Annual Review of Astronomy and Astrophysics最新文献

Extragalactic Archaeology: The Assembly History of Galaxies from Dynamical and Stellar Population Models 河外考古学：从动力学和恒星人口模型看星系的集合史

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2025-05-29 DOI: 10.1146/annurev-astro-052622-025659

Glenn van de Ven, Jesús Falcón-Barroso, Mariya Lyubenova

{"title":"Extragalactic Archaeology: The Assembly History of Galaxies from Dynamical and Stellar Population Models","authors":"Glenn van de Ven, Jesús Falcón-Barroso, Mariya Lyubenova","doi":"10.1146/annurev-astro-052622-025659","DOIUrl":"https://doi.org/10.1146/annurev-astro-052622-025659","url":null,"abstract":"In this review, we show how combining dynamical and stellar population models with integral field spectroscopic data of nearby galaxies enable uncovering their assembly history. ▪ We discuss the advantages and limitations of various dynamical modelling approaches, focusing on measuring the mass distributions of nearby galaxies, including central black holes and dark matter halos. ▪ We highlight the use of Schwarzschild's orbit-superposition method to robustly decompose galaxies into dynamically distinct components and derive their intrinsic properties. ▪ We cover the application of single stellar population models to interpret observations of unresolved stars in nearby galaxies. ▪ We outline how combining dynamical and stellar population models can reveal the fossil records of galaxy assembly, from the origin of inner galaxy structures, to the buildup of disks, to the recovery of past galaxy mergers. We close by demonstrating how these models of nearby galaxies provide a bridge between studies of resolved stars in the local Universe and high-redshift galaxy observations. Together with direct coupling to state-of-the-art cosmological simulations, extragalactic archaeology promises key insights into galaxy formation and evolution.","PeriodicalId":8138,"journal":{"name":"Annual Review of Astronomy and Astrophysics","volume":"147 1","pages":""},"PeriodicalIF":33.3,"publicationDate":"2025-05-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144176516","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Formation of Giant Planets 巨行星的形成

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2025-05-28 DOI: 10.1146/annurev-astro-052722-094843

Masahiro Ikoma, Hiroshi Kobayashi

引用次数: 0

Relativistic Magnetic Reconnection in Astrophysical Plasmas: A Powerful Mechanism of Nonthermal Emission 天体物理等离子体中的相对论性磁重联：一种强大的非热辐射机制

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2025-05-22 DOI: 10.1146/annurev-astro-020325-115713

Lorenzo Sironi, Dmitri A. Uzdensky, Dimitrios Giannios

{"title":"Relativistic Magnetic Reconnection in Astrophysical Plasmas: A Powerful Mechanism of Nonthermal Emission","authors":"Lorenzo Sironi, Dmitri A. Uzdensky, Dimitrios Giannios","doi":"10.1146/annurev-astro-020325-115713","DOIUrl":"https://doi.org/10.1146/annurev-astro-020325-115713","url":null,"abstract":"Magnetic reconnection—a fundamental plasma physics process, where magnetic field lines of opposite polarity annihilate—is invoked in astrophysical plasmas as a powerful mechanism of nonthermal particle acceleration, able to explain fast-evolving, bright high-energy flares. Near black holes and neutron stars, reconnection occurs in the relativistic regime, in which the mean magnetic energy per particle exceeds the rest mass energy. This review reports recent advances in our understanding of the kinetic physics of relativistic reconnection: ▪ Kinetic simulations have elucidated the physics of plasma heating and nonthermal particle acceleration in relativistic reconnection (RR). ▪ The physics of radiative RR, with its self-consistent interplay between photons and reconnection-accelerated particles—a peculiarity of luminous, high-energy astrophysical sources—is the new frontier of research. ▪ RR plays a key role in global models of high-energy sources, in terms of both global-scale layers as well as reconnection sites generated as a by-product of local magnetohydrodynamic instabilities. We summarize themes of active investigation and future directions, emphasizing the role of upcoming observational capabilities, laboratory experiments, and new computational tools.","PeriodicalId":8138,"journal":{"name":"Annual Review of Astronomy and Astrophysics","volume":"3 1","pages":""},"PeriodicalIF":33.3,"publicationDate":"2025-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144113678","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

High-Contrast Coronagraphy 高对比度Coronagraphy

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2025-05-19 DOI: 10.1146/annurev-astro-021225-022840

Matthew A. Kenworthy, Sebastiaan Y. Haffert

{"title":"High-Contrast Coronagraphy","authors":"Matthew A. Kenworthy, Sebastiaan Y. Haffert","doi":"10.1146/annurev-astro-021225-022840","DOIUrl":"https://doi.org/10.1146/annurev-astro-021225-022840","url":null,"abstract":"Imaging terrestrial exoplanets around nearby stars is a formidable technical challenge, requiring the development of coronagraphs to suppress the stellar halo of diffracted light at the location of the planet. In this review, we discuss the science requirements for high-contrast imaging, present an overview of diffraction theory and the Lyot coronagraph, and define the parameters used in our optimization. We discuss the working principles of coronagraphs both in the laboratory and on-sky with current high-contrast instruments, and we describe the required algorithms and processes necessary for terrestrial planet imaging with extremely large telescopes and proposed space telescope missions: ▪ Imaging terrestrial planets around nearby stars is possible with a combination of coronagraphs and active wavefront control using feedback from wavefront sensors. ▪ Ground-based 8–40 m class telescopes can target the habitable zone around nearby M-dwarf stars with contrasts of 10−7, and space telescopes can search around solar-type stars with contrasts of 10−10. ▪ Focal plane wavefront sensing, hybrid coronagraph designs, and multiple closed loops providing active correction are required to reach the highest sensitivities. ▪ Polarization effects need to be mitigated in order to reach 10−10 contrasts while keeping exoplanet yields as high as possible. ▪ Recent technological developments, including photonics and microwave kinetic inductance detectors, will be folded into high-contrast instruments. ","PeriodicalId":8138,"journal":{"name":"Annual Review of Astronomy and Astrophysics","volume":"73 1","pages":""},"PeriodicalIF":33.3,"publicationDate":"2025-05-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144097300","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Exoplanet Atmospheres at High Spectral Resolution 高光谱分辨率的系外行星大气

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2025-05-14 DOI: 10.1146/annurev-astro-052622-031342

Ignas A.G. Snellen

{"title":"Exoplanet Atmospheres at High Spectral Resolution","authors":"Ignas A.G. Snellen","doi":"10.1146/annurev-astro-052622-031342","DOIUrl":"https://doi.org/10.1146/annurev-astro-052622-031342","url":null,"abstract":"High-resolution spectroscopy (HRS) has grown into one of the main techniques for characterizing the atmospheres of extrasolar planets. High spectral resolving power allows for the efficient removal of telluric and host-star contamination. Combined with the large collecting area of ground-based telescopes, it enables detailed studies of atmospheric species, temperature structure, atmospheric loss, and global winds and circulation patterns. In this review, the wide range of HRS observation and data analysis techniques are described and literature results discussed. Key findings include the following: ▪ The highest irradiated planets show a rich spectrum of atomic and ionic species, just like stars. ▪ Retrieval analyses of hot Jupiters and directly imaged super-Jupiters point to solar metallicities and chemistry, but observed samples are still heterogeneous and incomplete. ▪ There appears to be a clear dichotomy between hot Jupiters with and without atmospheric inversions, depending on their equilibrium temperature. ▪ Some highly irradiated planets exhibit enormous leading and/or trailing tails of helium gas, providing unique insights into planet evolution and atmospheric escape processes. ▪ Minor isotopes of carbon and oxygen are now being detected in gas giant planets and brown dwarfs with the interesting potential to shed light on formation pathways. A list of potential pitfalls is provided for those new to the field, and synergies with the James Webb Space Telescope are discussed. HRS has a great future ahead with the advent of the extremely large telescopes, promising to bring temperate rocky exoplanets into view with their increase in HRS detection speed of up to three orders of magnitude.","PeriodicalId":8138,"journal":{"name":"Annual Review of Astronomy and Astrophysics","volume":"42 1","pages":""},"PeriodicalIF":33.3,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143979339","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Star Formation from Low to High Mass: A Comparative View 从低质量到高质量的恒星形成：比较视角

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2025-04-01 DOI: 10.1146/annurev-astro-013125-122023

H. Beuther, R. Kuiper, M. Tafalla

{"title":"Star Formation from Low to High Mass: A Comparative View","authors":"H. Beuther, R. Kuiper, M. Tafalla","doi":"10.1146/annurev-astro-013125-122023","DOIUrl":"https://doi.org/10.1146/annurev-astro-013125-122023","url":null,"abstract":"Star formation has often been studied by separating the low- and high-mass regimes with an approximate boundary at 8 M⊙. Although some of the outcomes of the star-formation process are different between the two regimes, it is less clear whether the physical processes leading to these outcomes are that different at all. Here, we systematically compare low- and high-mass star formation by reviewing the most important processes and quantities from an observational and theoretical point of view. We identify three regimes in which processes are either similar, quantitatively, or qualitatively different between low- and high-mass star formation. ▪ Similar characteristics can be identified for the turbulent gas properties and density structures of the star-forming regions. Many of the observational characteristics also do not depend that strongly on the environment. ▪ Quantitative differences can be found for outflow, infall, and accretion rates as well as mean column and volume densities. Also, the multiplicity significantly rises from low- to high-mass stars. The importance of the magnetic field for the formation processes appears still less well constrained. ▪ Qualitative differences between low- and high-mass star formation relate mainly to the radiative and ionizing feedback that occurs almost exclusively in regions forming high-mass stars. Nevertheless, accretion apparently can continue via disk structures in ionized accretion flows. Finally, we discuss to what extent a unified picture of star formation over all masses is possible and which issues need to be addressed in the future.","PeriodicalId":8138,"journal":{"name":"Annual Review of Astronomy and Astrophysics","volume":"21 1","pages":""},"PeriodicalIF":33.3,"publicationDate":"2025-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143775385","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The Star–Planet Composition Connection 恒星与行星构成的联系

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2024-09-13 DOI: 10.1146/annurev-astro-071221-053007

Johanna K. Teske

{"title":"The Star–Planet Composition Connection","authors":"Johanna K. Teske","doi":"10.1146/annurev-astro-071221-053007","DOIUrl":"https://doi.org/10.1146/annurev-astro-071221-053007","url":null,"abstract":"The mantra “know thy star, know thy planet” has proven to be very important for many aspects of exoplanet science. Here I review how stellar abundances inform our understanding of planet composition and, thus, formation and evolution. In particular, I discuss how: ▪ The strongest star–planet connection is still the giant planet–metallicity correlation, the strength of which may indicate a break point between the formation of planets versus brown dwarfs. ▪ We do not have very good constraints on the lower metallicity limit for planet formation, although new statistics from TESS are helping, and it appears that, at low [Fe/H], α elements can substitute for iron as seeds for planet formation. ▪ The depletion of refractory versus volatile elements in stellar photospheres (particularly the Sun) was initially suggested as a sign of small planet formation but is challenging to interpret, and small differences in binary star compositions can be attributed mostly to processes other than planet formation. ▪ We can and should go beyond comparisons of the carbon-to-oxygen ratio in giant planets and their host stars, incorporating other volatile and refractory species to better constrain planet formation pathways. ▪ There appears to be a positive correlation between small planet bulk density and host star metallicity, but exactly how closely small planet refractory compositions match those of their host stars—and their true diversity—is still uncertain.","PeriodicalId":8138,"journal":{"name":"Annual Review of Astronomy and Astrophysics","volume":"63 1","pages":""},"PeriodicalIF":33.3,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142231550","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Solar Flare Spectroscopy 太阳耀斑光谱学

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2024-09-13 DOI: 10.1146/annurev-astro-052920-010547

Lyndsay Fletcher

{"title":"Solar Flare Spectroscopy","authors":"Lyndsay Fletcher","doi":"10.1146/annurev-astro-052920-010547","DOIUrl":"https://doi.org/10.1146/annurev-astro-052920-010547","url":null,"abstract":"This review covers the techniques, observations, and inferences of solar flare spectroscopy. It is not a spectroscopist's view of solar flares but rather a solar flare physicist's view of spectroscopy. Spectroscopy is carried out across the electromagnetic spectrum, but this review emphasizes the optical to soft X-ray part of the spectrum and discusses results from spectroscopy applied to the preflare, impulsive, and gradual phases, as well as a few highlights from modeling. ▪ The main spectroscopic signatures of the preflare phase are line broadening in optically thin ultraviolet to soft X-ray lines and small Doppler shifts in active region filaments that are becoming unstable. ▪ In the impulsive phase, fast upflows of heated plasma into the corona and slow downflows of cooler chromospheric plasma take place at the sites of strong chromospheric energy deposition. ▪ Radiation-hydrodynamic modeling of optically thick spectral lines gives a picture of an impulsive-phase chromosphere with a dense, heated layer deep in the atmosphere and an overlying, downward moving condensation that is partially optically thin. ▪ Gradual-phase observations show us the heated coronal plasma cooling and draining but also provide evidence for ongoing slow energy input and slow upflows in other locations. ▪ Interesting hints of non-Maxwellian and nonequilibrium plasmas have been found, along with possible evidence of plasma turbulence from line broadening.","PeriodicalId":8138,"journal":{"name":"Annual Review of Astronomy and Astrophysics","volume":"3 1","pages":""},"PeriodicalIF":33.3,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142231553","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A Tale of Many H0 许多 H0 的故事

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2024-07-23 DOI: 10.1146/annurev-astro-052622-033813

Licia Verde, Nils Schöneberg, Héctor Gil-Marín

{"title":"A Tale of Many H0","authors":"Licia Verde, Nils Schöneberg, Héctor Gil-Marín","doi":"10.1146/annurev-astro-052622-033813","DOIUrl":"https://doi.org/10.1146/annurev-astro-052622-033813","url":null,"abstract":"▪The Hubble parameter, H0, is not an univocally defined quantity: It relates redshifts to distances in the near Universe, but it is also a key parameter of the ΛCDM standard cosmological model. As such, H0 affects several physical processes at different cosmic epochs and multiple observables. We have counted more than a dozen H0s that are expected to agree if (a) there are no significant systematics in the data and their interpretation and (b) the adopted cosmological model is correct.▪With few exceptions (proverbially confirming the rule), these determinations do not agree at high statistical significance; their values cluster around two camps: the low (68 km s1 Mpc1) and high (73 km s1 Mpc1) camps. It appears to be a matter of anchors. The shape of the Universe expansion history agrees with the model; it is the normalizations that disagree.▪Beyond systematics in the data/analysis, if the model is incorrect, there are only two viable ways to “fix” it: by changing the early time (z ≳ 1,100) physics and, thus, the early time normalization or by a global modification, possibly touching the model's fundamental assumptions (e.g., homogeneity, isotropy, gravity). None of these three options has the consensus of the community.▪The research community has been actively looking for deviations from ΛCDM for two decades; the one we might have found makes us wish we could put the genie back in the bottle.","PeriodicalId":8138,"journal":{"name":"Annual Review of Astronomy and Astrophysics","volume":"43 1","pages":""},"PeriodicalIF":33.3,"publicationDate":"2024-07-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141755178","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Theory and Observation of Winds from Star-Forming Galaxies 恒星形成星系风的理论与观测

IF 33.3 1区物理与天体物理

Annual Review of Astronomy and Astrophysics Pub Date : 2024-07-23 DOI: 10.1146/annurev-astro-041224-011924

Todd A. Thompson, Timothy M. Heckman

{"title":"Theory and Observation of Winds from Star-Forming Galaxies","authors":"Todd A. Thompson, Timothy M. Heckman","doi":"10.1146/annurev-astro-041224-011924","DOIUrl":"https://doi.org/10.1146/annurev-astro-041224-011924","url":null,"abstract":"Galactic winds shape the stellar, gas, and metal content of galaxies. To quantify their impact, we must understand their physics. We review potential wind-driving mechanisms and observed wind properties, with a focus on the warm ionized and hot X-ray-emitting gas. Energy and momentum injection by supernovae (SNe), cosmic rays, radiation pressure, and magnetic fields are considered in the light of observations:▪Emission and absorption line measurements of cool/warm gas provide our best physical diagnostics of galactic outflows.▪The critical unsolved problem is how to accelerate cool gas to the high velocities observed. Although conclusive evidence for no one mechanism exists, the momentum, energy, and mass-loading budgets observed compare well with theory.▪A model in which star formation provides a force ∼L/c, where L is the bolometric luminosity, and cool gas is pushed out of the galaxy's gravitational potential, compares well with available data. The wind power is ∼0.1 of that provided by SNe.▪The very hot X-ray-emitting phase may be a (or the) prime mover. Momentum and energy exchange between the hot and cooler phases is critical to the gas dynamics.▪Gaps in our observational knowledge include the hot gas kinematics and the size and structure of the outflows probed with UV absorption lines.Simulations are needed to more fully understand mixing, cloud–radiation, cloud–cosmic ray, andcloud–hot wind interactions, the collective effects of star clusters, and both distributed andclustered SNe. Observational works should seek secondary correlations in the wind data thatprovide evidence for specific mechanisms and compare spectroscopy with the column density–velocity results from theory.","PeriodicalId":8138,"journal":{"name":"Annual Review of Astronomy and Astrophysics","volume":"13 1","pages":""},"PeriodicalIF":33.3,"publicationDate":"2024-07-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141755177","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0