Astrophysical Journal最新文献_第3页

On the Escape of Low-frequency Waves from Magnetospheres of Neutron Stars 中子星磁层低频波的逸出

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/acfa78

Ephim Golbraikh, Yuri Lyubarsky

引用次数: 0

TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B 附近丝状分子云的TRAO巡天，恒星的普遍托儿所(TRAO- funs)。3猎户座B NGC 2068和NGC 2071区域的细丝和致密核

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/acf8c2

Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim

{"title":"TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B","authors":"Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim","doi":"10.3847/1538-4357/acf8c2","DOIUrl":"https://doi.org/10.3847/1538-4357/acf8c2","url":null,"abstract":"Abstract We present the results of molecular line observations performed toward the NGC 2068 and NGC 2071 regions of the Orion B cloud as the TRAO-FUNS project to study the roles of the filamentary structure in the formation of dense cores and stars in the clouds. Gaussian decomposition for the C 18 O spectra with multiple velocity components and the application of a friends-of-friends algorithm for the decomposed components allowed us to identify a few tens of velocity-coherent filaments. We also identified 48 dense cores from the observations of N 2 H + using a core finding tool, FellWalker. We performed a virial analysis for these filaments and dense cores, finding that the filaments with N 2 H + dense core are thermally supercritical, and the filaments with a larger ratio between the line mass and the thermal critical line mass tend to have more dense cores. We investigated the contribution of the nonthermal motions in dense cores and filaments, showing the dense cores are mostly in transonic/subsonic motions while their natal filaments are mostly in supersonic motions. This may indicate that gas turbulent motions in the filaments have been dissipated at the core scale to form the dense cores there. The filaments with (dynamically evolved) dense cores in infalling motions or with NH 2 D bright (or chemically evolved) dense cores are all found to be gravitationally critical. Therefore, the criticality of the filament is thought to provide a key condition for its fragmentation, the formation of dense cores, and their kinematical and chemical evolution.","PeriodicalId":50735,"journal":{"name":"Astrophysical Journal","volume":"7 6","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135410326","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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

Detection of a ∼0.1c Radio Knot in M81* Associated with a Moderate X-Ray Flare 探测到M81*中一颗与中等x射线耀斑相关的0.1c射电结

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/ad0371

Xuezheng Wang, Wu Jiang, Zhiqiang Shen, Zhen Yan, Ya-Ping Li, Ivan Martí-Vidal, Roman Gold

引用次数: 1

Heavy-ion Acceleration in ³He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter 富3he太阳高能粒子事件中的重离子加速:来自太阳轨道器的新见解

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/acf31b

G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco

{"title":"Heavy-ion Acceleration in <sup>3</sup>He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter","authors":"G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco","doi":"10.3847/1538-4357/acf31b","DOIUrl":"https://doi.org/10.3847/1538-4357/acf31b","url":null,"abstract":"Abstract We present Solar Orbiter energetic particle observations of two 3 He-rich events with features more clearly observed than in prior studies. The event of 2022 November 9 observed from 0.59 au contained hundreds of ultraheavy (UH; mass >78 amu) ions whereas previous observations at 1 au have shown only an occasional count or two. The event of 2023 April 8 observed from 0.29 au fortuitously had very low ambient activity, making it possible to observe spectra from the 3 He acceleration mechanism without contamination, revealing extremely low H and 4 He intensities arriving simultaneously with other ions observed in typical 3 He-rich events. Taken together with previous studies, we believe these data show that 3 He-rich events have a single acceleration mechanism that is responsible for the unique abundance features of 3 He, heavy ions, and UH ions. Considering the acceleration model of Roth & Temerin that heats the ions over a broad range of gyrofrequencies away from those damped by H and 4 He, we calculate reasonable fits to the observed abundances O–Fe. A key result is that high values of, e.g., Fe/O typical of such events is not due to preferential Fe heating, but on the contrary is due mainly to the depletion of O, which at elevated temperatures has a charge-to-mass ratio in the region of the waves damped by 4 He. The model also naturally incorporates features of high-ionization states and neutron-rich isotope enhancements that have been long-standing puzzles in observations of this type of flare.","PeriodicalId":50735,"journal":{"name":"Astrophysical Journal","volume":"1 2","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135456361","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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

Scattering of Superthermal Ions at Shocks: Dependence on Energy 过热离子在冲击中的散射:对能量的依赖

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/ad04dd

Michael Gedalin, Natalia Ganushkina, Nikolai V. Pogorelov, Vadim Roytershteyn

引用次数: 0

Evolutionary Relationship between Sunspot Groups and Soft X-Ray Flares over Solar Cycles 21–25 太阳活动周期21-25的太阳黑子群与软x射线耀斑的演化关系

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/ad0469

Jiaqi 家琪 Lin 林, Feng 锋 Wang 王, Linhua 林华 Deng 邓, Hui 辉 Deng 邓, Ying 盈 Mei 梅, Xiaojuan 小娟 Zhang 张

{"title":"Evolutionary Relationship between Sunspot Groups and Soft X-Ray Flares over Solar Cycles 21–25","authors":"Jiaqi 家琪 Lin 林, Feng 锋 Wang 王, Linhua 林华 Deng 邓, Hui 辉 Deng 邓, Ying 盈 Mei 梅, Xiaojuan 小娟 Zhang 张","doi":"10.3847/1538-4357/ad0469","DOIUrl":"https://doi.org/10.3847/1538-4357/ad0469","url":null,"abstract":"Abstract Studying the interaction between solar flares and sunspot groups (SGs) is crucial for understanding and predicting solar activity. We examined the distribution, correlation, and flaring rates in the northern and southern hemispheres to reveal the relationship between different classes of soft X-ray (SXR) flares and different magnetic classifications of SGs. We discovered a significant north–south asymmetry in SXR flares and SG distribution over Solar Cycles (SC) 21–25. In the rising phase of SC24, the northern hemisphere’s activity is significantly excessive. In the declining phase of SC24, the southern hemisphere’s activity becomes significantly excessive. The total numbers of various SXR flares and SGs vary between the northern and southern hemispheres over the solar cycle. B-class flares are negatively correlated with all SGs at maximum but positively correlated at minimum. C-class flares correlate best with α and β SGs. M-class flares correlate best with β γ δ and β SGs. X-class flares correlate highest with β γ δ SGs. The flaring rate of each flare class is lowest for α SGs and highest for β γ δ SGs. The flaring rates are higher in the southern hemisphere than in the northern hemisphere. Our results demonstrate that solar flares originate from different sources of solar active regions; the high-energy flares tend to be caused by more complex magnetic fields.","PeriodicalId":50735,"journal":{"name":"Astrophysical Journal","volume":"11 4","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135510252","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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

Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins 双黑洞质量比与黑洞自旋相关的证据

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/acf763

Christian Adamcewicz, Paul D. Lasky, Eric Thrane

{"title":"Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins","authors":"Christian Adamcewicz, Paul D. Lasky, Eric Thrane","doi":"10.3847/1538-4357/acf763","DOIUrl":"https://doi.org/10.3847/1538-4357/acf763","url":null,"abstract":"Abstract The astrophysical origins of the binary black hole systems seen with gravitational waves are still not well understood. However, features in the distribution of black hole masses, spins, redshifts, and eccentricities provide clues into how these systems form. Much has been learned by investigating these distributions one parameter at a time. However, we can extract additional information by studying the covariance between pairs of parameters. Previous work has shown preliminary support for an anticorrelation between mass ratio q ≡ m 2 / m 1 and effective inspiral spin χ eff in the binary black hole population. In this study, we test for the existence of this anticorrelation using updated data from the third gravitational-wave transient catalog and improve our copula-based framework to employ a more robust model for black hole spins. We find evidence for an anticorrelation in ( q , χ eff ) with 99.7% credibility. This may imply high common-envelope efficiencies, stages of super-Eddington accretion, or a tendency for binary black hole systems to undergo mass-ratio reversal during isolated evolution. Covariance in ( q , χ eff ) may also be used to investigate the physics of tidal spinup as well as the properties of binary black hole–forming active galactic nuclei.","PeriodicalId":50735,"journal":{"name":"Astrophysical Journal","volume":"6 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135510263","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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

Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270 G083.097+03.270中细丝合并和轮毂形成的观测证据

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/ad0048

Alik Panja, Lokesh K. Dewangan, Tapas Baug, Wen Ping Chen, Yan Sun, Tirthendu Sinha, Soumen Mondal

{"title":"Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270","authors":"Alik Panja, Lokesh K. Dewangan, Tapas Baug, Wen Ping Chen, Yan Sun, Tirthendu Sinha, Soumen Mondal","doi":"10.3847/1538-4357/ad0048","DOIUrl":"https://doi.org/10.3847/1538-4357/ad0048","url":null,"abstract":"Abstract We uncover a hub–filament system correlated with massive young stellar associations in G083.097+03.270. Diagnosed with simultaneous 12 CO, 13 CO, and C 18 O line observations, the region is found to host two distinct and elongated filaments having separate velocity components, interacting spatially and kinematically, that appear to have seeded the formation of a dense hub at the intersection. A large velocity spread at the hub, in addition to a clear bridging feature connecting the filaments in velocity, indicate the merging of filaments. Along the filament axis, the velocity gradient reveals a global gas motion with an increasing velocity dispersion inward to the hub signifying turbulence. Altogether, the clustering of Class I sources, a high excitation temperature, a high column density, and the presence of a massive outflow at the central hub suggest enhanced star formation. We propose that the merging of large-scale filaments and velocity gradients along filaments are the driving factors in the mass accumulation process at the hub that have sequentially led to the massive star formation. With two giant filaments merging to coincide with a hub therein with ongoing star formation, this site serves as a benchmark for the “filaments to clusters” star-forming paradigm.","PeriodicalId":50735,"journal":{"name":"Astrophysical Journal","volume":"39 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135564554","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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

Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1 光谱确认的Lyα发射体在z ~ 3.1的Lyman连续发射

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/acf9fa

Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng

{"title":"Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1","authors":"Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng","doi":"10.3847/1538-4357/acf9fa","DOIUrl":"https://doi.org/10.3847/1538-4357/acf9fa","url":null,"abstract":"Abstract We present a study of Lyman continuum (LyC) emission in a sample of ∼150 Ly α emitters (LAEs) at z ≈ 3.1 in the Subaru-XMM Deep Survey field. These LAEs were previously selected using the narrowband technique and spectroscopically confirmed with Ly α equivalent widths (EWs) ≥ 45 Å. We obtain deep UV images using a custom intermediate-band filter U J that covers a wavelength range of 3330 ∼ 3650 Å, corresponding to 810 ∼ 890 Å in the rest frame. We detect five individual LyC galaxy candidates in the U J band, and their escape fractions ( f esc ) of LyC photons are roughly between 40% and 80%. This supports a previous finding that a small fraction of galaxies may have very high f esc . We find that the f esc values of the five LyC galaxies are not apparently correlated with other galaxy properties such as Ly α luminosity and EW, UV luminosity and slope, and star formation rate (SFR). This is partly due to the fact that these galaxies only represent a small fraction (∼3%) of our LAE sample. For the remaining LAEs that are not detected in U J , we stack their U J -band images and constrain their average f esc . The upper limit of the average f esc value is about 16%, consistent with the results in the literature. Compared with the non-LyC LAEs, the LyC LAEs tend to have higher Ly α luminosities, Ly α EWs, and SFRs, but their UV continuum slopes are similar to those of other galaxies.","PeriodicalId":50735,"journal":{"name":"Astrophysical Journal","volume":"59 3","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135564666","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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

Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies 火-2银河系质量星系中暗物质晕的方向

2区物理与天体物理

Astrophysical Journal Pub Date : 2023-11-01 DOI: 10.3847/1538-4357/acea79

Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham

{"title":"Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies","authors":"Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham","doi":"10.3847/1538-4357/acea79","DOIUrl":"https://doi.org/10.3847/1538-4357/acea79","url":null,"abstract":"Abstract The shape and orientation of dark matter (DM) halos are sensitive to the microphysics of the DM particles, yet in many mass models, the symmetry axes of the Milky Way’s DM halo are often assumed to be aligned with the symmetry axes of the stellar disk. This is well motivated for the inner DM halo, but not for the outer halo. We use zoomed-in cosmological baryonic simulations from the Latte suite of FIRE-2 Milky Way–mass galaxies to explore the evolution of the DM halo’s orientation with radius and time, with or without a major merger with a Large Magellanic Cloud analog, and when varying the DM model. In three of the four cold DM halos we examine, the orientation of the halo minor axis diverges from the stellar disk vector by more than 20° beyond about 30 galactocentric kpc, reaching a maximum of 30°–90°, depending on the individual halo’s formation history. In identical simulations using a model of self-interacting DM with σ = 1 cm 2 g −1 , the halo remains aligned with the stellar disk out to ∼200–400 kpc. Interactions with massive satellites ( M ≳ 4 × 10 10 M ⊙ at pericenter; M ≳ 3.3 × 10 10 M ⊙ at infall) affect the orientation of the halo significantly, aligning the halo’s major axis with the satellite galaxy from the disk to the virial radius. The relative orientation of the halo and disk beyond 30 kpc is a potential diagnostic of self-interacting DM, if the effects of massive satellites can be accounted for.","PeriodicalId":50735,"journal":{"name":"Astrophysical Journal","volume":"37 5","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135614119","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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