The Astrophysical Journal最新文献_第2页

The Tip of Red Giant Branch Distances to Nearby Dwarf Galaxies WLM and Sextans A with JWST 用JWST观测红巨星分支到附近矮星系WLM和六分星A的距离

The Astrophysical Journal Pub Date : 2025-06-04 DOI: 10.3847/1538-4357/add52e

Ziming Yan, Shu Wang, Xiaodian Chen and Licai Deng

{"title":"The Tip of Red Giant Branch Distances to Nearby Dwarf Galaxies WLM and Sextans A with JWST","authors":"Ziming Yan, Shu Wang, Xiaodian Chen and Licai Deng","doi":"10.3847/1538-4357/add52e","DOIUrl":"https://doi.org/10.3847/1538-4357/add52e","url":null,"abstract":"Distance measurements to extragalactic systems that are both accurate and precise are cornerstones of modern astrophysics, underpinning the calibration of standard candles and the determination of the Hubble constant. Dwarf galaxies, such as Wolf–Lundmark–Melotte (WLM) and Sextans A, provide valuable laboratories for testing distance scales across different stellar populations. In this work, we utilize the high sensitivity and spatial resolution of the James Webb Space Telescope to measure the distances to WLM and Sextans A using the tip of the red giant branch (TRGB) method. Adopting the TRGB absolute magnitude calibrated by NGC 4258, we determine distance moduli of μ0,WLM = 24.977 ± 0.018(stat) ± 0.056(sys) mag for WLM and μ0,SexA = 25.740 ± 0.011(stat) ± 0.057(sys) mag for Sextans A. Our results are consistent within a 3% distance uncertainty with previous measurements based on TRGB, Cepheids, and J-Region Asymptotic Giant Branch methods. With improved distance measurements in the future, these two galaxies have the potential to serve as additional anchor points for TRGB calibration and reduce the TRGB-based distance uncertainty to below 2%.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"331 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144218756","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Polarization Evolution of Gamma-Ray Burst Prompt Emission with Bulk Acceleration 体加速下伽玛暴瞬发的极化演化

The Astrophysical Journal Pub Date : 2025-06-03 DOI: 10.3847/1538-4357/add0ac

Qian Zhong, Hong-Bang Liu, Kangfa Cheng, Zu-Ke Feng, Jiang-Chuan Tuo, Qian-Nan Mai, Jirong Mao and En-Wei Liang

{"title":"Polarization Evolution of Gamma-Ray Burst Prompt Emission with Bulk Acceleration","authors":"Qian Zhong, Hong-Bang Liu, Kangfa Cheng, Zu-Ke Feng, Jiang-Chuan Tuo, Qian-Nan Mai, Jirong Mao and En-Wei Liang","doi":"10.3847/1538-4357/add0ac","DOIUrl":"https://doi.org/10.3847/1538-4357/add0ac","url":null,"abstract":"During the prompt phase, Poynting-flux-dominated jets undergo acceleration accompanied by magnetic dissipation. By using an outward-propagating thin-shell model, where bulk Lorentz factors Γ increase with radius and the magnetic field strength decay is related to the acceleration and the energy conversion rate, this process can be investigated through time-resolved polarization analysis. Faster acceleration produces a greater flux, steeper light-curve growth followed by a sharper decline, and polarization degree decreases sharply. With a fixed acceleration index, lower energy conversion rates are associated with lower flux, shallower rises and declines in light curves, lower polarization degree, smoother decline for on-beam (q = θv/θj < 1) emission, and sharper decline for off-beam (q > 1) emission in polarization curves. Both jet acceleration and magnetic dissipation enhance the likelihood of polarization angle flips in observations with small viewing angles, while also leading to higher polarization degrees after the flip in observations with larger viewing angles. The joint analysis of light curves and polarization provides valuable insights into gamma-ray burst motion and energy conversion processes. Rapid decline in the light curve indicates fast acceleration and high energy conversion rates, while gradual light-curve decline coupled with polarization angle flips (for small viewing angles) or the higher polarization degree after flipping (for large viewing angles) suggests acceleration accompanied by magnetic dissipation. Otherwise, the jet is coasting or slowly accelerating at this time.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"81 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144218759","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Dynamically Driven Evolution of Molecular Gas in the Barred Spiral Galaxy M83 Traced by CO J = 2–1/1–0 Line Ratio Variations 用CO J = 2-1/1-0谱线比值追踪棒旋星系M83中分子气体的动态驱动演化

The Astrophysical Journal Pub Date : 2025-06-03 DOI: 10.3847/1538-4357/add1dc

Jin Koda, Fumi Egusa, Akihiko Hirota, Amanda M Lee, Tsuyoshi Sawada and Fumiya Maeda

{"title":"Dynamically Driven Evolution of Molecular Gas in the Barred Spiral Galaxy M83 Traced by CO J = 2–1/1–0 Line Ratio Variations","authors":"Jin Koda, Fumi Egusa, Akihiko Hirota, Amanda M Lee, Tsuyoshi Sawada and Fumiya Maeda","doi":"10.3847/1538-4357/add1dc","DOIUrl":"https://doi.org/10.3847/1538-4357/add1dc","url":null,"abstract":"We show the variations of the CO J = 2–1/1–0 line ratio (R21/10) across the barred spiral galaxy M83, using the 46 pc resolution data from the Atacama Large Millimeter/submillimeter Array. The R21/10 map clearly evidences the systematic large-scale variations as a function of galactic structures. Azimuthally, it starts from low R21/10 ≲ 0.7 in the interarm regions and becomes high ≳0.7 in the bar and spiral arms, suggesting that the density and/or kinetic temperature of molecular gas increase by about a factor of 2–3. This evolution is seen even in the parts of spiral arms without star formation, and R21/10 is often elevated even higher to ∼0.8–1.0 when H ii regions exist in the vicinity. Radially, R21/10 starts very high ≳1.0 at the galactic center, remains low ≲0.7 in the bar region, increases to ≳0.7 around the bar end, and again decreases to ≲0.7 in the rest of disk where the spiral arms dominate. The evolutionary sequence is synchronized with galactic rotation, and therefore, it is determined largely by the galactic structures and dynamics and is governed by the galactic rotation timescales. The R21/10 map also shows that the influence of stellar feedback is localized and limited. Massive, large, and non-star-forming molecular structures have low R21/10, which also suggests that the bulk molecular gas in the disk is not regulated by stellar feedback, but more likely by galactic structures and dynamics. These results are consistent with suggestions by the earlier studies of the Milky Way and other barred spiral galaxies, and thus, are likely general among barred spiral galaxies in the local Universe.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"81 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211134","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Clumpy Starburst in a Local Dwarf Galaxy, NGC 1522 本地矮星系ngc1522中的块状星暴

The Astrophysical Journal Pub Date : 2025-06-03 DOI: 10.3847/1538-4357/add0b7

Liuze Long, Yulong Gao, Qiusheng Gu, Yong Shi, Xin Li, Can Xu, Yifei Jin, Zhiyuan Zheng, Jing Dou, Fuyan Bian and Xiaoling Yu

{"title":"Clumpy Starburst in a Local Dwarf Galaxy, NGC 1522","authors":"Liuze Long, Yulong Gao, Qiusheng Gu, Yong Shi, Xin Li, Can Xu, Yifei Jin, Zhiyuan Zheng, Jing Dou, Fuyan Bian and Xiaoling Yu","doi":"10.3847/1538-4357/add0b7","DOIUrl":"https://doi.org/10.3847/1538-4357/add0b7","url":null,"abstract":"To investigate the star-forming process in nearby dwarf galaxies, we present integral field unit observations of the star-forming dwarf galaxy NGC 1522 with the Very Large Telescope/Multi Unit Spectroscopic Explorer as a part of the Dwarf Galaxy Integral Survey. Our observations reveal the presence of a star-forming clumpy ring in its central region. We identify nine distinct star-forming clumps based on an extinction-corrected Hα emission line map, with a total star formation rate of about 0.1 M⊙ yr−1. The nine clumps are considered to be starbursts, which represent an extreme case in the local Universe, without invoking major merging. We investigate the properties of ionized gas using the strong emission lines and “BPT” diagrams, in conjunction with velocity mapping. Our analysis unveils intriguing patterns, including a positive metallicity gradient and low N/O abundance ratio. This peculiar distribution of metallicity may signify external gas accretion. Our results suggest that the ongoing star formation in NGC 1522 might be triggered and sustained by the inflow of external metal-poor gas.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"36 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211132","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Binding Energies of Small Interstellar Molecules on Neutral and Charged Amorphous Solid Water Surfaces 星际小分子在中性和带电非晶固体水面上的结合能

The Astrophysical Journal Pub Date : 2025-06-03 DOI: 10.3847/1538-4357/add145

Tobe Vorsselmans and Erik C. Neyts

{"title":"Binding Energies of Small Interstellar Molecules on Neutral and Charged Amorphous Solid Water Surfaces","authors":"Tobe Vorsselmans and Erik C. Neyts","doi":"10.3847/1538-4357/add145","DOIUrl":"https://doi.org/10.3847/1538-4357/add145","url":null,"abstract":"The interstellar medium (ISM) is all but empty. To date, more than 300 molecules have already been discovered. Because of the extremely low temperature, the gas-phase chemistry is dominated by barrierless exothermic reactions of radicals and ions. However, several abundant molecules and organic molecules cannot be produced efficiently by gas-phase reactions. To explain the existence of such molecules in the ISM, gas-surface interactions between small molecules and dust particles covered with amorphous solid water (ASW) mantles must be considered. In general, surface processes such as adsorption, diffusion, desorption, and chemical reactions can be linked to the binding energy of molecules to the surface. Hence, a lot of studies have been performed to identify the binding energies of interstellar molecules on ASW surfaces. Cosmic radiation and free electrons may induce a negative charge on the dust particles, and the binding energies may be affected by this charge. In this study, we calculate the binding energies of CO, CH4, and NH3 on neutral and charged ASW surfaces using density functional theory calculations. Our results indicate that CO can interact with the surface charge, increasing its binding energy. In contrast, the binding energy of CH4 remains unchanged in the presence of surface charge, and that of NH3 typically decreases.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211133","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A Sample of Extreme Eclipsing Binaries with Accretion Disks from LAMOST and ZTF LAMOST和ZTF带吸积盘的极端食双星样本

The Astrophysical Journal Pub Date : 2025-06-03 DOI: 10.3847/1538-4357/adcf91

Jiangxinxin Zhuang, Zhi-Xiang Zhang, Wei-Min Gu and Senyu Qi

{"title":"A Sample of Extreme Eclipsing Binaries with Accretion Disks from LAMOST and ZTF","authors":"Jiangxinxin Zhuang, Zhi-Xiang Zhang, Wei-Min Gu and Senyu Qi","doi":"10.3847/1538-4357/adcf91","DOIUrl":"https://doi.org/10.3847/1538-4357/adcf91","url":null,"abstract":"Extreme eclipsing binaries may harbor peculiar physical properties. In this work, we aim to identify a sample of such systems by selecting binaries with pronounced eclipsing light curves, characterized by large variability (Δmag > 0.3 in the g band of the Zwicky Transient Facility, ZTF) and significant differences between primary and secondary eclipses (eclipse depth ratio >20 in the ZTF g band). We identified 23 candidates by combining the photometric data and the LAMOST spectroscopic survey. Spectroscopic analysis revealed that all of these systems are dominated by A-type stars in the optical band. Further investigation confirmed that all 23 candidates are Algol-type binaries, with 22 of them being newly discovered. Their orbital periods range from 2.57 to 19.21 days. These systems consist of low-luminosity, highly stripped subgiant donors and accreting A-type stars. The donor stars, with radii of 2.5–8.9 R⊙ and effective temperatures around 4000 K, have typical masses of M2 ∼ 0.3 M⊙, indicating substantial mass loss through Roche-lobe overflow. The presence of ellipsoidal variability and Hα emission provides strong evidence for ongoing mass transfer. By fitting the spectral energy distributions, spectra, and light curves, we found that most of the accretors have luminosities lower than expected from the mass–luminosity relation, aligning with the predicted faint phase for mass-gaining stars. Three objects of our sample exhibit pulsations with periods from 18 minutes to 8 hr, providing opportunities for asteroseismic studies. The low mass transfer rates and stability make the sample excellent systems for studying mass accretion, advancing our understanding of the evolution of Algol-type binaries.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"331 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211512","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Red Supergiant Problem Viewed from the Nebular Phase Spectroscopy of Type II Supernovae 从II型超新星星云相光谱看红超巨星问题

The Astrophysical Journal Pub Date : 2025-06-03 DOI: 10.3847/1538-4357/adceae

Qiliang Fang, 其亮方, Takashi J. Moriya and Keiichi Maeda

{"title":"Red Supergiant Problem Viewed from the Nebular Phase Spectroscopy of Type II Supernovae","authors":"Qiliang Fang, 其亮方, Takashi J. Moriya and Keiichi Maeda","doi":"10.3847/1538-4357/adceae","DOIUrl":"https://doi.org/10.3847/1538-4357/adceae","url":null,"abstract":"The red supergiant (RSG) problem refers to the observed dearth of luminous RSGs identified as progenitors of Type II supernovae (SNe II) in pre-SN imaging. Understanding this phenomenon is essential for studying pre-SN mass loss and the explodability of core-collapse SNe. In this work, we reassess the RSG problem using late-phase spectroscopy of a sample of 50 SNe II. The [O I] λλ6300,6363 emission in the spectra is employed to infer the zero-age main-sequence (ZAMS) mass distribution of the progenitors, which is then transformed into a luminosity distribution via an observation-calibrated mass–luminosity relation. The resulting luminosity distribution reveals an upper cutoff at dex, and the RSG problem is statistically significant at the 2σ–3σ level. Assuming single RSG progenitors that follow the mass–luminosity relation of KEPLER models, this luminosity cutoff corresponds to an upper ZAMS mass limit of . Comparisons with independent measurements, including pre-SN imaging and plateau-phase light curve modeling, consistently yield an upper ZAMS mass limit below ∼25 M⊙, with a significance level of 1σ–3σ. While each individual method provides only marginal significance, the consistency across multiple methodologies suggests that the lack of luminous RSG progenitors may reflect a genuine physical problem. Finally, we discuss several scenarios to account for this issue should it be confirmed as a true manifestation of stellar physics.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211129","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Event Rate Density and Luminosity Function of Newborn-magnetar-driven X-Ray Transients from Neutron Star Binary Mergers 中子星双并合中新生磁驱动x射线瞬变的事件率密度和光度函数

The Astrophysical Journal Pub Date : 2025-06-03 DOI: 10.3847/1538-4357/add2f7

Le Zou, Ji-Gui Cheng, Rui-Chong Hu, Wen-Jin Xie and En-Wei Liang

{"title":"Event Rate Density and Luminosity Function of Newborn-magnetar-driven X-Ray Transients from Neutron Star Binary Mergers","authors":"Le Zou, Ji-Gui Cheng, Rui-Chong Hu, Wen-Jin Xie and En-Wei Liang","doi":"10.3847/1538-4357/add2f7","DOIUrl":"https://doi.org/10.3847/1538-4357/add2f7","url":null,"abstract":"X-ray transients (XTs) driven by newborn magnetars from mergers of neutron star binaries (NSBs) have occasionally been detected in the narrow-field Chandra Deep Field-South (CDF-S) survey and the Swift/X-Ray Telescope observations of short gamma-ray bursts. Quantifying their event rate density (ERD) and luminosity function (LF) is critical for understanding NSB coalescence and magnetar formation. Utilizing population synthesis calculations incorporating various equations of state (EoSs), we derive a local ERD of ∼300 Gpc−3 yr−1 and a redshift-dependent ERD profile peaking at z = 1.81 followed by a rapid decline beyond z ∼ 4. Constructing an XT sample based on CDF-S and Swift observations, we characterize the LF by a single power-law function at L ≤ 4.75 × 1046 erg s−1 with a slope of −1.03, followed by a broken power-law function in which the break luminosity is Lb = 4.38 × 1047 erg s−1 and the slopes are −0.28 and −1.66. Based on the ERD and the LF, we estimate that the Einstein Probe (EP) detection rate is ∼31 yr−1, adopting a conservative threshold flux of 10−9 erg s−1, a luminosity range of L ∈ [2 × 1044, 2 × 1049] erg s−1, and a correction for the jet opening angle of ∼16∘. This detection rate is consistent with the EP observations during its first year of operation. It is important to note that our estimation is subject to uncertainties arising from the LF derivation. Future EP observations of these XT events will be crucial in reducing these uncertainties.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"52 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211511","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Mapping the Star Formation and H i Gas Properties of Galaxies along Large-scale Structures around the Virgo Cluster 沿着室女座星团周围的大尺度结构绘制星系的恒星形成和H气体特性

The Astrophysical Journal Pub Date : 2025-06-03 DOI: 10.3847/1538-4357/adceaf

Hyein Yoon, 혜인 윤, O. Ivy Wong, Aeree Chung and Shan Huang

{"title":"Mapping the Star Formation and H i Gas Properties of Galaxies along Large-scale Structures around the Virgo Cluster","authors":"Hyein Yoon, 혜인 윤, O. Ivy Wong, Aeree Chung and Shan Huang","doi":"10.3847/1538-4357/adceaf","DOIUrl":"https://doi.org/10.3847/1538-4357/adceaf","url":null,"abstract":"We investigate the star formation and neutral atomic hydrogen (H i) gas properties of galaxies along three large-scale filaments and two galaxy groups in the wide field around the Virgo cluster. Our goal is to understand how galaxies are processed in low-density environments before falling into high-density regions. Combining the spatial distribution of galaxies with multiwavelength colors such as W3 − W1, NUV − r, and g − r, we find a predominance of blue galaxies across the structures, indicating normal-to-enhanced star formation, similar to that of isolated galaxies. However, one filament and one group show a significant number of red galaxies (32% and 20%, respectively), suggesting that star formation has been suppressed in low-density environments before reaching high-density regions. Intriguingly, these red galaxies span a wide range of stellar masses, and the presence of red dwarfs support that not only mass but also environment plays an important role in the quenching of star formation in cluster outskirts. One particular filament, potentially connected to Virgo, already has a group of red populations outside Virgo’s R200, making these galaxies good candidates for being “preprocessed” before entering the Virgo cluster. In addition, several galaxies in the filaments and groups possess relatively low H i gas contents, similar to cluster galaxies. However, the overall fraction of H i-deficient galaxies is not as significantly high as the fraction of red galaxies in these structures. This suggests that H i gas properties are less influenced by the environment than star formation properties in low-density regions, possibly due to gas replenishment through accretion.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"168 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144218829","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Resonant Absorption and Fluctuations via Hybrid Simulations on Coronal Loops. I. Plasma Multifluid Description 基于日冕环混合模拟的共振吸收和波动。1 .等离子体多流体描述

The Astrophysical Journal Pub Date : 2025-06-03 DOI: 10.3847/1538-4357/adceac

Hugo A. Carril, Jaume Terradas, Roberto E. Navarro, Adolfo F. Viñas and Marcel Goossens

{"title":"Resonant Absorption and Fluctuations via Hybrid Simulations on Coronal Loops. I. Plasma Multifluid Description","authors":"Hugo A. Carril, Jaume Terradas, Roberto E. Navarro, Adolfo F. Viñas and Marcel Goossens","doi":"10.3847/1538-4357/adceac","DOIUrl":"https://doi.org/10.3847/1538-4357/adceac","url":null,"abstract":"We investigate the resonant absorption process of a combination of left- and right-hand polarized waves (with a fixed perturbation amplitude) in a plasma slab with linearly inhomogeneous particle densities. Different thicknesses of the layers and angles of the background magnetic field to the plane of the slab, representing the degree of magnetization of the slab, are studied via 2D−3V PIC-hybrid simulations with a fixed perturbation amplitude. We identify the process of resonant absorption of the large-scale mode in the inhomogeneous layers and compare the damping rate of the transverse oscillations with single-fluid, linear MHD estimations. By following the spectral densities of the magnetic field fluctuations, it is found that kinetic scales are achieved in most of the simulated cases, particularly in the case of thinner inhomogeneous layers and in cases where the plasma slab is not weakly magnetized. In particular, the scales of the fluctuations can reach the proton inertial length. The small-scale fluctuations are identified as quasi-perpendicular oscillations localized within the inhomogeneous layers, and their properties in the spectral representation agree with theoretical properties of kinetic Alfvén waves predicted by kinetic and Hall-MHD theories.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"25 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211128","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0