Font;C. Fruck;D. Galindo;R. L'opez;M. Garczarczyk;M. Gaug;P. Giammaria;N. Godinovi'c;D. Góra;D. Guberman;D. Hadasch;A. Hahn;T. Hassan;M. Hayashida;J. Herrera;J. Hose;D. Hrupec;K. Ishio;Y. Konno;H. Kubo;J. Kushida;D. Kuvevzdi'c;D. Lelas;E. Lindfors;S. Lombardi;F. Longo;M. L'opez;C. Maggio;P. Majumdar;M. Makariev;G. Maneva;M. Manganaro;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;U. Menzel;M. Minev;J. Miranda;R. Mirzoyan;A. Moralejo;V. Moreno;E. Moretti;T. Nagayoshi;V. Neustroev;A. Niedźwiecki;M. N. Rosillo;C. Nigro;K. Nilsson;D. Ninci;K. Nishijima;K. Noda;L. Nogu'es;S. Paiano;J. Palacio;D. Paneque;R. Paoletti;J. Paredes;G. Pedaletti;Michele Peresano;L. Perri;M. Persic;P. Moroni;E. Prandini;I. Puljak;J. Garcia;I. Reichardt;M. Rib'o;J. Rico;C. Righi;A. Rugliancich;T. Saito;K. Satalecka;S. Schroeder;T. Schweizer;S. Shore;J. Sitarek;I. vSnidari'c;D. Sobczynska;A. Stamerra;M. Strzys;T. Suri'c;L. Takalo;F. Tavecchio;P. Temnikov;T. Terzi'c;M. Teshima;N. Torres-Albà;A. Treves;S. Tsujimoto;G. Vanzo;M. Acosta;I. Vovk;J. Ward;M. Will;D. Zari'c;A. Arbet-Engels;D. Baack;M. Balbo;A. Biland;M. Blank;T. Bretz;K. Bruegge;M. Bulinski;J. Buss;A. Dmytriiev;D. Dorner;S. Einecke;D. Elsaesser;T. Herbst;D. Hildebrand;L. Kortmann;L. Linhoff;M. Mahlke;K. Mannheim;S. Mueller;D. Neise;A. Neronov;M. Noethe;J. Oberkirch;A. Paravac;W. Rhode;B. Schleicher;F. Schulz;K. Sedlaczek;A. Shukla;V. Sliusar;R. Walter;A. Archer;W. Benbow;R. Bird;R. Brose;J. Buckley;V. Bugaev;J. Christiansen;W. Cui;M. Daniel;A. Falcone;Q. Feng;J. Finley;G. Gillanders;O. Gueta;D. Hanna;O. Hervet;J. Holder;G. Hughes;M. Hutten;T. Humensky;C. Johnson;P. Kaaret;P. Kar;N. Kelley-Hoskins;M. Kertzman;D. Kieda;M. Krause;F. Krennrich;S. Kumar;M. Lang;T. T. Lin-T.;G. Maier;S. McArthur;P. Moriarty;R. Mukherjee;S. O’Brien;R. Ong;A. Otte;N. Park;A. Petrashyk;A. Pichel;M. Pohl;J. Quinn;K. Ragan;P. Reynolds;G. Richards;E. Roache;A. Rovero;C. Rulten;I. Sadeh;M. Santander;G. Sembroski;K. Shahinyan;I. Sushch;J. Tyler;S. Wakely;A. Weinstein;R. Wells;P. Wilcox;A. Wilhel;D. Williamson;B. Zitzer;M. Perri;F. Verrecchia;C. Leto;M. Villata;C. Raiteri;S. Jorstad;V. Larionov;D. Blinov;T. Grishina;E. Kopatskaya;E. Larionova;A. Nikiforova;D. Morozova;Y. Troitskaya;I. Troitsky;O. Kurtanidze;M. Nikolashvili;S. O. Kurtanidze;G. Kimeridze;R. Chigladze;A. Strigachev;A. Sadun;J. Moody;W. P. Chen;H. C. Lin;J. Acosta-Pulido;M. Ar'evalo;M. Carnerero;P. A. Gonz'alez-Morales;A. Manilla-Robles;H. Jermak;I. Steele;C. Mundel;E. Ben'itez;D. Hiriart;P. Smith;W. Max-Moerbeck;A. Readhead;J. Richards;T. Hovatta;A. Lahteenmaki;M. Tornikoski;J. Tammi;M. Georganopoulos;M. V. E. Zurich;CH-8093 Zurich;Switzerland.;U. Udine;I. Trieste;I. Udine;Italy.;National Centre for Radio Astrophysics;I. Rome;U. Padova;Infn;I-35131 Padova;C. Rijeka;51000 Rijeka;U. O. S. -. Fesb;21000 Split;U. O. Z. -. Fer;10000 Zagreb;University of Osijek;Osijek;Rudjer Boskovic Institute;Zagreb;Croatia.;Saha Institute of Nuclear Physics;Hbni;1. Bidhannagar;Salt Lake;Sector-1;Kolkata 700064;India.;M. F. Physik;D-80805 Munchen;H Germany;U. Complutense;Madrid;Spain.;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;E-38200 La Laguna;U. L. Laguna;D. Astrof'isica;E-38200 La Laguna;Tenerife;University of L'od'z;D. O. Astrophysics;PL-90236 L'od'z;Poland;D. Elektronen-Synchrotron;D. Zeuthen;Institut de F'isica d'Altes Energies;T. Science;Technology;E-08193 Bellaterra;U. Siena;I. Pisa;I-53100 Siena;Technische Universitat Dortmund;D. Dortmund;U. Wurzburg;D-97074 Wurzburg;Finnish Magic Consortium Tuorla Observatory;Finnish Magic Consortium Finnish Centre of Astronomy with Eso-Finnish-Magic-Consortium-Finnish-Centre-of-with-Eso-1387882574;U. Turku;20 Vaisalantie;FI-21500 Piikkio;A. Division;U. Oulu;F. Oulu;Finland.;D. D. F'isica-D.;CERES-IEEC;U. Barcelona;U. Barcelona;Icc;IEEC-UB;J. Icrr;T. U. O. Tokyo;D. Physics;Kyoto University;T. University;The University of Tokushima;Inst. for Nucl. Research;Nucl. Energy;B. Pisa;I. Pisa;Now at Centro Brasileiro de Pesquisas F'isicas;22290-180 Urca;R. Janeiro;Brasil.;H. Berlin;I. Germany;A. N. D. D. Fisica-A.-N.-D.-D.-Fisica-1387882413;Universita di UdineI.N.F.N. Trieste;Trieste;A. Spain;also at INAF-Trieste;D. PhysicsAstronomy;U. Bologna;U. Geneva;I. D. C. F. Astrophysics;also at the Department of Physics of Kyoto University-also-at-the-Department-of-Physics-of-Kyoto-1388334149;A. III.PhysikalischesInstitut;Aachen;W. University;S. Louis;MO Fred Lawrence Whipple Observatory;H. C. F. Astrophysics;Amado;A. D. O. Physics;Astronomy;U. California;L. Angeles;C. I. O. Physics;U. Potsdam;P. Department;California State Polytechnic University;S. Obispo;C. I. O. Physics;P. University;W. Lafayette;I. Physics;Center for Computational Astrophysics;Tsinghua University;Beijing;China.;D. O. Astronomy;Astrophysics;P. S. University;U. Park;Particle Physics Department;M. University;Montreal.;QC H3A 2T8;Canada.;S. O. Physics;National University of Ireland Galway;University Road;Galway.;Ireland;Santa Cruz Institute for Particle Physics;Santa Cruz;the Bartol Research Institute;U. Delaware;Newark;D. P. Department;C. University;New York.;N. D. O. Physics;U. Iowa;Van Allen Hall;Iowa City;IA Department of Physics;U. Utah;Salt lake City;UT Department of Physics;D. University;I. S. University;Barnard College;University College Dublin;Center for Computational Astrophysics;G. I. O. Technology;Enrico Fermi Institute;U. Chicago;Instituto de Astronom'ia y F'isica del Espacio;28 CC67-Suc.;Ciudad de Buenos Aires;Arg;A. D. O. P. Sciences;C. I. O. Technology;Bishopstown;Cork;U. Minnesota;U. Alabama;now at Fred Lawrence Whipple Observatory;S. S. D. C. -. Asi-S.;-INAF;Osservatorio Astronomico di Roma;Osservatorio Astrofisico di Torino;A. Institute;S. University;P. Observatory;St.-Petersburg;Russia.;Institute for Theoretical;C. Physics;U. Crete;F. F. Research-F.;Technology - Hellas;Iesl;Voutes;7. Heraklion;Greece.;A. Observatory;E. A. Observatory;Kazan Federal University;Xinjiang Astronomical Observatory;Chinese Academy of Sciences;I. O. Astronomy;N. A. Observatory;Bulgarian academy of Sciences;U. Denver;Brigham Young University;G. I. O. Astronomy;National Central University;E. Observatory;A. R. Institute;Liverpool John Moores University;I. D. Astronom'ia;Universidad Nacional Autnoma de M'exico;S. Observatory;U. Arizona;U. Chile;D. D. Astronom'ia-D.;C. 9. Astronomy;C. I. O. Technology.;T. Observatory;A. L. M. R. Observatory;Aalto University Department of Electronics;Nanoengineering;U. M. County;Nasa Goddard Space Flight Center;Astronomy - MS 108;R. University;Inst. for Nucl. Research;Boston University

VizieR Online Data Catalog: W3(H2O/OH) continuum & line data cubes at 1.3mm (Ahmadi+, 2018)

VizieR 在线数据目录：W3(H2O/OH) 连续体

• DOI: 10.26093/cds/vizier.36180046
• 发表时间: 2018
• 期刊: VizieR Online Data Catalog
• 作者: Ahmadi A.

GAMA/H-ATLAS: linking the properties of submm detected and undetected early-type galaxies - I. z = 0.06 sample

GAMA/H-ATLAS：将已检测到的亚毫米级星系和未检测到的早期型星系的特性联系起来 - I. z = 0.06 样本

• DOI: 10.1093/mnras/stt310
• 发表时间: 2013
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Agius N