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.

超新星创建了我们在太阳系，星系和整个可见宇宙中看到的重型化学元素。尽管星星发展了数百万或数十亿年，但超新星爆炸发生了几秒钟，而发光的残余持续了多年。我们的目标是了解这些爆炸是如何发生的，以及它们如何在我们的银河系中创建中子恒星，脉冲星和黑洞。 2017年，当发现第一个与重力波源的电磁对应物时，进行了突破性的发现。这被称为基洛诺瓦，因为它比新星亮1000倍。引力波和Kilonova来自一对合并的中子星。光学和红外光来自重型元素的放射性衰减，我们称之为R过程。这些在元素周期表中比铁重，并且这种中子星的合并可能是所有这些重元素的原因。否则，项目将在未来几年中找到更多，而引力波和电磁信号的组合为宇宙打开了一个新窗口。被用作宇宙码的热核超新星，并导致诺贝尔奖获得了黑矮星的奖。但是，它们的爆炸方式和祖细胞系统的爆炸方式准确，仍然使我们感到困惑。白矮人比太阳的质量大，但大小的恒星大。它们的密度令人难以置信，一茶匙的WD材料重约10万吨。为了了解它们的爆炸方式，我们将使用当前存在的最复杂的3维计算机模型来对其光谱进行建模。用超新星形成的元素形成了我们的星系中的行星系统 - 铁，硅，氧，镁，对于形成行星系统至关重要。我们银河系中其他恒星周围已知的行星系统的多样性令人震惊。我们知道成千上万的系外行星。现在在调查中通常发现了发现新行星的热木星，多个行星系统和超级地铁。我们可以在年轻恒星的头几百万年生命中看到星球在年轻恒星的磁盘中形成。在南半球（ALMA）建造的最新大型设施，提供了有关原始磁盘的壮观数据，以及我们在磁盘化学方面的工作旨在了解其起源。我们在这一领域的首要任务是找到另一个像行星这样的地球 - 距离其母星的尺寸，年龄和距离，以支持大气和液态水。这次搜索需要仔细测试方法，以提取我们期望的微小信号，并提议开发此方法，以期待未来检测地球双胞胎的奖项。我们很快将在最大的望远镜上具有非常精确的光谱仪，以测量恒星的速度至每秒米。在这个级别上，不再是仪器测量精度阻碍我们的星球搜索的仪器，而是像恒星一样的真实活动。我们的项目旨在了解和减轻这种效果。天体物理学的关键部分是将我们对物理学的详细知识汇总在一起，我们可以在地球上测量到遥远宇宙中只能看到（通过电磁辐射）。这将通过模型原子的计算机计算来完成。这些代码计算了电子在原子中的激发方式，并确保天体物理模型确定引起超新星，超大质量黑洞，星系光谱和恒星中光谱线的元素。现在，我们已经检测到了Kilonova，我们必须对最重的元素进行相同的计算。我们还将运行新颖的实验，以使用强大的激光器（例如瓦肯激光）来模仿在积聚源（例如黑洞二进制文件）中导致X射线发射的气体物理。我们将使用这些新颖的实验室数据测试世界领先的计算机代码，该计算机代码用于建模靠近其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