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Queen's University Belfast Astronomy Observation and Theory Consolidated Grant 2020-2023

贝尔法斯特女王大学天文学观测和理论综合补助金 2020-2023

基本信息

批准号：
ST/T000198/1
负责人：
Stephen Smartt
金额：
$ 117.31万
依托单位：
Queen's University Belfast
依托单位国家：
英国
项目类别：
Research Grant
财政年份：
2020
资助国家：
英国
起止时间：
2020 至无数据
项目状态：
未结题

来源：
https://gtr.ukri.org/projects?ref=ST%2FT000198%2F1
关键词：
Queen University Belfast Astronomy Observation

项目摘要

Supernovae create the heavy chemical elements we see in our solar system, the Galaxy and entire visible Universe. While stars evolve over millions or billions of years, a supernova explosion happens in seconds and the glowing remnant lasts for years. We aim to understand how these explosions happen and how they create the neutron stars, pulsars and black holes in our galaxy. In 2017 a breakthrough discovery was made when the first electromagnetic counterpart to a gravitational wave source was found. This was termed a kilonova because it was 1000 times brighter than a nova. The gravitational waves and the kilonova were from a pair of merging neutron stars. The optical and infrared light arose from the radioactive decay of heavy elements, which we call r-process elements. These are heavier than iron in the periodic table and such neutron star mergers may be responsible for all these heavy elements. Or projects will find more of these in the coming years and the combination of gravitational waves and electromagnetic signals opens up a new window on the Universe. The thermonuclear supernovae that are used as cosmic yardsticks and led to the Nobel Prize winning discovery of dark energy come from white dwarf stars. But exactly how they explode and what the progenitor systems are still eludes us. A white dwarf is a star greater than the mass of the sun, but the size of the earth. They are incredibly dense, one teaspoon of WD material weighs about 10 thousand tonnes. To understand how they explode, we will model their spectra with the most sophisticated 3 dimensional computer models that currently exist. The elements created in supernovae form planetary systems in our galaxy - iron, silicon, oxygen, magnesium are all critical to forming planetary systems. The diversity in the known planetary systems around other stars in our galaxy (called exoplanets) is astounding. We know of thousands of exoplanets. Hot Jupiters, multiple planetary systems and super-earths are now commonly found in surveys to discover new planets. We can see planet formation in the disks of young stars during their first few million years of life. The latest large facility built in the southern hemisphere (ALMA), has provided spectacular data on proto-planetary disks and our work on the chemistry of the disk aims to understand their origins. Our top priority in this area is to find another earth like planet - the right size, age and distance from its parent star to support an atmosphere and liquid water. This search requires careful tests of the methods to extract the tiny signals we expect and we propose to develop this with an eye on the future prize of detecting an earth twin. We will soon have extraordinarily precise spectrometers on the biggest telescopes to measure the velocity of stars down to metres per second. At this level, it is no longer the instrument measuring precision that hinders our planet searching, but the real activity on the surface of Sun like stars. Our project will aim to understand and mitigate this effect. A critical part of astrophysics is pulling together our detailed knowledge of physics that we can measure on earth to what we can only see (through electromagnetic radiation) in the distant Universe. This will be done through computer calculations of model atoms. These codes calculate how electrons are excited in atoms and ensures that astrophysical models identify the elements that cause the spectral lines in supernovae, supermassive black holes, galaxy spectra and stars. Now that we have detected a kilonova we must do the same calculations for the heaviest elements. We will also run novel experiments to use powerful lasers (e.g. the VULCAN laser) to mimic the physics of gas that causes x-ray emission in accreting sources such as black hole binaries. We will use these novel laboratory data to test the world's leading computer code that is used to model the central regions of galaxies close to their black holes.

超新星创造了我们在太阳系、银河系和整个可见宇宙中看到的重化学元素。虽然恒星的演化经历了数百万或数十亿年，但超新星爆炸在几秒钟内就发生了，而发光的残骸会持续数年。我们的目标是了解这些爆炸是如何发生的，以及它们是如何在我们的星系中创造出中子星、中子星和黑洞的。2017年，当第一个引力波源的电磁对应物被发现时，取得了突破性的发现。这被称为千新星，因为它比新星亮1000倍。引力波和千诺瓦波来自一对合并的中子星。可见光和红外光来自重元素的放射性衰变，我们称之为r过程元素。在元素周期表中，这些元素比铁重，中子星星的合并可能是所有这些重元素的原因。或者在未来几年内，项目将发现更多这样的东西，引力波和电磁信号的结合为宇宙打开了一扇新的窗户。被用作宇宙尺度的热核超新星来自白色矮星，它们导致了诺贝尔奖获得者对暗能量的发现。但它们究竟是如何爆炸的，以及它们的祖先系统是什么，我们仍然不清楚。一颗白色矮星是一颗比太阳质量大，但和地球大小相当的星星。它们的密度令人难以置信，一茶匙WD材料重约1万吨。为了了解它们是如何爆炸的，我们将用目前存在的最复杂的三维计算机模型来模拟它们的光谱。超新星中产生的元素形成了我们银河系中的行星系统-铁，硅，氧，镁都是形成行星系统的关键。我们银河系中其他恒星周围的已知行星系统（称为系外行星）的多样性令人震惊。我们知道有上千颗系外行星。热彗星、多行星系统和超级地球现在经常出现在发现新行星的调查中。我们可以看到年轻恒星在其生命的最初几百万年期间在其盘中形成行星。在南半球建造的最新大型设施（阿尔马）提供了关于原行星盘的壮观数据，我们对盘的化学工作旨在了解它们的起源。我们在这一领域的首要任务是找到另一颗类似地球的行星--合适的大小、年龄和与其母星星的距离，以支持大气层和液态水。这项研究需要对提取我们期望的微小信号的方法进行仔细测试，我们建议开发这一方法，并着眼于未来探测地球孪生兄弟的奖励。我们很快就会在最大的望远镜上安装非常精确的光谱仪，测量恒星的速度，精确到每秒米。在这个层面上，阻碍我们行星搜索的不再是仪器的测量精度，而是太阳表面类似恒星的真实的活动。我们的项目旨在了解和减轻这种影响。天体物理学的一个关键部分是将我们在地球上可以测量的详细物理知识与我们只能在遥远的宇宙中看到的（通过电磁辐射）结合起来。这将通过模型原子的计算机计算来完成。这些代码计算电子如何在原子中被激发，并确保天体物理模型识别导致超新星，超大质量黑洞，星系光谱和恒星光谱线的元素。既然我们已经探测到了一个千诺瓦，我们必须对最重的元素做同样的计算。我们还将进行新的实验，使用强大的激光器（例如VULCAN激光器）来模拟在吸积源（如黑洞双星）中引起x射线发射的气体物理学。我们将使用这些新的实验室数据来测试世界领先的计算机代码，该代码用于模拟靠近黑洞的星系中心区域。

项目成果

期刊论文数量（9）

专著数量（0）

科研奖励数量（0）

会议论文数量（0）

专利数量（0）

Multiwavelength Observations of the Blazar PKS 0735+178 in Spatial and Temporal Coincidence with an Astrophysical Neutrino Candidate IceCube-211208A

布拉扎尔 PKS 0735 178 与天体物理中微子候选者 IceCube-211208A 时空重合的多波长观测

DOI：
10.3847/1538-4357/ace327
发表时间：
2023
期刊：
The Astrophysical Journal
影响因子：
0
作者：
Acharyya, A.;Adams, C. B.;Archer, A.;Bangale, P.;Bartkoske, J. T.;Batista, P.;Benbow, W.;Brill, A.;Buckley, J. H.;Christiansen, J. L.
通讯作者：
Christiansen, J. L.

VERITAS Discovery of Very High Energy Gamma-Ray Emission from S3 1227+25 and Multiwavelength Observations

DOI：
10.3847/1538-4357/acd2d0
发表时间：
2023-05
期刊：
The Astrophysical Journal
影响因子：
0
作者：
A. Acharyya;C. Adams;A. Archer;P. Bangale;W. Benbow;A. Brill;J. Christiansen;A. Chromey;M. Errando;A. Falcone;Q. Feng;J. Finley;G. Foote;L. Fortson;A. Furniss;G. Gallagher;W. Hanlon;D. Hanna;O. Hervet;C. Hinrichs;J. Hoang;J. Holder;Weidong Jin;Madalyn Johnson;P. Kaaret;M. Kertzman;D. Kieda;T. Kleiner;N. Korzoun;F. Krennrich;Mark Lang;Matt Lundy;G. Maier;Conor McGrath;M. Millard;J. Millis;Connor Mooney;P. Moriarty;R. Mukherjee;S. O’Brien;R. Ong;M. Pohl;E. Pueschel;J. Quinn;K. Ragan;Paul Reynolds;D. Ribeiro;E. Roache;I. Sadeh;A. Sadun;L. Saha;M. Santander;G. Sembroski;R. Shang;M. Splettstoesser;A. Talluri;J. Tucci;V. Vassiliev;David Williams;S. Wong;T. Hovatta;S. Jorstad;S. Kiehlmann;A. Lahteenmaki;I. Liodakis;A. Marscher;W. Max-Moerbeck;A. Readhead;R. Reeves;Paul S. Smith;M. Tornikoski
通讯作者：
A. Acharyya;C. Adams;A. Archer;P. Bangale;W. Benbow;A. Brill;J. Christiansen;A. Chromey;M. Errando;A. Falcone;Q. Feng;J. Finley;G. Foote;L. Fortson;A. Furniss;G. Gallagher;W. Hanlon;D. Hanna;O. Hervet;C. Hinrichs;J. Hoang;J. Holder;Weidong Jin;Madalyn Johnson;P. Kaaret;M. Kertzman;D. Kieda;T. Kleiner;N. Korzoun;F. Krennrich;Mark Lang;Matt Lundy;G. Maier;Conor McGrath;M. Millard;J. Millis;Connor Mooney;P. Moriarty;R. Mukherjee;S. O’Brien;R. Ong;M. Pohl;E. Pueschel;J. Quinn;K. Ragan;Paul Reynolds;D. Ribeiro;E. Roache;I. Sadeh;A. Sadun;L. Saha;M. Santander;G. Sembroski;R. Shang;M. Splettstoesser;A. Talluri;J. Tucci;V. Vassiliev;David Williams;S. Wong;T. Hovatta;S. Jorstad;S. Kiehlmann;A. Lahteenmaki;I. Liodakis;A. Marscher;W. Max-Moerbeck;A. Readhead;R. Reeves;Paul S. Smith;M. Tornikoski

A precursor plateau and pre-maximum [O ii ] emission in the superluminous SN2019szu: a pulsational pair-instability candidate

超光速 SN2019szu 中的前驱平台和最大前 [O ii ] 发射：脉动对不稳定性候选者