Astrophysical Journal Supplement Series最新文献_第6页

A Small-scale Structure Model of a Jet Based on Observations of Microvariability 基于微变率观测的射流小尺度结构模型

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-29 DOI: 10.3847/1538-4365/aceda8

Jingran Xu, Shaoming Hu, Xu Chen, Yunguo Jiang, Sofya Alexeeva

{"title":"A Small-scale Structure Model of a Jet Based on Observations of Microvariability","authors":"Jingran Xu, Shaoming Hu, Xu Chen, Yunguo Jiang, Sofya Alexeeva","doi":"10.3847/1538-4365/aceda8","DOIUrl":"https://doi.org/10.3847/1538-4365/aceda8","url":null,"abstract":"Abstract We developed a multiregion radiation model for the evolution of flux and spectral index with time. In this model, each perturbation component in the jet produces an independent flare. The model can be used to study the decomposition of microvariability, the structural scale of the perturbed components, and the physical parameters of the acceleration processes. Based on the shock acceleration model for a relativistic jet, the influence of the acceleration parameters on multiband flare parameters is calculated. We present the results of multiband optical microvariability of the blazar BL Lacertae observed during 89 nights in the period from 2009 to 2021, and use them as a sample for model fitting. The results show that both the amplitude and duration of flares decomposed from the microvariability light curves conform to a log-normal distribution. The time delays between the optical bands follow a normal distribution and amount to several minutes, which corroborate with both predictions from the theoretical model and the calculation of the discrete correlation function. Using the spectral index evolution and the simultaneous fitting of the multiband variability curves, we obtain the acceleration and radiation parameters to constrain and distinguish the origins of different flares. Based on the flare decomposition, we can effectively reproduce the time-domain evolution trends of the optical variations and energy spectrum, and explain the various redder-when-brighter and bluer-when-brighter behaviors.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"34 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135199608","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

CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates* chianti -原子发射谱线数据库。第十七章。10.1版:修订的电离和重组速率和其他更新*

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-28 DOI: 10.3847/1538-4365/acec79

Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi

{"title":"CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates*","authors":"Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi","doi":"10.3847/1538-4365/acec79","DOIUrl":"https://doi.org/10.3847/1538-4365/acec79","url":null,"abstract":"Abstract The CHIANTI atomic database provides sets of assessed data that are used for simulating spectral observations of astrophysical plasmas. This article describes updates that will be released as version 10.1 of the database. A key component of CHIANTI is the provision of ionization and recombination rates that are used to compute the ionization balance of a plasma over a range of temperatures. Parameters for calculating the ionization rates of all stages of ions from H through Zn were compiled and inserted into the CHIANTI database in 2009. These were based on all measurements that were available at the time and supplemented with distorted wave calculations. Since then, there have been a number of new laboratory measurements for ions that produce spectral lines that are commonly observed. Parameters have been fit to these new measurements to provide improved ability to reproduce the ionization cross sections and rate coefficients, and these are added to the database. CHIANTI 10.1 also includes new recombination rates for the phosphorus isoelectronic sequence, and the updated ionization and recombination rates have been used to calculate a new ionization equilibrium file. In addition, CHIANTI 10.1 has new electron collision and radiative data sets for eight ions in the nitrogen and oxygen isoelectronic sequences and updated energy level and wavelength data for six other ions.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"63 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135343809","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: 9

Improvement of Pan-STARRS Photometric Calibration with LAMOST and Gaia 利用LAMOST和Gaia改进Pan-STARRS光度定标

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-28 DOI: 10.3847/1538-4365/acee73

Kai Xiao, Haibo Yuan, Bowen Huang, Ruoyi Zhang, Lin Yang, Shuai Xu

引用次数: 1

Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M _⊙ at Z = 0.02 使用MESA和k−ω模型的Wolf-Rayet恒星网格:从25到120 M⊙，Z = 0.02

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-27 DOI: 10.3847/1538-4365/aced88

Zhi 志 Li 李, Yan 焱 Li 李

{"title":"Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M <sub>⊙</sub> at Z = 0.02","authors":"Zhi 志 Li 李, Yan 焱 Li 李","doi":"10.3847/1538-4365/aced88","DOIUrl":"https://doi.org/10.3847/1538-4365/aced88","url":null,"abstract":"Abstract To explore overshoot mixing and rotational mixing beyond the convective core during the core He-burning phase in massive stars, we computed a grid of stellar models, both rotating and nonrotating, with the k − ω model at Z = 0.02, covering a mass range of 25–120 M ⊙ . The rotating models start with a rotation rate of v ini / v crit = 0.4 at the zero-age main sequence, and the evolution is computed until the end of the central carbon-burning phase. Models with the k − ω model provide larger convective cores and a broadening of the main-sequence width. The diffusive-overshoot models with f ov = 0.027 are, on average, closer to the k − ω models for massive stars at Z = 0.02, particularly for the stars with masses greater than 40 M ⊙ . The final masses of the Wolf–Rayet (WR) stars range from 9.5–17.5 M ⊙ and 10–23 M ⊙ for the rotating and nonrotating models, respectively. In the rotating models, the C/N ratio decreases slowly below 0.1 outside the convective core, resulting in a flatter element transition region. In addition, the lifetimes of the WNC phase are 1–4 × 10 4 yr, which is about 1 order of magnitude longer than that in the nonrotating models. The masses of the WNC stars are dominated by internal mixing processes and the maximum masses of the He-burning convective cores during the core He-burning phase are in the range of 15–35 M ⊙ . The expected WNC/WR ratios are 0.059 and 0.004 for the rotating and nonrotating models, respectively.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"326 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135538972","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

Aliphatics and Aromatics in the Universe: The Pre-JWST Era 宇宙中的脂肪族和芳香族:前jwst时代

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-27 DOI: 10.3847/1538-4365/acebe6

X. J. Yang, Aigen Li

{"title":"Aliphatics and Aromatics in the Universe: The Pre-JWST Era","authors":"X. J. Yang, Aigen Li","doi":"10.3847/1538-4365/acebe6","DOIUrl":"https://doi.org/10.3847/1538-4365/acebe6","url":null,"abstract":"Abstract The so-called “unidentified infrared emission” (UIE) features at 3.3, 6.2, 7.7, 8.6, and 11.3 μ m ubiquitously seen in a wide variety of astrophysical regions are generally attributed to polycyclic aromatic hydrocarbon (PAH) molecules. Astronomical PAHs often have an aliphatic component (e.g., aliphatic sidegroups like methyl –CH 3 may be attached as functional groups to PAHs) as revealed by the detection in many UIE sources of the aliphatic C–H stretching feature at 3.4 μ m. With its unprecedented sensitivity and spatial resolution, and high spectral resolution, the James Webb Space Telescope (JWST) holds great promise for revolutionizing the studies of aliphatics and aromatics in the Universe. To facilitate analyzing JWST observations, we present a theoretical framework for determining the aliphatic fractions ( η ali ) of PAHs (the fractions of C atoms in aliphatic units) from the emission intensity ratios of the 3.4 μ m aliphatic C–H feature to the 3.3 μ m aromatic C–H feature. To demonstrate the effectiveness of this framework, we compile the 3.3 and 3.4 μ m UIE data obtained in the pre-JWST era for an as-complete-as-possible sample, and then apply the framework to these pre-JWST data. We derive a median aliphatic fraction of 〈 η ali 〉 ≈ 5.4%, and find that the aliphatic fractions are the highest in protoplanetary nebulae illuminated by cool stars lacking ultraviolet radiation. Nevertheless, the “hardness” of stellar photons is not the only factor affecting the PAH aliphaticity, and other factors such as the starlight intensity may also play an important role.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"26 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135536789","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

Deciphering the Morphological Origins of X-shaped Radio Galaxies: Numerical Modeling of Backflow versus Jet Reorientation 解密x形射电星系的形态起源:回流与喷流重新定向的数值模拟

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-22 DOI: 10.3847/1538-4365/acebca

Gourab Giri, Bhargav Vaidya, Christian Fendt

{"title":"Deciphering the Morphological Origins of X-shaped Radio Galaxies: Numerical Modeling of Backflow versus Jet Reorientation","authors":"Gourab Giri, Bhargav Vaidya, Christian Fendt","doi":"10.3847/1538-4365/acebca","DOIUrl":"https://doi.org/10.3847/1538-4365/acebca","url":null,"abstract":"Abstract X-shaped radio galaxies (XRGs) develop when certain extragalactic jets deviate from their propagation path. An asymmetric ambient medium (backflow model) or complex active galactic nucleus activity (jet-reorientation model) enforcing the jet direction to deviate may cause these structures. In this context, the present investigation focuses on the modeling of XRGs by performing 3D relativistic magnetohydrodynamic simulations. We implement different jet-propagation models applying an initially identical jet-ambient medium configuration to understand distinctive features. This study, the first of its kind, demonstrates that all adopted models produce XRGs with notable properties, thereby challenging the notion of a universal model. Jet reorientation naturally explains several contentious properties of XRGs, including wing alignment along the ambient medium’s primary axis, development of collimated lobes, and the formation of noticeably longer wings than active lobes. These XRGs disrupt the cluster medium by generating isotropic shocks and channeling more energy than in the backflow scenario. Our synthetic thermal X-ray maps of the cluster medium reveal four clear elongated cavities associated with the wing-lobe alignment, regardless of projection effects, but they affect their age estimation. We show that the depth and geometric alignment of the evolved cavities may qualify as promising characteristics of XRGs, which may be used to disentangle different formation scenarios.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"71 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136060876","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 Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog 全色哈勃仙女座宝库。第二十一章。传统分辨恒星测光目录

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-22 DOI: 10.3847/1538-4365/acea61

Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman

{"title":"The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog","authors":"Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman","doi":"10.3847/1538-4365/acea61","DOIUrl":"https://doi.org/10.3847/1538-4365/acea61","url":null,"abstract":"Abstract We present the final legacy version of stellar photometry for the Panchromatic Hubble Andromeda Treasury (PHAT) survey. We have reprocessed all of the Hubble Space Telescope Wide Field Camera 3 and Advanced Camera for Surveys near-ultraviolet (F275W, F336W), optical (F475W, F814W), and near-infrared (F110W, F160W) imaging from the PHAT survey using an improved method that optimized the survey depth and chip-gap coverage by including all overlapping exposures in all bands in the photometry. An additional improvement was gained through the use of charge transfer efficiency (CTE)–corrected input images, which provide more complete star finding as well as more reliable photometry for the NUV bands, which had no CTE correction in the previous version of the PHAT photometry. While this method requires significantly more computing resources and time than earlier versions where the photometry was performed on individual pointings, it results in smaller systematic instrumental completeness variations as demonstrated by cleaner maps in stellar density, and it results in optimal constraints on stellar fluxes in all bands from the survey data. Our resulting catalog has 138 million stars, 18% more than the previous catalog, with lower density regions gaining as much as 40% more stars. The new catalog produces nearly seamless population maps that show relatively well-mixed distributions for populations associated with ages older than 1–2 Gyr and highly structured distributions for the younger populations.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"30 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136060875","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

Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths 火星尘埃类似物在紫外-可见-近红外波段的光学常数

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-21 DOI: 10.3847/1538-4365/acf0be

Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker

{"title":"Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths","authors":"Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker","doi":"10.3847/1538-4365/acf0be","DOIUrl":"https://doi.org/10.3847/1538-4365/acf0be","url":null,"abstract":"Abstract We present an advanced light-scattering model to retrieve the optical constants of three Martian dust analogs: Johnson Space Center regolith simulant, Enhanced Mojave Mars Simulant, and Mars Global Simulant. The samples are prepared to have narrow particle-size distributions within the geometric-optics domain. We carry out laboratory measurements to obtain the particle-size distributions, shapes, and diffuse reflectance spectra of the Martian analogs deposited on a surface. Our model framework includes a ray-optics code to compute scattering properties for individual particles, and a radiative-transfer treatment to simulate the surface. The irregular shapes of the dust particles are taken into account in the model. We compare our derived imaginary parts of the refractive indices with those in the literature and find that they are much smaller than the ones that are commonly used for Martian dust. A sensitivity study shows that the retrieved optical constants are sensitive to the particle shape, which needs to be accounted for in applications that use different shapes. Finally, the derived values are validated by using them to reproduce the reflectance spectrum of the Martian surface regolith as observed by the Nadir and Occultation for Mars Discovery instrument on board the ExoMars mission.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"99 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136101498","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: 1

Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3 盖亚DR3中年轻恒星揭示的局部螺旋结构的运动学

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-20 DOI: 10.3847/1538-4365/acf3e3

Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li

引用次数: 0

The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source 35 - 40ghz太阳射电光谱仪的新月和噪声源标定

1区物理与天体物理

Astrophysical Journal Supplement Series Pub Date : 2023-09-20 DOI: 10.3847/1538-4365/acee00

ZiQian 自乾 Shang 尚, Zhao 昭 Wu 武, Yan 岩 Liu 刘, Yu 宇 Bai 白, Guang 光 Lu 路, YuanYuan 园园 Zhang 张, Lei 磊 Zhang 张, YanRui 艳蕊 Su 苏, Yao 耀 Chen 陈, FaBao 发宝 Yan 严

{"title":"The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source","authors":"ZiQian 自乾 Shang 尚, Zhao 昭 Wu 武, Yan 岩 Liu 刘, Yu 宇 Bai 白, Guang 光 Lu 路, YuanYuan 园园 Zhang 张, Lei 磊 Zhang 张, YanRui 艳蕊 Su 苏, Yao 耀 Chen 陈, FaBao 发宝 Yan 严","doi":"10.3847/1538-4365/acee00","DOIUrl":"https://doi.org/10.3847/1538-4365/acee00","url":null,"abstract":"Abstract Calibrating solar radio flux has always been a concern in the solar community. Previously, fluxes were calibrated by matching load or the new Moon for relative calibration, and at times with the assistance of other stations’ data. Moreover, the frequency coverage seldom exceeded 26 GHz. This paper reports the upgraded and calibrated Chashan Broadband Solar millimeter spectrometer (CBS) working from 35 to 40 GHz at the Chashan Solar Observatory (CSO). Initially, the calibration of the solar radiation brightness temperature is accomplished using the new Moon as the definitive source. Subsequently, the 35–40 GHz standard flux is achieved by establishing the correlation between the solar radio flux, brightness temperature, and frequency. Finally, the calibration of the solar radio flux is implemented by utilizing a constant temperature-controlled noise source as a reference. The calibration in 2023 February and March reveals that the solar brightness temperature is 11,636 K at 37.25 GHz with a standard deviation (STD) of 652 K. The solar radio flux’s intensity is ∼3000–4000 solar flux units (SFU) in the range of 35–40 GHz with a consistency bias of ±5.3%. The system sensitivity is about ∼5–8 SFU by a rough evaluation, a noise factor of about 200 K, and the coefficient of variation of the system transmission slope of 6.5% @ 12 hr at 37.25 GHz. It is expected that the upgraded CBS will capture more activity during the upcoming solar cycle.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"158 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136308082","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