The Astrophysical Journal最新文献_第10页

An Analytical Galactic Chemical Evolution Model with Gas Inflow and a Terminal Wind

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb729

Kateryna A. Kvasova and Evan N. Kirby

引用次数: 0

Rising from the Ashes: A Metallicity-dependent Star Formation Gap Splits the Milky Way’s α Sequences

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb83e

Angus Beane

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ULX Collimation by Outflows in Moderately Magnetized Neutron Stars

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb714

Fatemeh Kayanikhoo, Włodek Kluźniak and Miljenko Čemeljić

引用次数: 0

Cosmological Predictions for Minor Axis Stellar Density Profiles in the Inner Regions of Milky Way–mass Galaxies

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb9e8

Madeline Lucey, Robyn E. Sanderson, Danny Horta, Aritra Kundu, Philip F. Hopkins, Arpit Arora, Jasjeev Singh and Nondh Panithanpaisal

{"title":"Cosmological Predictions for Minor Axis Stellar Density Profiles in the Inner Regions of Milky Way–mass Galaxies","authors":"Madeline Lucey, Robyn E. Sanderson, Danny Horta, Aritra Kundu, Philip F. Hopkins, Arpit Arora, Jasjeev Singh and Nondh Panithanpaisal","doi":"10.3847/1538-4357/adb9e8","DOIUrl":"https://doi.org/10.3847/1538-4357/adb9e8","url":null,"abstract":"ΛCDM cosmology predicts the hierarchical formation of galaxies, which build up mass by merger events and accreting smaller systems. The stellar halo of the Milky Way (MW) has proven to be useful a tool for tracing this accretion history. However, most of this work has focused on the outer halo where dynamical times are large and the dynamical properties of accreted systems are preserved. In this work, we investigate the inner galaxy regime, where dynamical times are relatively small and systems are generally completely phase mixed. Using the FIRE-2 and Auriga cosmological zoom-in simulation suites of MW-mass galaxies, we find the stellar density profiles along the minor axis (perpendicular to the galactic disk) within the Navarro–Frenk–White scale radii (R ≈ 15 kpc) are best described as an exponential disk with scale height < 0.3 kpc and a power-law component with slope α ≈ −4. The stellar density amplitude and slope for the power-law component are not significantly correlated with metrics of the galaxy’s accretion history. Instead, we find the stellar profiles strongly correlate with the dark matter profile. Across simulation suites, the galaxies studied in this work have a stellar-to-dark-matter mass ratio that decreases as 1/r2 along the minor axis.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"93 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665957","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

Toward Multienergy Neutrino Astronomy: Diagnosing Enhanced Circumstellar Material around Stripped-envelope Supernovae 迈向多能中微子天文学：诊断剥离包囊超新星周围增强的环恒星物质

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb721

Ryo Sawada and Yosuke Ashida

{"title":"Toward Multienergy Neutrino Astronomy: Diagnosing Enhanced Circumstellar Material around Stripped-envelope Supernovae","authors":"Ryo Sawada and Yosuke Ashida","doi":"10.3847/1538-4357/adb721","DOIUrl":"https://doi.org/10.3847/1538-4357/adb721","url":null,"abstract":"A novel approach is proposed to reveal a secret birth of enhanced circumstellar material (CSM) surrounding a collapsing massive star using neutrinos as a unique probe. In this scheme, nonthermal TeV-scale neutrinos produced in ejecta–CSM interactions are tied with thermal MeV neutrinos emitted from a pre-explosion burning process, based on a scenario that CSM had been formed via the presupernova activity. Taking a representative model of the presupernova neutrinos, the spectrum and light curve of the corresponding high-energy CSM neutrinos are calculated at multiple mass-loss efficiencies, which are considered as a systematic uncertainty. In addition, as a part of the method demonstration, the detected event rates along time at JUNO and IceCube, as representative detectors, are estimated for the presupernova and CSM neutrinos, respectively, and are compared with the expected background rate at each detector. The presented method is found to be reasonably applicable for the range up to ∼1 kpc and even farther with future experimental efforts. The potentialities of other neutrino detectors, such as SK-Gd, Hyper-Kamiokande, and KM3NeT, are also discussed. This is a pioneering work of performing astrophysics with neutrinos from diverse energy regimes, initiating multienergy neutrino astronomy in the forthcoming era where next-generation large-scale neutrino telescopes are operating.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"56 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665950","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 New Reaction Rate of the 27Al(p,γ)28Si Reaction Based on Indirect Low-energy Cross-section Measurements 基于间接低能截面测量的 27Al(p,γ)28Si 反应的新反应速率

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb7e4

M. La Cognata, S. Palmerini, F. Dell’Agli, P. Ventura, P. Adsley, R. Alba, S. Cherubini, M. Costa, A. Di Pietro, P. Figuera, G. L. Guardo, M. Gulino, F. Hammache, M. La Commara, L. Lamia, D. Lattuada, C. Maiolino, M. Mazzocco, A. Oliva, R. G. Pizzone, P. M. Prajapati, G. G. Rapisarda, S. Romano, D. Santonocito, M. L. Sergi, R. Spartá and A. Tumino

{"title":"A New Reaction Rate of the 27Al(p,γ)28Si Reaction Based on Indirect Low-energy Cross-section Measurements","authors":"M. La Cognata, S. Palmerini, F. Dell’Agli, P. Ventura, P. Adsley, R. Alba, S. Cherubini, M. Costa, A. Di Pietro, P. Figuera, G. L. Guardo, M. Gulino, F. Hammache, M. La Commara, L. Lamia, D. Lattuada, C. Maiolino, M. Mazzocco, A. Oliva, R. G. Pizzone, P. M. Prajapati, G. G. Rapisarda, S. Romano, D. Santonocito, M. L. Sergi, R. Spartá and A. Tumino","doi":"10.3847/1538-4357/adb7e4","DOIUrl":"https://doi.org/10.3847/1538-4357/adb7e4","url":null,"abstract":"The Mg–Al cycle is characteristic of the high-temperature (T ∼ 0.055 GK) H-burning of evolved stars and their nucleosynthesis. A proper comprehension of this reaction network can help in solving debated questions such as the occurrence of anticorrelation in Mg–Al abundances in globular clusters. Recent high-resolution surveys have shown that such an anticorrelation may hide the existence of multiple stellar populations and that the relative abundances of Mg isotopes may not be correlated with Al. Proton-induced reactions on 27Al play a key role in this respect, in particular the interplay between the (p, α) and (p, γ) channels, determining the closure (or not) of the Mg–Al cycle. Presently, the situation is still debated owing to the large uncertainty affecting existing experimental nuclear data. A recent indirect measurement indicates a further reduction in the 27Al(p, α)24Mg reaction rate with respect to the ones commonly adopted in astrophysical models. In the present work, we update the 27Al(p,γ)28Si reaction rate based on the same indirect measurement results. In the case of AGB stars experiencing hot bottom burning, the revised rate would lead to a ∼35% increase in 27Al abundance with respect to what is presently foreseen, with interesting astrophysical consequences.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"14 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665952","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

Single-pulse Morphology of PSR J1935+1616 (B1933+16) Based on Archival Data from FAST 基于 FAST 存档数据的 PSR J1935+1616 (B1933+16) 单脉冲形态学

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb7cd

R. W. Tian, R. S. Zhao, Marilyn Cruces, H. Liu, D. Li, P. Wang, C. H. Niu, Biping Gong, C. C. Miao, X. Zhu, H. W. Xu, W. L. Li, S. D. Wang, Z. F. Tu, Q. J. Zhi, S. J. Dang, L. H. Shang and S. Xiao

{"title":"Single-pulse Morphology of PSR J1935+1616 (B1933+16) Based on Archival Data from FAST","authors":"R. W. Tian, R. S. Zhao, Marilyn Cruces, H. Liu, D. Li, P. Wang, C. H. Niu, Biping Gong, C. C. Miao, X. Zhu, H. W. Xu, W. L. Li, S. D. Wang, Z. F. Tu, Q. J. Zhi, S. J. Dang, L. H. Shang and S. Xiao","doi":"10.3847/1538-4357/adb7cd","DOIUrl":"https://doi.org/10.3847/1538-4357/adb7cd","url":null,"abstract":"We utilized archive data from the Five-hundred-meter Aperture Spherical Radio Telescope (FAST) to analyze the single-pulse profile morphology of PSR J1935+1616 (B1933+16). The results show that PSR J1935+1616 exhibits significant micropulses as well as various changes in single-pulse profile morphology. In the FAST archive data, a total of 969 single pulses with microstructure were identified, accounting for 9.69% of the total pulse sample, with characteristic widths of μs. About half of these pulses display quasiperiodic micropulses, with a periodicity of 231.77 ± 9.90 μs. Among the 520 single pulses with quasiperiodic microstructure, 208 also exhibit quasiperiodicity in circular polarization, with a characteristic period of . The micropulse characteristic width in circular polarization is 106.52 ± 46.14 μs. Compared to normal pulses, the relative energy (E/<E>) of a single pulse with microstructure follows a double-Gaussian distribution, while those of normal pulses follow a single-Gaussian distribution. Based on the intensity of the leading and trailing components in the single-pulse profile morphology of PSR J1935+1616, we classified the pulses into four morphological modes (A, B, C, and D). The relative energy distribution of pulses in Mode A is significantly different from the others, following a double-Gaussian distribution, while the relative energy distributions in Modes B, C, and D follow a single-Gaussian distribution. Our study also suggests a possible correlation between micropulses and single-pulse profile morphology. Single pulses with micropulses are most likely to occur in Mode A, while their occurrence is least likely in Mode D.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143672336","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

Spatial and Chemical Complexity in the W75N Star-forming Region

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb62d

Morgan M. Giese, Will E. Thompson, Dariusz C. Lis and Susanna L. Widicus Weaver

{"title":"Spatial and Chemical Complexity in the W75N Star-forming Region","authors":"Morgan M. Giese, Will E. Thompson, Dariusz C. Lis and Susanna L. Widicus Weaver","doi":"10.3847/1538-4357/adb62d","DOIUrl":"https://doi.org/10.3847/1538-4357/adb62d","url":null,"abstract":"We present the analysis of NOEMA interferometric observations of the high-mass star-forming region W75N(B) with a focus on molecular composition and distribution of prebiotic molecules in the source’s multiple cores. Over 20 molecules are identified across the region, with many being fit for column density, rotational temperature, spectral line FWHM, and vlsr. This work includes the first known detection and initial analysis of complex organic molecules in the MM2 and MM3 regions. Furthermore, parameter maps were created from the six molecules that were well fit across multiple regions. The molecular emission was imaged and correlated across different molecules and the continuum to reveal structural features. From the spatial and spectral analysis of the MM1 region, these results concur with those from other studies showing that there is a difference in chemical composition between the MM1a and MM1b regions, with sulfur-bearing molecules tracing MM1a and organic molecules tracing MM1b. The molecular emission imaged toward the MM3 region reveals two peaks, possibly indicating the presence of multiple young stellar objects. These results provide detailed quantitative information about the physical parameters and distributions of molecules in this source. Additionally, these results are part of a follow-up of a single-dish survey of multiple star-forming regions and are discussed in this context.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677586","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

Recovering Ion Distribution Functions. I. Slepian Reconstruction of Velocity Distribution Functions from MMS and Solar Orbiter

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb6a0

Srijan Bharati Das and Michael Terres

{"title":"Recovering Ion Distribution Functions. I. Slepian Reconstruction of Velocity Distribution Functions from MMS and Solar Orbiter","authors":"Srijan Bharati Das and Michael Terres","doi":"10.3847/1538-4357/adb6a0","DOIUrl":"https://doi.org/10.3847/1538-4357/adb6a0","url":null,"abstract":"Plasma velocity distribution functions (VDFs) constitute a fundamental observation of numerous operational and future missions. An efficient parameterization of VDFs is crucial for (1) preserving enough information to investigate macroscopic moments along with kinetic effects, (2) producing smooth distributions whereby it is possible to perform derivatives in phase space to support numerical solvers, and (3) economic data management and its storage. Previous studies have used spherical harmonics as an efficient basis for representing electron VDFs. In this paper, we present a novel algorithm targeted toward decomposing ion VDFs measured by electrostatic analyzers on board Magnetospheric Multiscale (MMS) Mission and Solar Orbiter (SolO) spacecraft. We use Slepian functions, custom-designed bases providing compact support in phase space, initially developed in information theory and later used for terrestrial and planetary applications. In this paper, we choose well-studied, well-measured, and complex intervals from MMS and SolO containing a range of simpler gyrotropic and agyrotropic distributions to benchmark the robustness of our reconstruction method. We demonstrate the advantages of using Slepian functions over spherical harmonics for solar wind plasma distributions. We also demonstrate that our choice of basis representation efficiently preserves phase space complexities of a 3D agyrotropic distribution function. This algorithm shown in this study will be extended to Parker Solar Probe and future missions such as Helioswarm.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"70 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665883","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

Compton Scattering of Thermal Disk Radiation with Black Hole Disk Winds

The Astrophysical Journal Pub Date : 2025-03-21 DOI: 10.3847/1538-4357/adb962

Keigo Fukumura

{"title":"Compton Scattering of Thermal Disk Radiation with Black Hole Disk Winds","authors":"Keigo Fukumura","doi":"10.3847/1538-4357/adb962","DOIUrl":"https://doi.org/10.3847/1538-4357/adb962","url":null,"abstract":"Galactic black hole (BH) X-ray binaries (XRBs) are known to exhibit episodic outbursts, during which accretion and spectral mode distinctively transition between low/hard and high/soft state. X-ray observations during high/soft state occasionally reveal a pronounced presence of a powerful disk wind in these systems. However, it is unexplored to date how such winds may influence disk emission in that regime. In this work, we consider an observational implication by Compton scattering of thermal disk radiation due to accretion disk winds by performing multidimensional Monte Carlo simulations in the context of a stratified wind of large solid angle launched over a large radial extent of the disk. The Compton-scattered thermal disk spectrum is computed for a different wind property, i.e., wind density and its radial gradient. We find that the intrinsic disk radiation can be significantly down-scattered by winds of moderate-to-high density to the extent that the transmitted spectrum can substantially deviate from the conventional multicolor-disk emission in a tangible way. We thus claim that the conventional treatment of spectral hardening in the disk atmosphere may be insufficient to fully account for the observed disk continuum in the presence of strong wind scattering. It is suggested that the effect of scattering process (by fw) should be incorporated to accurately evaluate an intrinsic disk spectrum besides the conventional hardening (color correction) factor (by fc). We argue that BH spin measurements using thermal continuum-fitting in transient XRBs may well be mildly (if not significantly) altered by such spectral “contamination.”","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"77 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665956","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