The Astrophysical Journal最新文献_第4页

On the Formation of Star-forming Galaxies Having Anomalously Low-metallicity Regions: The Role of Galaxy Interaction and Circumgalactic Medium/Intergalactic Medium Accretion 具有异常低金属丰度区域的造星星系的形成：星系相互作用和星系周围介质/星系间介质吸积的作用

The Astrophysical Journal Pub Date : 2025-10-12 DOI: 10.3847/1538-4357/ae0a10

Yibo Cao and Zhizheng Pan

{"title":"On the Formation of Star-forming Galaxies Having Anomalously Low-metallicity Regions: The Role of Galaxy Interaction and Circumgalactic Medium/Intergalactic Medium Accretion","authors":"Yibo Cao and Zhizheng Pan","doi":"10.3847/1538-4357/ae0a10","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0a10","url":null,"abstract":"Gas accretion from both the circumgalactic medium (CGM)/intergalactic medium (IGM) and interacting companion galaxy can dilute the gas phase metallicity of a galaxy. However, their relative contribution to the chemical evolution of galaxies remains to be quantified. To this end, in this work we study a sample of 510 star-forming galaxies (SFGs) having anomalously low-metallicity (ALM) regions selected from the MaNGA data available in the Data Release 17 from the Sloan Digital Sky Survey. ALM regions are defined as those having gas-phase metallicities that are at least ∼2σ lower than the empirical relation between stellar mass surface density (Σ*) and gas phase metallicity, i.e., the Σ*–Z relation. We find that ALM galaxies have higher star formation rates and H i gas fractions than normal SFGs at fixed M*. Also, ∼25% of the ALM galaxies exhibit tidal features, while the tidal fraction is only ∼12% for normal SFGs, indicating that galaxy interaction is an important factor responsible for the ALM phenomenon. To explore the origin of nontidal ALM galaxies, we compare their morphologies and environments with those of mass-matched normal SFGs. We find that nontidal ALM galaxies tend to have more disk-dominated morphologies and reside in less-dense environment. These findings suggest that cold gas accretion from the CGM/IGM is the primary cause for the ALM phenomenon, while galaxy interaction plays a minor but nonnegligible role.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"38 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145277452","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

Breaking Gyrochronology through the Collapse of Coronal Winds 通过日冕风的崩塌打破陀螺年代学

The Astrophysical Journal Pub Date : 2025-10-12 DOI: 10.3847/1538-4357/ae03b0

Michaël Lévesque and Paul Charbonneau

{"title":"Breaking Gyrochronology through the Collapse of Coronal Winds","authors":"Michaël Lévesque and Paul Charbonneau","doi":"10.3847/1538-4357/ae03b0","DOIUrl":"https://doi.org/10.3847/1538-4357/ae03b0","url":null,"abstract":"Gyrochronology, a method for dating aged field stars (≳a few Gyr) based on their rotation rate, has recently been shown to fail for many stars older than the Sun. The explanation most often put forth is that a shutdown or mode change in the stellar dynamo leads to a sharp decrease in angular momentum loss in magnetized coronal winds. In this paper, we explore an alternate possibility, namely, a collapse of the wind itself through a reduction of coronal heating. We show that in the low coronal temperature (T0) limit, even at solar-like low rotation rates (Ω) and coronal magnetic field strength (Br0), magnetocentrifugal effects are important and preclude expression of the mass and angular momentum loss rates as power laws of T0 or Ω when T0 drops below ≃1.5 MK. Mass loss is found to scale linearly with power input into the wind at all coronal temperatures. Introducing an ad hoc power-law relationship while retaining the “standard” dynamo relationship Br0 ∝ Ω, we show that reproducing the observed break in gyrochronology requires an exponent σ ≳ 1.5, which is associated with a drop by over 3 orders of magnitude in power input into the quiet corona. This appears physically unrealistic, given current observations of chromospheric and coronal nonthermal emission in aged solar-type stars.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"86 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145277439","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

Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing 在4.97小时轨道上运行的白矮星的罗氏极限附近凌日的行星碎片及其消失

The Astrophysical Journal Pub Date : 2025-10-12 DOI: 10.3847/1538-4357/adfecb

Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez and Jan van Roestel

{"title":"Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing","authors":"Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez and Jan van Roestel","doi":"10.3847/1538-4357/adfecb","DOIUrl":"https://doi.org/10.3847/1538-4357/adfecb","url":null,"abstract":"We present the discovery of deep, irregular, periodic transits toward the white dwarf ZTF J1944+4557 using follow-up time-series photometry and spectroscopy from Palomar, Keck, McDonald, Perkins, and Lowell observatories. We find a predominant period of 4.9704 hr, consistent with an orbit near the Roche limit of the white dwarf, with individual dips over 30% deep and lasting between 15 and 40 minutes. Similar to the first known white dwarf with transiting debris, WD 1145+017, the transit events are well-defined with prominent out-of-transit phases where the white dwarf appears unobscured. Spectroscopy concurrent with transit photometry reveals that the average Ca K equivalent width remains constant in and out of transit. The broadening observed in several absorption features cannot be reproduced by synthetic photospheric models, suggesting the presence of circumstellar gas. Simultaneous g + r- and g + i-band light curves from the CHIMERA instrument reveal no color dependence to the transit depths, requiring transiting dust grains to have sizes s ≳ 0.2 μm. The transit morphologies appear to be constantly changing at a rate faster than the orbital period. Overall transit activity varies in the system, with transit features completely disappearing during the seven months between our 2023 and 2024 observing seasons and then reappearing in 2025 March, still repeating at 4.9704 hr. Our observations of the complete cessation and resumption of transit activity provide a novel laboratory for constraining the evolution of disrupted debris and processes like disk exhaustion and replenishment timescales at white dwarfs.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"377 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145277446","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

Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria 用陀螺年表标准评价旋转周期恢复的极限

The Astrophysical Journal Pub Date : 2025-10-12 DOI: 10.3847/1538-4357/ae03a7

Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida and Ryan J. Reynolds

{"title":"Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria","authors":"Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida and Ryan J. Reynolds","doi":"10.3847/1538-4357/ae03a7","DOIUrl":"https://doi.org/10.3847/1538-4357/ae03a7","url":null,"abstract":"Contamination from nearby sources often compromises stellar rotation periods derived from photometric light curves, particularly in data with large pixel scales such as The Transiting Exoplanet Survey Satellite (TESS). This problem is compounded when both the target and contaminant are intrinsically variable, a scenario that challenges deblending algorithms, which often assume constant contaminants. We assess the reliability of rotation period detections using wide binary systems, whose components share a common age and rotational history. By applying gyrochronology constraints, we identify period combinations that yield consistent ages between components, helping to isolate true rotation signals. Simulating blends with degraded Kepler data, our method recovers correct rotation periods with an 88% success rate for periods <12 days, where TESS detections are most reliable. Applying this framework to nearly 300 wide binaries observed by TESS, we find that, despite significant contamination, a subset of pairs shows consistent gyrochronological ages. We establish a practical detection threshold for TESS blended observations, finding that periods shorter than ∼8 days are reliably recovered, while those longer than ∼10 days become significantly more challenging and often remain inconclusive. As expected, rotation periods are more often recovered when the highest-amplitude periodogram peak is linked to the brighter star and the second to the dimmer star. However, many cases deviate from this pattern, indicating it cannot always be assumed. Our results highlight the limitations of standard deblending methods and demonstrate that astrophysical constraints, such as gyrochronology, provide a valuable tool for extracting reliable rotation periods from complex photometric blends.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"40 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145277436","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

Starspot Temperature of CoRoT-2 from Multiwavelength Observations with SPARC4 SPARC4多波长观测CoRoT-2的星斑温度

The Astrophysical Journal Pub Date : 2025-10-12 DOI: 10.3847/1538-4357/adf8e2

Adriana Valio, Eder Martioli, Andre O. Kovacs, Viktor Y. D. Sumida, Leandro de Almeida, Diego Lorenzo-Oliveira, Francisco Jablonski and Claudia V. Rodrigues

{"title":"Starspot Temperature of CoRoT-2 from Multiwavelength Observations with SPARC4","authors":"Adriana Valio, Eder Martioli, Andre O. Kovacs, Viktor Y. D. Sumida, Leandro de Almeida, Diego Lorenzo-Oliveira, Francisco Jablonski and Claudia V. Rodrigues","doi":"10.3847/1538-4357/adf8e2","DOIUrl":"https://doi.org/10.3847/1538-4357/adf8e2","url":null,"abstract":"Measuring starspot temperatures is crucial for understanding stellar magnetic activity as it affects stellar brightness variations, influences exoplanet transit measurements, and provides constraints on the physical conditions and energy transport in active regions, offering insights into stellar dynamos. Our goal is to determine the temperature of starspots on the active star CoRoT-2 to enhance our understanding of magnetic activity in young, solar-like stars. Multiwavelength observations were conducted using the Simultaneous Polarimeter and Rapid Camera in Four bands instrument on the 1.6 m telescope at Pico dos Dias Observatory (Brazil), capturing simultaneous transit data in four photometric bands (g, r, i, and z). The ECLIPSE model, combined with Markov Chain Monte Carlo fitting, was used to model spot characteristics during the planetary transit of CoRoT-2 b. The spot intensities were analyzed considering three different methods: the assumption of blackbody emission, the PHOENIX atmospheric model, and multiwavelength fitting assuming the same spot parameters for all wavelengths. Two starspots were detected in the residuals of the light curve, yielding temperature estimates of 5040–5280 K based on the three different methods. These values align more closely with the temperatures of solar penumbrae than with typical umbral temperatures, suggesting relatively moderate magnetic activity. The radius of the spots ranged from 0.34 to 0.61 the planetary radius, or equivalently (38–69) × 106 m, much larger than sunspots. This study provides a method to estimate spot temperatures on active stars using multiband photometry, with results indicating penumbral-like temperatures on CoRoT-2. The methodology enhances precision in starspot temperature estimation, beneficial for studies of stellar activity and exoplanet characterization.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"113 4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145277432","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

Development of Turbulence in Postshock Regions 后激波区域湍流的发展

The Astrophysical Journal Pub Date : 2025-10-12 DOI: 10.3847/1538-4357/adfa19

Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist and Alyssa Goodman

引用次数: 0

Fermi Detection of γ-Rays from the Radio-quiet Seyfert Galaxy NGC 3281 Fermi探测来自无线电安静的Seyfert星系NGC 3281的γ射线

The Astrophysical Journal Pub Date : 2025-10-12 DOI: 10.3847/1538-4357/ae07cf

Jun-Rong Liu, Hua Feng and Jian-Min Wang

{"title":"Fermi Detection of γ-Rays from the Radio-quiet Seyfert Galaxy NGC 3281","authors":"Jun-Rong Liu, Hua Feng and Jian-Min Wang","doi":"10.3847/1538-4357/ae07cf","DOIUrl":"https://doi.org/10.3847/1538-4357/ae07cf","url":null,"abstract":"We report the detection of significant γ-ray emission with the Fermi Large Area Telescope from the radio-quiet Seyfert 2 galaxy NGC 3281, with a luminosity of 5.9 (±1.7) × 1041erg s−1 at a significance of 6.22σ (TS = 42.81). The power-law photon index is 2.61 (±0.24), indicative of a soft spectrum. The star formation activity in NGC 3281 is insufficient to explain its γ-ray luminosity based on the empirical relation between the infrared and γ-ray luminosities observed in other sources. The multiwavelength spectrum can be explained as due to inverse Compton scattering by relativistic electrons in the corona or the jet of seed photons from the corona, disk, and torus. The source is Compton thick, and attenuation of GeV photons due to pair production in the corona is nonnegligible (with an optical depth of about 10). The intrinsic γ-ray luminosity is inferred to be 3.4 × 1042 and 2.2 × 1041 erg s−1 for the corona and jet model, respectively. The observed γ-ray and radio luminosities are roughly consistent with the known correlation between the two quantities, among the lowest-luminosity regime. The jet origin is valid only if the radio emission is dominated by the jet.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"38 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145277437","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

Unions with UNIONS: Using Galaxy–Galaxy Lensing to Probe Galaxy Mergers 联合与联合：利用星系-星系透镜探测星系合并

The Astrophysical Journal Pub Date : 2025-10-12 DOI: 10.3847/1538-4357/ae03b8

Isaac Cheng, Jack Elvin-Poole, Michael J. Hudson, Ruxin Barré, Sara L. Ellison, Robert W. Bickley, Thomas J. L. de Boer, Sébastien Fabbro, Leonardo Ferreira, Sacha Guerrini, Fabian Hervas Peters, Hendrik Hildebrandt, Martin Kilbinger, Alan W. McConnachie, Ludovic van Waerbeke and Anna Wittje

{"title":"Unions with UNIONS: Using Galaxy–Galaxy Lensing to Probe Galaxy Mergers","authors":"Isaac Cheng, Jack Elvin-Poole, Michael J. Hudson, Ruxin Barré, Sara L. Ellison, Robert W. Bickley, Thomas J. L. de Boer, Sébastien Fabbro, Leonardo Ferreira, Sacha Guerrini, Fabian Hervas Peters, Hendrik Hildebrandt, Martin Kilbinger, Alan W. McConnachie, Ludovic van Waerbeke and Anna Wittje","doi":"10.3847/1538-4357/ae03b8","DOIUrl":"https://doi.org/10.3847/1538-4357/ae03b8","url":null,"abstract":"We use galaxy–galaxy lensing to investigate how the dark matter (DM) haloes and stellar content of galaxies with 0.012 ≤ z ≤ 0.32 and change as a result of the merger process. To this end, we construct two samples of galaxies obtained from the Ultraviolet Near Infrared Optical Northern Survey, comprising 1623 postmergers and ∼30,000 nonmerging controls, that live in low-density environments to use as our lenses. These samples are weighted to share the same distributions of stellar mass, redshift, and geometric mean distance to a galaxy’s three nearest neighbors to ensure differences in the lensing signal are due to the merger process itself. We do not detect a statistically significant difference in the excess surface density profile of postmergers and nonmerging controls with current data. Fitting haloes composed of a pointlike stellar mass component and an extended DM structure described by a Navarro–Frenk–White profile to the lensing measurements yields, for both samples, halo masses of Mhalo ∼ 4 × 1012M⊙ and a moderately negative correlation between Mhalo and concentration c. This allows us to rule out, at the 95% confidence level, merger-induced starbursts in which more than 60% of the stellar mass is formed in the burst. The application of our methods to upcoming surveys that are able to provide samples ∼10× larger than our current catalog is expected to detect the weak-lensing signatures of mergers and further constrain their properties.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145277447","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 Parallel Ionizing Emissivity Survey (PIE). I. Survey Design and Selection of Candidate Lyman Continuum Leakers at 3.1 < z < 3.5 平行电离发射率测量（PIE）。1 . 3.1 < z < 3.5的Lyman连续体泄密者候选人的调查设计与选择

The Astrophysical Journal Pub Date : 2025-10-09 DOI: 10.3847/1538-4357/ae0291

Alexander Beckett, Marc Rafelski, Claudia Scarlata, Wanjia Hu, Keunho Kim, Ilias Goovaerts, Matthew A. Malkan, Wayne Webb, Harry Teplitz, Matthew Hayes, Vihang Mehta, Anahita Alavi, Andrew J. Bunker, Annalisa Citro, Nimish Hathi, Alaina Henry, Alexandra Le Reste, Alessia Moretti, Michael J. Rutkowski, Maxime Trebitsch and Anita Zanella

{"title":"The Parallel Ionizing Emissivity Survey (PIE). I. Survey Design and Selection of Candidate Lyman Continuum Leakers at 3.1 < z < 3.5","authors":"Alexander Beckett, Marc Rafelski, Claudia Scarlata, Wanjia Hu, Keunho Kim, Ilias Goovaerts, Matthew A. Malkan, Wayne Webb, Harry Teplitz, Matthew Hayes, Vihang Mehta, Anahita Alavi, Andrew J. Bunker, Annalisa Citro, Nimish Hathi, Alaina Henry, Alexandra Le Reste, Alessia Moretti, Michael J. Rutkowski, Maxime Trebitsch and Anita Zanella","doi":"10.3847/1538-4357/ae0291","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0291","url":null,"abstract":"We present the survey design and initial results from the Parallel Ionizing Emissivity (PIE) survey. PIE is a large Hubble Space Telescope survey designed to detect Lyman continuum (LyC) emitting galaxies at 3.1 < z < 3.5 and stack their images in order to measure average LyC escape fractions as a function of galaxy properties. PIE has imaged 37 independent fields in three filters (F336W, F625W, and F814W), of which 18 are observed with a fourth band (F475W) from the accompanying PIE+ program. We use photometric colors to select candidate Lyman break galaxies (LBGs) at 3.1 < z < 3.5, which can be followed up using ground-based spectrographs to confirm their redshifts. Unlike previous surveys, we use many independent fields to remove biases caused by correlated absorption in the intergalactic medium (IGM). In this paper, we describe the survey design, photometric measurements, and the use of mock galaxy samples to optimize our color selection. With three filters, we can select a galaxy sample of which ≈90% are LBGs and over 30% lie in the 3.1 < z < 3.5 range for which we can detect uncontaminated LyC emission in F336W. We also use mock IGM sight lines to measure the expected transmission of the IGM, which will allow us to determine escape fractions from our stacked galaxies. We color-select ≈1400 galaxies, and predict that this includes ≈80 LyC-emitting galaxies and ≈500 that we can use in stacking. Finally, we present the Keck/LRIS spectrum of a galaxy at z ≈ 2.99, demonstrating that we can confirm the redshifts of z ∼ 3 galaxies from the ground.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"110 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255710","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

Eclipsing Millisecond Pulsars with He Star Companions 日食毫秒脉冲星与He星伴星

The Astrophysical Journal Pub Date : 2025-10-09 DOI: 10.3847/1538-4357/ae057b

Yunlang Guo, Bo Wang, Xiangdong Li, Dongdong Liu and Wenshi Tang

{"title":"Eclipsing Millisecond Pulsars with He Star Companions","authors":"Yunlang Guo, Bo Wang, Xiangdong Li, Dongdong Liu and Wenshi Tang","doi":"10.3847/1538-4357/ae057b","DOIUrl":"https://doi.org/10.3847/1538-4357/ae057b","url":null,"abstract":"Eclipsing millisecond pulsars (MSPs) are a type of pulsar binaries with close orbits (≲1.0 day). They are important objects for studying the accretion history of neutron stars (NSs), pulsar winds, and the origin of isolated MSPs, etc. Recently, a new eclipsing MSP, PSR J1928+1815, was discovered by the Five-hundred-meter Aperture Spherical radio Telescope. It is the first known pulsar with a He star companion, as suggested in Yang et al. The system features a short orbital period of ∼0.15 days and a relatively massive companion ≳1.0 M⊙. However, the origin of PSR J1928+1815 remains highly uncertain. In this paper, we investigated the formation of the new subclass of eclipsing MSPs containing (evolved) He star companions through the NS + He star channel. We found that if an NS binary undergoes subsequent mass-transfer phases following Case BA or Case BB, it may appear as an eclipsing MSP during the detached phase. Additionally, we obtained the initial parameter space for producing eclipsing MSPs with He star companions. Using the binary population synthesis approach, we estimated their birth rate to be ∼2.1–4.7 × 10−4 yr−1, corresponding to a total number of ∼220 systems in the Galaxy. Moreover, we concluded that PSR J1928+1815 may originate from the evolution of an NS + He star system with an initial orbital period of ∼0.1 days, which can undergo the Case BB mass transfer.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"338 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255716","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