The Astrophysical Journal Letters最新文献_第10页

Responses of a Coronal Hole to a Fast Flare-driven Coronal Wave 日冕洞对快速耀斑驱动的日冕波的响应

The Astrophysical Journal Letters Pub Date : 2025-06-22 DOI: 10.3847/2041-8213/ade38c

Xiaofan Zhang, Huadong Chen, Guiping Zhou, Li Feng, Yang Su, Jinhan Guo, Leping Li, Wei Lin, Suli Ma, Yuandeng Shen, Ruisheng Zheng, Suo Liu, Xianyong Bai, Yuanyong Deng and Jingxiu Wang

{"title":"Responses of a Coronal Hole to a Fast Flare-driven Coronal Wave","authors":"Xiaofan Zhang, Huadong Chen, Guiping Zhou, Li Feng, Yang Su, Jinhan Guo, Leping Li, Wei Lin, Suli Ma, Yuandeng Shen, Ruisheng Zheng, Suo Liu, Xianyong Bai, Yuanyong Deng and Jingxiu Wang","doi":"10.3847/2041-8213/ade38c","DOIUrl":"https://doi.org/10.3847/2041-8213/ade38c","url":null,"abstract":"Coronal waves, significant solar phenomena, act as diagnostic tools for scientists studying solar atmosphere properties. Here, we present a novel observation detailing how a coronal wave event, associated with an X5.0 class flare, influenced the properties of an adjacent coronal hole (CH) through interaction. The coronal wave was observed in both extreme-ultraviolet (EUV) observations from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory and Lyα observations from the Solar Disk Imager on board the Advanced Space-based Solar Observatory. Utilizing the method of differential emission measure, we found that as the coronal wave passed through, the adjacent CH experienced an increase in temperature from 1.31 to 1.43 MK and a rise in density from ∼1.62 × 108 to 1.76 × 108 cm−3 within the rising period of ∼7 minutes. Subsequently, after the wave passed, the entire CH transitioned to a new state with a slight temperature increase and a 14% decrease in density, with more pronounced changes observed at the CH’s boundary. Taking into account the impacts of radiative loss and heat conduction, the coronal wave was estimated to provide an average energy of 2.2 × 108 erg cm−2 to the CH during the short rising period. This study highlights the identification of the coronal wave in both EUV and Lyα observations, shedding light on the significant energy input, particularly within the CH. These findings provide new insights into better understanding kinematics of fast coronal waves, energy transfer processes open versus closed magnetic topologies, and the possible acceleration of solar winds.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"58 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144370777","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

Dissecting the Massive Pristine, Neutral Gas Reservoir of a Remarkably Bright Galaxy at z = 14.179 解析z = 14.179的一个非常明亮的星系的巨大原始中性气藏

The Astrophysical Journal Letters Pub Date : 2025-06-22 DOI: 10.3847/2041-8213/ade393

Kasper E. Heintz, Clara L. Pollock, Joris Witstok, Stefano Carniani, Kevin N. Hainline, Francesco D’Eugenio, Chamilla Terp, Aayush Saxena and Darach Watson

{"title":"Dissecting the Massive Pristine, Neutral Gas Reservoir of a Remarkably Bright Galaxy at z = 14.179","authors":"Kasper E. Heintz, Clara L. Pollock, Joris Witstok, Stefano Carniani, Kevin N. Hainline, Francesco D’Eugenio, Chamilla Terp, Aayush Saxena and Darach Watson","doi":"10.3847/2041-8213/ade393","DOIUrl":"https://doi.org/10.3847/2041-8213/ade393","url":null,"abstract":"At cosmic dawn, the first stars and galaxies are believed to form from and be deeply embedded in clouds of dense, pristine gas. Here we present a study of the James Webb Space Telescope/NIRSpec data of the most distant, spectroscopically confirmed galaxy observed to date, JADES-GS-z14-0 (GS-z14 for short), at z = 14.179, combined with recently reported far-infrared measurements of the [O iii]-88 μm and [C ii]-158 μm line transitions and underlying dust-continuum emission. Based on the observed prominent damped Lyα (DLA) absorption profile, we determine a substantial neutral atomic hydrogen (H i) column density, , consistent with previous estimates though seemingly at odds with the dynamical and gas mass of the galaxy. Using various independent but complementary approaches, considering the implied neutral gas mass from the DLA measurement, the star formation rate surface density, and the metal abundance, we demonstrate that the total gas mass of GS-z14 is of the order Mgas = 109.5–109.8M⊙. This implies a substantial gas mass fraction, fgas ≈ 0.7–0.9 and that the bulk of the interstellar medium (ISM) is in the form of H i, with mass ratios . We show that the derived gas mass is fully consistent with the nondetection of [C ii]-158 μm, assuming an appropriate scaling to the neutral gas. The low dust-to-gas ratio, AV/NHI = (1.3 ± 0.6) × 10−23 mag cm2, derived in the line of sight through the DLA further indicates that the absorbing gas is more pristine than the central, star-forming regions probed by the [O iii]-88 μm emission. These results highlight the implications for far-infrared line-detection searchers attainable with the Atacama Large Millimeter/submillimeter Array and demonstrate that the bright, relatively massive galaxy GS-z14 at z = 14.179 is deeply embedded in a substantial, pristine H i gas reservoir dominating its baryonic matter content.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144370780","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

Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori 用等离子环面的质量测量来限制正在进行的火山放出气体率和太阳系外行星的内部组成

The Astrophysical Journal Letters Pub Date : 2025-06-22 DOI: 10.3847/2041-8213/adde5e

V. Abby Boehm, Darryl Z. Seligman and Nikole K. Lewis

{"title":"Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori","authors":"V. Abby Boehm, Darryl Z. Seligman and Nikole K. Lewis","doi":"10.3847/2041-8213/adde5e","DOIUrl":"https://doi.org/10.3847/2041-8213/adde5e","url":null,"abstract":"We present a novel method of constraining volcanic activity on extrasolar terrestrial worlds via characterization of circumstellar plasma tori. Our work generalizes the physics of the Io plasma torus to propose a hypothetical circumstellar plasma torus generated by exoplanetary volcanism. The quasi-steady torus mass is determined by a balance between material injection and ejection rates from volcanic activity and corotating magnetospheric convection, respectively. By estimating the Alfvén surfaces of planet-hosting stars, we calculate the torus mass-removal timescale for a number of exoplanets with properties amenable to plasma torus construction. Assuming a uniform toroidal geometry comparable to Io’s “warm” torus, we calculate quasi-steady torus masses inferable from the optical depth of atomic spectral features in torus-contaminated stellar spectra. The calculated quasi-steady masses can be used to constrain the volcanic outgassing rates of each species detected in the torus, providing quantitative estimates of bulk volcanic activity and interior composition with minimal assumptions. Such insight into the interior state of an exoplanet is otherwise accessible only after destruction via tidal forces. We demonstrate the feasibility of our method by showcasing known exoplanets that are susceptible to tidal heating and could generate readily detectable tori with realistic outgassing rates of order 1 t s−1, comparable to the Io plasma torus mass injection rate. This methodology may be applied to stellar spectra measured with ultraviolet instruments with sufficient resolution to detect atomic lines and sensitivity to recover the ultraviolet continuum of GKM dwarf stars. This further motivates the need for ultraviolet instrumentation above Earth’s atmosphere.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"243 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144370783","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

Thermonuclear Superburst of MAXI J1752−457 Observed with NinjaSat and MAXI 用NinjaSat和MAXI观测到的MAXI J1752−457热核超爆

The Astrophysical Journal Letters Pub Date : 2025-06-19 DOI: 10.3847/2041-8213/addd00

Amira Aoyama, Teruaki Enoto, Takuya Takahashi, Sota Watanabe, Tomoshi Takeda, Wataru Iwakiri, Kaede Yamasaki, Satoko Iwata, Naoyuki Ota, Arata Jujo, Toru Tamagawa, Tatehiro Mihara, Chin-Ping Hu, Akira Dohi, Nobuya Nishimura, Motoko Serino, Motoki Nakajima, Takao Kitaguchi, Yo Kato, Nobuyuki Kawai and (NinjaSat collaboration)

{"title":"Thermonuclear Superburst of MAXI J1752−457 Observed with NinjaSat and MAXI","authors":"Amira Aoyama, Teruaki Enoto, Takuya Takahashi, Sota Watanabe, Tomoshi Takeda, Wataru Iwakiri, Kaede Yamasaki, Satoko Iwata, Naoyuki Ota, Arata Jujo, Toru Tamagawa, Tatehiro Mihara, Chin-Ping Hu, Akira Dohi, Nobuya Nishimura, Motoko Serino, Motoki Nakajima, Takao Kitaguchi, Yo Kato, Nobuyuki Kawai and (NinjaSat collaboration)","doi":"10.3847/2041-8213/addd00","DOIUrl":"https://doi.org/10.3847/2041-8213/addd00","url":null,"abstract":"An uncatalogued bright X-ray transient was detected with MAXI on 2024 November 9, named MAXI J1752−457. The NinjaSat X-ray observatory promptly observed the source from November 10 to 18, while the small angular separation from the Sun hampered follow-up campaigns by other X-ray observatories. The MAXI and NinjaSat light curves in the 2–10 keV band showed first and second decaying components at the early and late phases, approximated by exponential functions with e-folding constants of 1.2 ± 0.2 and 14.9 ± 0.9 hr (1σ errors), respectively. A single blackbody model reproduces the X-ray spectrum with a softening trend of its temperature decreasing from 1.8 ± 0.1 keV to 0.59 ± 0.06 keV. Assuming the unknown source distance at 8 kpc, at which the initial X-ray luminosity roughly corresponds to the Eddington limit, the shrinking blackbody radius was estimated at 5–11 km. This X-ray brightening is interpreted as a superburst in a Galactic low-mass X-ray binary, which is powered by thermonuclear burning triggered presumably by carbon ignition close to the outer crust of the neutron star. The transition between two decaying components occurred at 5.5–7.7 hr, corresponding to the thermal timescale of the burning layer. The ignition column density is estimated to be (1.8–2.8) × 1012 g cm−2.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"237 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329230","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 Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions 帕克太阳探测器、太阳神号和Wind任务观测到的alfv<s:1>慢太阳风的温度各向异性和氦丰度特征

The Astrophysical Journal Letters Pub Date : 2025-06-19 DOI: 10.3847/2041-8213/ade0ac

Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens and Stuart D. Bale

{"title":"The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions","authors":"Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens and Stuart D. Bale","doi":"10.3847/2041-8213/ade0ac","DOIUrl":"https://doi.org/10.3847/2041-8213/ade0ac","url":null,"abstract":"Slow solar wind is typically characterized as having low Alfvénicity, but the occasional occurrence of highly Alfvénic slow solar wind (HASSW) raises questions about its source regions and evolution. In this work, we conduct a statistical analysis of temperature anisotropy and helium abundance in HASSW using data from the Parker Solar Probe (PSP) within 0.25 au, Helios between 0.3 au and 1 au, and Wind near 1 au. Our findings reveal that HASSW is prevalent close to the Sun, with PSP observations displaying a distinct “U-shaped” Alfvénicity distribution with respect to increasing solar wind speed, unlike the monotonic increase trend seen in Helios and Wind data. This highlights a previously unreported population of unusually low-speed HASSW, which is found in both sub-Alfvénic and super-Alfvénic regimes. The observed decreasing overlap in temperature anisotropy between HASSW and fast solar wind (FSW) with increasing heliocentric distance suggests different underlying heating processes. Additionally, HASSW exhibits two distinct helium abundance populations, particularly evident in PSP data, with generally higher helium abundance compared to less Alfvénic slow solar wind. Moreover, the decreasing overlap in temperature anisotropy versus helium abundance distributions between HASSW and FSW with decreasing radial distance implies that not all HASSW originates from the same source region as FSW.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"44 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329231","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

Measuring Scaling Relations: Fitting Technique Matters 测量尺度关系：拟合技术问题

The Astrophysical Journal Letters Pub Date : 2025-06-19 DOI: 10.3847/2041-8213/ade13c

Bryanne McDonough, Olivia Curtis and Tereasa G. Brainerd

{"title":"Measuring Scaling Relations: Fitting Technique Matters","authors":"Bryanne McDonough, Olivia Curtis and Tereasa G. Brainerd","doi":"10.3847/2041-8213/ade13c","DOIUrl":"https://doi.org/10.3847/2041-8213/ade13c","url":null,"abstract":"Scaling relationships, both integrated and spatially resolved, arise owing to the physical processes that govern galaxy evolution and are frequently measured in both observed and simulated data. However, the accuracy and comparability of these measurements are hindered by various differences between studies such as spatial resolution, sample selection criteria, and fitting technique. In this Letter, we compare variations of standard least-squares techniques to the ridge line method for identifying spatially resolved scaling relations (Σ*−ΣSFR, Σ*−Σgas, and Σgas−ΣSFR) for TNG100 galaxies. We find that using the ridge line technique to fit these scaling relations with a double linear function (in logarithmic space) results in significantly better fits than fitting with ordinary least squares. We further illustrate the utility of the ridge line technique with an investigation into the dependence of resolved star formation main-sequence (rSFMS) measurements on spatial resolution and smoothing scale. Specifically, we find that the slope of the rSFMS at low Σ* is independent (within 2σ) of spatial resolution and smoothing scale. Finally, we discuss the need for a consistent reanalysis of resolved scaling relations in the literature and physically motivate adoption of the ridge line technique over other fitting methods.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"19 1","pages":"L32"},"PeriodicalIF":0.0,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144335091","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 Novel Method of Modeling Extended Emission of Compact Jets: Application to Swift J1727.8−1613 一种新型紧凑型射流扩展发射建模方法：在Swift J1727.8−1613上的应用

The Astrophysical Journal Letters Pub Date : 2025-06-19 DOI: 10.3847/2041-8213/ade13b

Andrzej A. Zdziarski, Callan M. Wood and Francesco Carotenuto

{"title":"A Novel Method of Modeling Extended Emission of Compact Jets: Application to Swift J1727.8−1613","authors":"Andrzej A. Zdziarski, Callan M. Wood and Francesco Carotenuto","doi":"10.3847/2041-8213/ade13b","DOIUrl":"https://doi.org/10.3847/2041-8213/ade13b","url":null,"abstract":"Flat radio spectra of compact jets launched by both supermassive and stellar-mass black holes (BHs) are explained by an interplay of self-absorbed synchrotron emission up to some distance along the jet and optically thin synchrotron at larger distances. Their spatial structure is usually studied using core shifts, in which the position of the peak (core) of the emission depends on the frequency. Here, we propose a novel and powerful method to fit the spatial dependence of the flux density at a given frequency of the jet and counterjet (when observed), using the theoretical spatial dependencies provided as simple analytical formulae. We apply our method to the spatial structure of the jets in the luminous hard spectral state of the BH X-ray binary Swift J1727.8−1613. It was the most resolved continuous jet from an X-ray binary ever observed. We find that the observed approaching jet is significantly intrinsically stronger than the receding one, which we attribute to an increase in the emission of both jets with time (observationally confirmed), together with the light travel effect, causing the receding jet to be observed at an earlier epoch than the approaching one. The jets are relatively slow, with a velocity of ∼(0.3–0.4)c. Our findings imply that the magnetic field strength increased with time. Additionally, the magnetic flux is significantly lower than in jets launched by “magnetically arrested disks.” Our method is general, and we propose that it be applied to jets launched by both stellar-mass and supermassive BHs.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"1 1","pages":"L35"},"PeriodicalIF":0.0,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144335031","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

Three Fast-spinning Medium-sized Hilda Asteroids Uncovered by TESS TESS发现了三颗快速旋转的中型希尔达小行星

The Astrophysical Journal Letters Pub Date : 2025-06-18 DOI: 10.3847/2041-8213/ade05b

Nóra Takács, Csaba Kiss, Róbert Szakáts, Emese Plachy, Csilla E. Kalup, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, Róbert Szabó, Attila Bódi and András Pál

{"title":"Three Fast-spinning Medium-sized Hilda Asteroids Uncovered by TESS","authors":"Nóra Takács, Csaba Kiss, Róbert Szakáts, Emese Plachy, Csilla E. Kalup, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, Róbert Szabó, Attila Bódi and András Pál","doi":"10.3847/2041-8213/ade05b","DOIUrl":"https://doi.org/10.3847/2041-8213/ade05b","url":null,"abstract":"Hilda asteroids, which orbit in a 3:2 resonance with Jupiter, serve as key indicators of dynamical processes in the early solar system. Their spin rates, an important probe of these mechanisms, can constrain their density and collisional evolution, offering valuable insights into their origin. In this Letter, we report on the identification of three fast-rotating Hilda asteroids with spin periods in the 3.2–3.7 hr range using data from the Transiting Exoplanet Survey Satellite. These rotation periods are significantly shorter than the previous ∼5.0 hr shortest rotation periods obtained from ground-based observations in the ∼10 km size range and are comparable with the ∼3.0 hr breakup limit of Hildas a few kilometers in size, derived from the FOSSIL survey. These fast-rotating asteroids require either considerable cohesion (in the order of a few kPa) or densities ρ ≳1.5 g cm−3, in contrast to the typically assumed ρ ≲1 g cm−3, to prevent rotational breakup. C-type asteroids, which are common in the outer main belt, have densities of ρ ≈ 1.5 g cm−3 and are known to comprise a small but notable fraction of Hildas. The observed occurrence rate of the ≤4 hr rotation periods may be explained by the 10%–15% fraction of C-type asteroids, likely mixed into these populations from the outer main belt during giant planet dynamical interactions in the early solar system.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"45 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329362","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

Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly 重子声学振荡：非零中微子质量的2σ+探测与动态暗能量和透镜异常的更新

The Astrophysical Journal Letters Pub Date : 2025-06-18 DOI: 10.3847/2041-8213/ade1cc

Shouvik Roy Choudhury

{"title":"Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly","authors":"Shouvik Roy Choudhury","doi":"10.3847/2041-8213/ade1cc","DOIUrl":"https://doi.org/10.3847/2041-8213/ade1cc","url":null,"abstract":"We obtain constraints in a 12 parameter cosmological model using the recent Dark Energy Spectroscopic Instrument Data Release (DR) 2 Baryon Acoustic Oscillations (BAO) data, combined with cosmic microwave background (CMB) power spectra (Planck Public Release, PR, 4) and lensing (Planck PR4 + Atacama Cosmology Telescope DR 6) data, uncalibrated Type Ia supernovae (SNe) data from Pantheon+ and Dark Energy Survey (DES) Year 5 (DESY5) samples, and Weak Lensing (WL; DES Year 1) data. The cosmological model consists of six Λ cold dark matter parameters and additionally, the dynamical dark energy parameters (w0, wa), the sum of neutrino masses (∑mν), the effective number of non-photon radiation species (Neff), the scaling of the lensing amplitude (Alens), and the running of the scalar spectral index (αs). Our major findings are the following: (i) With CMB+BAO+DESY5+WL, we obtain the first 2σ+ detection of a non-zero eV (95%). Replacing DESY5 with Pantheon+ still yields a ∼1.9σ detection. (ii) The cosmological constant lies at the edge of the 95% contour with CMB+BAO+Pantheon+ but is excluded at 2σ+ with DESY5, leaving evidence for dynamical dark energy data-set dependent and inconclusive. (iii) With CMB+BAO+SNe+WL, Alens = 1 is excluded at >2σ, while it remains consistent with unity without WL data—suggesting that the existence of lensing anomaly with Planck PR4 likelihoods may depend on non-CMB data sets. (iv) The Hubble tension persists at 3.6σ–4.2σ with CMB+BAO+SNe; WL data have minimal impact.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329363","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

Modification of the Power Spectral Density of Magnetic Field Fluctuations by Quasi-perpendicular Interplanetary Shocks 准垂直行星际冲击对磁场波动功率谱密度的修正

The Astrophysical Journal Letters Pub Date : 2025-06-18 DOI: 10.3847/2041-8213/ade25b

Byeongseon Park, Alexander Pitňa, Jana Šafránková and Zdeněk Němeček

{"title":"Modification of the Power Spectral Density of Magnetic Field Fluctuations by Quasi-perpendicular Interplanetary Shocks","authors":"Byeongseon Park, Alexander Pitňa, Jana Šafránková and Zdeněk Němeček","doi":"10.3847/2041-8213/ade25b","DOIUrl":"https://doi.org/10.3847/2041-8213/ade25b","url":null,"abstract":"We investigate the role of interplanetary (IP) shocks in solar wind turbulence using observations of Solar Orbiter, Parker Solar Probe, and Wind. Employing statistical analysis of quasi-perpendicular fast forward (FF) and fast reverse (FR) shocks, we revisit evolution of magnetic field turbulence across IP shocks. Our previous work indicates that the spectral properties of magnetic fluctuations are statistically conserved across different types of IP shocks, except FR shocks in the transition range of frequencies. We focus on the spectral index in the transition range ( ) using 1 minute sliding windows at 10 s intervals to probe the turbulent dissipation near shocks. We address the influence of key turbulence parameters, particularly cross helicity (σc) and fluctuation amplitude (σB), on . Our results demonstrate (1) an immediate change in across the shock with no evidence for further gradual or asymptotic evolution over extended intervals, and this implies that shock universally serves as a thin boundary separating two turbulence states; (2) the dominant factor forming the steepness of is σc, rather than σB; and (3) the statistically shallower downstream of FR shocks results from a systematic reduction in σc across shocks. These findings suggest that the observed spectral modification is primarily governed by changes in turbulence Alfvénicity, not directly by dissipation processes related to the shock, and can be commonly observed toward extensive heliospheric distances.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"44 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329489","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