The Astrophysical Journal最新文献_第6页

The SOFIA Massive (SOMA) Star Formation Survey. V. Clustered Protostars 索非亚大质量（SOMA）恒星形成调查。五、聚集的原恒星

The Astrophysical Journal Pub Date : 2025-06-02 DOI: 10.3847/1538-4357/adcd79

Zoie Telkamp, Rubén Fedriani, Jonathan C. Tan, Chi-Yan Law, Yichen Zhang, Adele Plunkett, Samuel Crowe, Yao-Lun Yang, James M. De Buizer, Maria T. Beltran, Mélisse Bonfand, Ryan Boyden, Giuliana Cosentino, Prasanta Gorai, Mengyao Liu, Viviana Rosero, Kotomi Taniguchi, Kei E. I. Tanaka and Tatiana M. Rodríguez

{"title":"The SOFIA Massive (SOMA) Star Formation Survey. V. Clustered Protostars","authors":"Zoie Telkamp, Rubén Fedriani, Jonathan C. Tan, Chi-Yan Law, Yichen Zhang, Adele Plunkett, Samuel Crowe, Yao-Lun Yang, James M. De Buizer, Maria T. Beltran, Mélisse Bonfand, Ryan Boyden, Giuliana Cosentino, Prasanta Gorai, Mengyao Liu, Viviana Rosero, Kotomi Taniguchi, Kei E. I. Tanaka and Tatiana M. Rodríguez","doi":"10.3847/1538-4357/adcd79","DOIUrl":"https://doi.org/10.3847/1538-4357/adcd79","url":null,"abstract":"We present ∼8–40 μm SOFIA-FORCAST images of seven regions of “clustered” star formation as part of the SOFIA Massive Star Formation Survey. We identify a total of 34 protostar candidates and build their spectral energy distributions (SEDs). We fit these SEDs with a grid of radiative transfer models based on the turbulent core accretion (TCA) theory to derive key protostellar properties, including initial core mass, Mc, clump environment mass surface density, Σcl, and current protostellar mass, m*. We also carry out empirical graybody (GB) estimation of Σcl, which allows a case of restricted SED fitting within the TCA model grid. We also release version 2.0 of the open-source Python package sedcreator, which is designed to automate the aperture photometry and SED building and fitting process for sources in clustered environments, where flux contamination from close neighbors typically complicates the process. Using these updated methods, SED fitting yields values of Mc ∼ 30–200 M⊙, Σcl,SED ∼ 0.1–3 g cm−2, and m* ∼ 4–50 M⊙. The GB fitting yields smaller values of Σcl,GB ≲ 1 g cm−2. From these results, we do not find evidence for a critical Σcl needed to form massive (≳8 M⊙) stars. However, we do find tentative evidence for a dearth of the most massive (m* ≳ 30 M⊙) protostars in the clustered regions, suggesting a potential impact of environment on the stellar initial mass function.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"38 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144202067","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

The Role of Pressure in the Structure and Stability of GMCs in the Andromeda Galaxy 压力在仙女座星系gmc结构和稳定性中的作用

The Astrophysical Journal Pub Date : 2025-06-02 DOI: 10.3847/1538-4357/adcf9d

Charles J. Lada, Jan Forbrich, Mark R. Krumholz and Eric Keto

{"title":"The Role of Pressure in the Structure and Stability of GMCs in the Andromeda Galaxy","authors":"Charles J. Lada, Jan Forbrich, Mark R. Krumholz and Eric Keto","doi":"10.3847/1538-4357/adcf9d","DOIUrl":"https://doi.org/10.3847/1538-4357/adcf9d","url":null,"abstract":"We revisit the role of pressure in the structure, stability, and confinement of Giant Molecular Clouds (GMCs) in light of recently published observations and analysis of the GMCs in the Andromeda galaxy (M31). That analysis showed that, in the absence of any external pressure, most GMCs (57% by number) in M31 would be gravitationally unbound. Here, after a more detailed examination of the global measurements of surface densities and velocity dispersions, we find that GMCs in M31, when they can be traced to near their outermost molecular boundaries, require external pressures for confinement that are consistent with estimates for the mid-plane pressure of this galaxy. We introduce and apply a novel methodology to measure the radial profile of internal pressure within any GMC that is spatially resolved by the CO observations. We show that, for the best-resolved examples in M31, the internal pressures increase steeply with surface density in a power-law fashion with pint ∼ Σ2. At high surface densities, many of these extragalactic GMC profiles break from the single power-law and exhibit upward curvature. Both these characteristics of the variation of internal pressure with surface density are in agreement with theoretical expectations for hydrostatic equilibrium at each radial surface of a GMC, including the outermost boundary.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"70 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144202112","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

Multicomponent Ionized Gas Outflows in the Hot Dust-obscured Galaxy W2026+0716 with Keck/OSIRIS 热尘埃遮蔽星系W2026+0716的多组分电离气体流出与Keck/OSIRIS

The Astrophysical Journal Pub Date : 2025-06-02 DOI: 10.3847/1538-4357/adc9b5

Chao Liu, Chao-Wei Tsai, Peter R. M. Eisenhardt, Hyunsung D. Jun, Guodong Li, Jingwen Wu, Roberto J. Assef, Andrew W. Blain, Maren Cosens, Tanio Díaz-Santos, Román Fernández Aranda, Lei Hao, Mai Liao, Shuai Liu, Daniel Stern, Andrey Vayner, Shelley Wright and Sherry Yeh

{"title":"Multicomponent Ionized Gas Outflows in the Hot Dust-obscured Galaxy W2026+0716 with Keck/OSIRIS","authors":"Chao Liu, Chao-Wei Tsai, Peter R. M. Eisenhardt, Hyunsung D. Jun, Guodong Li, Jingwen Wu, Roberto J. Assef, Andrew W. Blain, Maren Cosens, Tanio Díaz-Santos, Román Fernández Aranda, Lei Hao, Mai Liao, Shuai Liu, Daniel Stern, Andrey Vayner, Shelley Wright and Sherry Yeh","doi":"10.3847/1538-4357/adc9b5","DOIUrl":"https://doi.org/10.3847/1538-4357/adc9b5","url":null,"abstract":"We present narrowband-filtered integral field unit observations of the hot dust-obscured galaxy (Hot DOG) WISE J202615.27+071624.0 (hereafter W2026+0716) at redshift z = 2.570 using Keck/OSIRIS. Our analysis reveals a multicomponent ionized gas outflow structure in this heavily obscured active galactic nucleus (AGN) host galaxy. Multicomponent Gaussian decomposition of the [O iii] and Hα emission lines uncovers extremely broad and asymmetric profiles, characteristic of AGN-driven outflows. Kinematic mapping shows spatially distinct structures: the [O iii]- and Hα-dominated components (with radii of 1.20 ± 0.56 kpc) are separated by a projected offset of ∼1.1 kpc and exhibit divergent velocity regimes. The [O iii] outflow reaches a velocity of 3210 ± 50 km s−1, while the Hα outflow component attains 2310±840 km s−1. Dynamical modeling supports a biconical outflow structure, with [O iii] and Hα emissions dominating separate cones and significant dust obscuration of the redshifted outflow. Their comparable momentum outflow rates and energy outflow rates suggest a potential physical connection in their driving mechanisms. Spectral energy distribution analysis reveals anomalous optical/UV excess, attributed to AGN photon scattering by dust or outflowing material, classifying W2026+0716 as a “Blue Hot DOG”. The derived outflow timescale (∼105 yr) aligns with the evolutionary phase of Blue Hot DOGs, suggesting AGN feedback operates persistently during this transitional stage.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"62 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211135","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 Low Metallicity Massive Contact Binary Star System Candidate in WLM Identified by Hubble and James Webb Space Telescope Imaging 哈勃和詹姆斯·韦伯太空望远镜成像发现的WLM中一颗低金属丰度大质量接触双星系统候选者

The Astrophysical Journal Pub Date : 2025-06-02 DOI: 10.3847/1538-4357/adca39

Maude Gull, Daniel R. Weisz, Kareem El-Badry, Jan Henneco, Alessandro Savino, Meredith Durbin, Yumi Choi, Roger E. Cohen, Andrew A. Cole, Matteo Correnti, Julianne J. Dalcanton, Karoline M. Gilbert, Steven R. Goldman, Puragra Guhathakurta, Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman and Benjamin F. Williams

{"title":"A Low Metallicity Massive Contact Binary Star System Candidate in WLM Identified by Hubble and James Webb Space Telescope Imaging","authors":"Maude Gull, Daniel R. Weisz, Kareem El-Badry, Jan Henneco, Alessandro Savino, Meredith Durbin, Yumi Choi, Roger E. Cohen, Andrew A. Cole, Matteo Correnti, Julianne J. Dalcanton, Karoline M. Gilbert, Steven R. Goldman, Puragra Guhathakurta, Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman and Benjamin F. Williams","doi":"10.3847/1538-4357/adca39","DOIUrl":"https://doi.org/10.3847/1538-4357/adca39","url":null,"abstract":"We present archival Hubble Space Telescope (HST) and JWST ultraviolet through near-infrared time series photometric observations of a massive minimal-contact binary candidate in the metal-poor galaxy Wolf–Lundmark–Melotte (Z = 0.14Z⊙). This discovery marks the lowest metallicity contact binary candidate observed to date. We determine the nature of the two stars in the binary by using the eclipsing binary modeling software PHysics Of Eclipsing BinariEs (PHOEBE) to train a neural network to fit our observed panchromatic multiepoch photometry. The best-fit model consists of two hot main-sequence stars ( K, M⊙, and K, M⊙). We discuss plausible evolutionary paths for the system, and suggest the system is likely to be currently in a contact phase. Future spectroscopy will help to further narrow down evolutionary pathways. This work showcases a novel use of data of JWST and HST imaging originally taken to characterize RR Lyrae. We expect time series imaging from LSST, BlackGEM, etc. to uncover similar types of objects in nearby galaxies.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"14 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211137","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

Evidence for a Catastrophically Disrupted Open Cluster 灾难性疏散星团被破坏的证据

The Astrophysical Journal Pub Date : 2025-06-02 DOI: 10.3847/1538-4357/adceb8

Alexis N. Miller, Kyle R. Tregoning, Jeff J. Andrews, Simon C. Schuler, Jason L. Curtis, Marcel A. Agüeros, Phillip A. Cargile and Julio Chanamé

{"title":"Evidence for a Catastrophically Disrupted Open Cluster","authors":"Alexis N. Miller, Kyle R. Tregoning, Jeff J. Andrews, Simon C. Schuler, Jason L. Curtis, Marcel A. Agüeros, Phillip A. Cargile and Julio Chanamé","doi":"10.3847/1538-4357/adceb8","DOIUrl":"https://doi.org/10.3847/1538-4357/adceb8","url":null,"abstract":"Of the many discoveries uncovered by the Gaia astrometric mission, some of the most exciting are related to nearby dispersed stellar structures. We analyze one such structure in the Milky Way disk, OCSN-49, a coeval stellar stream with 257 identified members spanning approximately 30° across the sky. We obtained high-resolution spectroscopic data for four members that span the stream’s extent, finding these four stars to have solar metallicities and remarkably homogeneous chemistry. Through a combination of isochrone fitting, lithium abundance analysis, and gyrochronology, we find a consistent stellar age of 400–600 Myr. Integrating stellar orbits backwards reveals that OCSN-49 converged to a single point at a much younger age. By integrating unbound model stars forward and comparing them to the current phase-space distribution of OCSN-49, we derive a dynamical age of 83 ± 1 Myr, inconsistent with the age of the stellar population. The discrepancy between the kinematic and stellar age indicators is naturally explained by a disruptive event that unbound OCSN-49 roughly 500 Myr into its lifetime. Based on rate estimates, disruption due to a passing giant molecular cloud (GMC) is the most likely culprit. Assuming a single encounter, we find that a nearly head-on collision with a fairly massive GMC (∼105M⊙) was necessary to unbind the cluster, although encounters with multiple GMCs may be responsible. To our knowledge, OCSN-49 serves as the first known remnant of a catastrophically disrupted open cluster, and therefore serves as a benchmark for further investigating cluster disruption in the Milky Way.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"26 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211138","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

SMILES: Potentially Higher Ionizing Photon Production Efficiency in Overdense Regions 在超密集区域中潜在的更高的电离光子产生效率

The Astrophysical Journal Pub Date : 2025-06-02 DOI: 10.3847/1538-4357/add263

Yongda Zhu, Stacey Alberts, Jianwei Lyu, Jane Morrison, George H. Rieke, Yang Sun, Jakob M. Helton, Zhiyuan Ji, Rachana Bhatawdekar, Nina Bonaventura, Andrew J. Bunker, Xiaojing Lin, Marcia J. Rieke, Pierluigi Rinaldi, Irene Shivaei, Christopher N. A. Willmer and Junyu Zhang

{"title":"SMILES: Potentially Higher Ionizing Photon Production Efficiency in Overdense Regions","authors":"Yongda Zhu, Stacey Alberts, Jianwei Lyu, Jane Morrison, George H. Rieke, Yang Sun, Jakob M. Helton, Zhiyuan Ji, Rachana Bhatawdekar, Nina Bonaventura, Andrew J. Bunker, Xiaojing Lin, Marcia J. Rieke, Pierluigi Rinaldi, Irene Shivaei, Christopher N. A. Willmer and Junyu Zhang","doi":"10.3847/1538-4357/add263","DOIUrl":"https://doi.org/10.3847/1538-4357/add263","url":null,"abstract":"The topology of reionization and the environments where galaxies efficiently produce ionizing photons are key open questions. For the first time, we investigate the trend between ionizing photon production efficiency, ξion, and galaxy overdensity, . We analyze the ionizing properties of 79 galaxies between 1.0 < z < 5.2 using JWST NIRSpec medium-resolution spectra from the Systematic Mid-infrared Instrument Legacy Extragalactic Survey (SMILES) program. Among these, 67 galaxies have Hα coverage, spanning 1.0 < z < 3.1. The galaxy overdensity, , is measured using the JADES photometric catalog, which covers the SMILES footprint. For the subset with Hα coverage, we find that is positively correlated with , with a slope of . Additionally, the mean ξion for galaxies in overdense regions ( ) is 2.43 times that of galaxies in lower density regions ( ). This strong trend is found to be independent of redshift evolution. Furthermore, our results confirm the robust correlations between ξion and the rest-frame equivalent widths of the [O iii] or Hα emission lines. Our results suggest that galaxies in high-density regions are efficient producers of ionizing photons.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"36 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144202033","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

Multifluid and Kinetic 2D and 3D Simulations of Thermal Farley–Buneman Instability Turbulence in the Solar Chromosphere 太阳色球层热法利-布曼不稳定湍流的多流体和动力学二维和三维模拟

The Astrophysical Journal Pub Date : 2025-06-02 DOI: 10.3847/1538-4357/adcd70

Samuel Evans, Meers Oppenheim, Juan Martínez-Sykora and Yakov Dimant

引用次数: 0

Galaxy Cluster Characterization with Machine Learning Techniques 用机器学习技术表征星系团

The Astrophysical Journal Pub Date : 2025-06-02 DOI: 10.3847/1538-4357/adcd69

M. Sadikov, J. Hlavacek-Larrondo, L. Perreault-Levasseur, C. L. Rhea, M. McDonald, M. Ntampaka and J. ZuHone

{"title":"Galaxy Cluster Characterization with Machine Learning Techniques","authors":"M. Sadikov, J. Hlavacek-Larrondo, L. Perreault-Levasseur, C. L. Rhea, M. McDonald, M. Ntampaka and J. ZuHone","doi":"10.3847/1538-4357/adcd69","DOIUrl":"https://doi.org/10.3847/1538-4357/adcd69","url":null,"abstract":"We present an analysis of the X-ray properties of the galaxy cluster population in the z = 0 snapshot of the IllustrisTNG simulations, utilizing machine learning techniques to perform clustering and regression tasks. We examine five properties of the hot gas (the central cooling time, the central electron density, the central entropy excess, the concentration parameter, and the cuspiness) which are commonly used as classification metrics to identify cool core (CC), weak cool core (WCC) and non-cool core (NCC) clusters of galaxies. Using mock Chandra X-ray images as inputs, we first explore an unsupervised clustering scheme to see how the resulting groups correlate with the CC/WCC/NCC classification based on the different criteria. We observe that the groups replicate almost exactly the separation of the galaxy cluster images when classifying them based on the concentration parameter. We then move on to a regression task, utilizing a ResNet model to predict the value of all five properties. The network is able to achieve a mean percentage error of 1.8% for the central cooling time, and a balanced accuracy of 0.83 on the concentration parameter, making them the best-performing metrics. Finally, we use simulation-based inference to extract posterior distributions for the network predictions. Our neural network simultaneously predicts all five classification metrics using only mock Chandra X-ray images. This study demonstrates that machine learning is a viable approach for analyzing and classifying the large galaxy cluster data sets that will soon become available through current and upcoming X-ray surveys, such as the extended Roentgen Survey with an Imaging Telescope Array.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"44 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144211136","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

Characterizing Chromospheric Condensation with High-cadence Si iv Observations from IRIS 用IRIS高节奏Si - iv观测表征色球凝结

The Astrophysical Journal Pub Date : 2025-06-02 DOI: 10.3847/1538-4357/add3fc

Chunming Zhu, Willow Reed, Alysa Derks and Dana Longcope

{"title":"Characterizing Chromospheric Condensation with High-cadence Si iv Observations from IRIS","authors":"Chunming Zhu, Willow Reed, Alysa Derks and Dana Longcope","doi":"10.3847/1538-4357/add3fc","DOIUrl":"https://doi.org/10.3847/1538-4357/add3fc","url":null,"abstract":"Chromospheric flare ribbons are believed to result from coronal magnetic energy released by reconnection and propagating down to the cooler, lower atmosphere. They offer an opportunity to study flare reconnection using chromospheric observations at a spatial and temporal resolution higher than typically available by direct coronal observation. Transient downflows, known as chromospheric condensations (CCs), often occur at the leading edge of a ribbon as a prompt response to the energy input. These have properties that have recently been shown to relate to the coronal energy release process driving them. We use a set of IRIS observations of flare ribbons, made at high cadence in the sit-and-stare mode, to identify and analyze a sample of 134 CC episodes. Among this sample, 132 episodes have at least one time frame that exhibited a double-Gaussian profile. Clear CC appears to occur in only about one fifth of all ribbon pixels, indicating that flare energy release is necessary but not sufficient for producing the characteristic form of CC. We find that condensation pixels form clusters averaging 1 arcsec in extent, all undergoing similar and concurrent time evolution. This suggests that coronal reconnection and associated energy release occur in localized patches whose spatial extent maps to around 1 arcsec in the chromosphere.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"30 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144202069","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

Further Investigations into Emission Components of PSR B0950+08 and Correlations between Them with Single Pulses PSR B0950+08发射成分与单脉冲相关性的进一步研究

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/add1d9

Jie Liu, Zhen Yan, Hao Tong, Hong-Guang Wang, Zhi-Qiang Shen, Rui Wang, Xiao-Wei Wang and Zhi-Peng Huang

{"title":"Further Investigations into Emission Components of PSR B0950+08 and Correlations between Them with Single Pulses","authors":"Jie Liu, Zhen Yan, Hao Tong, Hong-Guang Wang, Zhi-Qiang Shen, Rui Wang, Xiao-Wei Wang and Zhi-Peng Huang","doi":"10.3847/1538-4357/add1d9","DOIUrl":"https://doi.org/10.3847/1538-4357/add1d9","url":null,"abstract":"With the phase-to-phase cross-correlation method, we analyzed the single pulses of PSR B0950+08 obtained at the Five-hundred-meter Aperture Spherical radio Telescope. The correlation map produced with the single pulses reveals a modulation of the correlation coefficients, which are between the intensities at different phases of the single pulses. The modulation varies by a period of two phase bins with 2048 bins over the whole pulse phase. Such a modulation is related to the microstructures of the single pulses and may ultimately imply that the Lorentz factors of the charged particles in the pulsar magnetosphere are highly similar along the line of sight trajectory. The modulation rule reverses after a constant phase separation of . It also reverses around the peak phase of the mean pulse profile, implying that the Lorentz factors are different from the normal value around the reversal phase. According to the analyses with the correlation map, we propose that the bridge emission between the main pulse (MP) and its preceding interpulse (IP) is the overlap of the MP and the IP. For the “weak emission” trailing the MP, it is identified as an independent profile component. There are strong emissions from the IP but no giant pulse from the MP during this observation. The correlation between the IPs and the MPs is mainly dominated by the positive correlations between the subcomponents of the IP and one subcomponent of the MP, according to our analyses.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"41 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193021","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