The Astrophysical Journal最新文献_第10页

Simulations of Galactic Outflows Driven by Active Galactic Nuclei and Starbursts 由活动星系核和星暴驱动的星系外流模拟

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/ae00c4

Ryan Tanner, Kimberly A. Weaver and Anna Ogorzałek

{"title":"Simulations of Galactic Outflows Driven by Active Galactic Nuclei and Starbursts","authors":"Ryan Tanner, Kimberly A. Weaver and Anna Ogorzałek","doi":"10.3847/1538-4357/ae00c4","DOIUrl":"https://doi.org/10.3847/1538-4357/ae00c4","url":null,"abstract":"Using the hydro code Athena++, we run a series of large-scale hydrodynamic simulations of galactic outflows on a scale of ∼5 kpc scale over a time period of 5 Myr. We compare the kinematics, composition, and simulated X-ray emission of starburst (SB) versus active galactic nuclei (AGN) dominated galactic outflows. Our set of simulations includes galactic outflows driven solely by a nuclear SB, an AGN wind, and a mixture of SBs and AGN winds. We find significant differences in the kinematics, composition, and simulated X-ray emission between SB- versus AGN-dominated outflows. Starburst-driven outflows are characterized by turbulent, multiphase, complex flows, with each phase having a distinct kinematic profile (as traced by various oxygen ions), while AGN-driven outflows are more symmetric, more single phase, with primarily very hot (>107 K) gas, and are smooth in appearance. In mixed SB-AGN simulations, the dominant component (SB or AGN) determines the outflow characteristics. In cases where the energy input of the SB is similar to the energy of the AGN, the resulting outflow appears similar to the SB-only outflow, but when the energy input from the AGN wind is much greater than the SB then the outflow appears similar to the AGN-only outflow. When we generate synthetic X-ray observations, the AGN-dominated outflows are essentially invisible in soft to medium-energy X-rays (0.1–10.0 keV), but the SB-driven outflows show complex filamentary structures that are visible in the X-ray. Finally, we show the observational possibilities for various proposed and future X-ray telescopes.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"21 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145241250","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 HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies HST遗留档案局部群成像均匀还原（LAURELIN）。36个超暗矮星系的光度测定和恒星形成历史

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/ae00c8

Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel and Benjamin F. Williams

{"title":"The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies","authors":"Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel and Benjamin F. Williams","doi":"10.3847/1538-4357/ae00c8","DOIUrl":"https://doi.org/10.3847/1538-4357/ae00c8","url":null,"abstract":"We present uniformly measured resolved stellar photometry and star formation histories (SFHs) for 36 nearby (≲400 kpc) ultra-faint dwarf galaxies (UFDs; −7.1 ≤ MV ≤ +0.0) from new and archival Hubble Space Telescope (HST) imaging. We measure homogeneous distances to all systems via isochrone fitting and find good agreement (≤2%) for the 18 UFDs that have literature RR Lyrae distances. From the ensemble of SFHs, we find (i) an average quenching time (here defined as the lookback time by which 80% of the stellar mass formed, τ80) of 12.48 ± 0.18 Gyr ago ( ), which is compatible with reionization-based quenching scenarios; and (ii) modest evidence of a delay (≲800 Myr) in quenching times of UFDs thought to be satellites of the LMC or on their first infall, relative to long-term Galactic satellites, which is consistent with previous findings. We show that robust SFH measurement via the ancient main-sequence turnoff (MSTO) requires a minimum effective luminosity (i.e., luminosity within the observed field of view) of MV ≤ −2.5, which corresponds to ∼100 stars around the MSTO. We also find that increasing the signal-to-noise ratio above ∼100 at the MSTO does not improve SFH precision, which remains dominated by stochastic effects associated with the number of available stars. A main challenge driving the precision of UFD SFHs is the limitations in the accuracy of foreground dust maps. We make all photometry catalogs public as the first data release of a larger HST archival program targeting all dwarf galaxies within ∼1.3 Mpc.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"34 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145241251","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 Farside Magnetic Structures in Modeling the 2024 Solar Eclipse 月球背面磁结构在模拟2024年日食中的作用

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/ae0323

Guanglu Shi, Jiahui Shan, Li Feng, Jun Chen and Weiqun Gan

{"title":"The Role of Farside Magnetic Structures in Modeling the 2024 Solar Eclipse","authors":"Guanglu Shi, Jiahui Shan, Li Feng, Jun Chen and Weiqun Gan","doi":"10.3847/1538-4357/ae0323","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0323","url":null,"abstract":"The corona is a crucial region that connects the solar surface to the solar wind and serves as the primary site of solar activity. The 2024 total solar eclipse (TSE) provides a unique opportunity to investigate the large-scale coronal structure. Combined with TSE observations, we study the impact of the magnetic structure of the farside active region, located in the eastern hemisphere of the Sun that has not yet rotated into the Earth field of view, on a global magnetohydrodynamic simulation. To address the limitation of single-view measurements for the routine synoptic map, we correct the magnetic field in the farside region by incorporating full-disk magnetograms measured several days after the TSE, allowing us to capture the temporal evolution of the photospheric magnetic field in near real time. Simulation results demonstrate that the local magnetic field in the farside active region can significantly influence the global coronal structure, by altering the position of the heliospheric current sheet, and further affect the global distribution of plasma parameters, even in polar regions. A comparison of the simulation results with white-light TSE + Large Angle and Spectrometric Coronagraph C2 observations and in situ measurements by the Parker Solar Probe reveals that the composite synoptic map improves the accuracy of the coronal modeling. This work provides robust support for advancing our understanding of coronal evolution, as well as deepening the link between the photosphere and large-scale coronal structure. Furthermore, it establishes a theoretical foundation for the future development of multiview stereoscopic measurements of the photospheric magnetic field.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"80 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145241253","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 the Nature of Periodic Amplitude Modulation in Pulsars 脉冲星周期调幅特性的表征

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/ae03c1

Rahul Basu, Dipanjan Mitra and George I. Melikidze

{"title":"Characterizing the Nature of Periodic Amplitude Modulation in Pulsars","authors":"Rahul Basu, Dipanjan Mitra and George I. Melikidze","doi":"10.3847/1538-4357/ae03c1","DOIUrl":"https://doi.org/10.3847/1538-4357/ae03c1","url":null,"abstract":"In recent years, periodic amplitude modulation has emerged as a unique emission feature in the single-pulse sequence of pulsars alongside periodic nulling and subpulse drifting. Despite ample evidence for the uniqueness of this phenomenon, the periodic modulation in several pulsars are often confused with subpulse drifting, primarily due to lack of clear characterization of the emission features from a representative sample of pulsars. In this work, we present a detailed analysis of the single-pulse behavior from 17 pulsars exhibiting periodic amplitude modulation, 6 of them being new detections. The pulsar switches between different intensity states as a result of periodic amplitude modulation, and we propose a novel statistical scheme to identify these emission states. The periodic modulation can be divided into three broad categories: phase stationary modulation, modulations with phase shift, and intermittent periodic modulations. The phase stationary behavior is seen when the emission intensity across a major part of the pulse window changes periodically. The phase shifts are associated with intensity changes at specific locations within the emission window in a periodic manner, while in some pulsars, the periodic modulations become more prominent only at specific intervals resulting in intermittent behavior.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"24 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145241254","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

Betelgeuse’s Buddy: X-Ray Constraints on the Nature of α Ori B 参宿四的伙伴：α座星B性质的x射线约束

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/adff83

Anna J. G. O’Grady, Brendan O’Connor, Jared A. Goldberg, Meridith Joyce, László Molnár, Christian I. Johnson, Jeremy Hare, Katelyn Breivik, Maria R. Drout, Maxwell Moe and Annalisa Calamida

{"title":"Betelgeuse’s Buddy: X-Ray Constraints on the Nature of α Ori B","authors":"Anna J. G. O’Grady, Brendan O’Connor, Jared A. Goldberg, Meridith Joyce, László Molnár, Christian I. Johnson, Jeremy Hare, Katelyn Breivik, Maria R. Drout, Maxwell Moe and Annalisa Calamida","doi":"10.3847/1538-4357/adff83","DOIUrl":"https://doi.org/10.3847/1538-4357/adff83","url":null,"abstract":"The ∼2100 daylong secondary period of Betelgeuse’s optical lightcurve and radial velocity motivated the prediction of a low-mass stellar companion, expected to be at maximal apparent separation from Betelgeuse around 2024 December. We carried out Director’s Discretionary Time observations with the Chandra X-ray Observatory to identify any X-ray emission from the companion and constrain its nature as either a compact object or young stellar object (YSO). Past X-ray observations occurred at the wrong phase of the companion’s orbit for optimal detection prospects and/or lacked the deep exposure required to constrain the typical X-ray luminosities of YSOs. In our 41.85 ks exposure with Chandra, we do not detect an X-ray source at the position of Betelgeuse. For an estimated hydrogen column density NH = 6 × 1022 cm−2, we place a limit on the X-ray luminosity LX ≲ 2 × 1030 erg s−1 (≲4.7 × 10−4 L⊙) in 0.5–8 keV for a 10 MK plasma temperature spectral model, or LX ≲ 5 × 1029 erg s−1 (≲1.2 × 10−4 L⊙) for an absorbed power law with photon index Γ = 2. These limits robustly exclude an accreting compact object (white dwarf or neutron star) as the companion. Solar-mass YSOs with an age similar to Betelgeuse (∼10 Myr) display a range of X-ray luminosities (1028−32 erg s−1), and we can place upper bounds within this range for most absorbing columns. Based on these considerations, we conclude that the companion to Betelgeuse is likely a low-mass YSO.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145241219","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

ALMA Observations of CO in Five Planetary Nebulae: Insights into Nebular Shaping ALMA对五个行星状星云中CO的观测：对星云形成的洞察

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/ae0037

D. R. Schmidt, K. R. Gold, H. Liszt and L. M. Ziurys

{"title":"ALMA Observations of CO in Five Planetary Nebulae: Insights into Nebular Shaping","authors":"D. R. Schmidt, K. R. Gold, H. Liszt and L. M. Ziurys","doi":"10.3847/1538-4357/ae0037","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0037","url":null,"abstract":"The J = 2→1 transition of CO near 230 GHz has been imaged in five bipolar/multipolar planetary nebulae (K3-45, K3-58, M1-7, M2-48, and M3-28) using ALMA with 1″ angular resolution. Single-dish data from the Arizona Radio Observatory Submillimeter Telescope (ARO SMT) were added to provide sensitivity on spatial scales up to 30″—essential for these data. The images show that the molecular gas resides primarily in the central regions of the nebulae and not in the bipolar flows of the optical images. CO appears to trace the remnant asymptotic giant branch (AGB) wind (Vexp ∼ 12–14 km s−1) but has a higher velocity component (V > 16–23 km s−1) that represents gas swept up in the outflows. The orientations, with respect to the plane of the sky, of the bipolar outflows are 45° ± 5, 65° ± 10, and 65° ± 5 for K3–45, K3-58, and M1-7, respectively, with the blueshifted lobes oriented to the NE, W, and NW. For M2-48 and M3-28, the flows lie in the plane of the sky, with the blueshifted lobes roughly lying E and N. Based on CO, velocities in the bipolar flows are estimated to be Voutflow > 18–31 km s−1. Revised CO column densities are consistent with past measurements, except for M2-48, where the value increased to Ntot ∼ cm−2; a value was also obtained for the first time for K3-58 (Ntot ∼ 5 × 1016 cm−2). Given the unusual 12C/13C ratios observed in two sources, the bipolar ejection may have an origin in runaway He-burning in the late AGB phase.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"10 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145241220","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

Mass Loss and Subsequent Thermal Evolution of Surviving Helium White Dwarfs Shocked by Thermonuclear Supernovae 受热核超新星冲击的幸存氦白矮星的质量损失和随后的热演化

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/adfcd7

Tin Long Sunny Wong and Lars Bildsten

{"title":"Mass Loss and Subsequent Thermal Evolution of Surviving Helium White Dwarfs Shocked by Thermonuclear Supernovae","authors":"Tin Long Sunny Wong and Lars Bildsten","doi":"10.3847/1538-4357/adfcd7","DOIUrl":"https://doi.org/10.3847/1538-4357/adfcd7","url":null,"abstract":"Following a Type Ia supernova (SN Ia) in a double white dwarf (WD) binary, a surviving WD companion leaves at its orbital velocity ≈ 1000–3000 km s–1. The Gaia mission has discovered seven such hypervelocity WDs with inflated radii indicative of shock heating by SN ejecta. We study the interaction between SN ejecta and Roche lobe filling, 0.08–0.45 M⊙ helium WD companions using 3D hydrodynamical simulations with Athena++. Given the importance of the later thermal evolution, we include an accurate equation of state for the degenerate helium WD donor. We show that a lower-mass, larger-radius WD companion is more strongly impacted by SN ejecta and undergoes substantial mass loss. We find a tight relation between the fractional mass loss and the ratio between the ejecta ram pressure and donor volume-averaged pressure, which can be used for predicting mass loss in other systems. In the most extreme case, the companion becomes a very inflated ≈0.02 M⊙ object. We find helium mass loss ≈ 0.005−0.06 M⊙ with velocities ≈ 1000−4000 km s−1, which may lead to emission lines in the nebular phase. The surviving helium WD receives a kick velocity, but its final velocity is essentially determined by its orbital velocity, ≲1600 km s−1. We model the postexplosion evolution of the shock-heated companions using MESA, and find reasonable agreement with the hypervelocity stars D6-2, J0546+0836, J1332–3541, and SDSS J1637+3631. A surviving ≳0.3 M⊙ helium WD can be ruled out in SN 1972E and SN 2011fe, and any surviving helium WD is likely ruled out in SN remnants 0509-67.5 and SN 1006.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"53 62 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145241214","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

Predicting Solar Magnetic Activity from S ph and Seismic Parameters Using Random Forest Regression 利用随机森林回归从S - ph和地震参数预测太阳磁活动

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/adfe6a

Ki-Beom Kim and Heon-Young Chang

引用次数: 0

How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation 尘埃模型如何塑造高z星系形态：来自新星团模拟的见解

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/adfed9

Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero and Sukyoung K. Yi

{"title":"How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation","authors":"Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero and Sukyoung K. Yi","doi":"10.3847/1538-4357/adfed9","DOIUrl":"https://doi.org/10.3847/1538-4357/adfed9","url":null,"abstract":"Dust plays a pivotal role in shaping the observed morphology of galaxies. While traditional cosmological simulations often assume a fixed dust-to-gas or dust-to-metal (DTM) mass ratio to model dust effects, recent advancements have enabled on-the-fly (OTF) dust modeling that captures the spatial and temporal evolution of dust. In this work, we investigate the impact of dust modeling on galaxy morphology using the NewCluster simulation, which implements a detailed OTF dust model. We generate mock images of NewCluster galaxies under both OTF and fixed DTM models using the radiative transfer code SKIRT, and compare their morphology to JWST observations. We measure morphology indices and use the G–M20 test to classify galaxies. We find that the OTF galaxy models exhibit brighter centers and more pronounced bulges than those of the fixed DTM models, resulting in a lower late-type galaxy fraction, particularly at high redshifts. This central brightening is linked to a phenomenon we refer to as the DTM cavity, a localized depression in the DTM ratio driven by intense bulge starbursts. Our results highlight the importance of modeling dust evolution in a physically motivated manner, as fixed DTM models fail to capture key morphological features.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"49 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145241217","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

On the Stability Analysis of Astrophysical Cooling Functions 天体物理冷却函数的稳定性分析

The Astrophysical Journal Pub Date : 2025-10-07 DOI: 10.3847/1538-4357/adf960

Amanda Stricklan, Tim Waters and James Klimchuk

{"title":"On the Stability Analysis of Astrophysical Cooling Functions","authors":"Amanda Stricklan, Tim Waters and James Klimchuk","doi":"10.3847/1538-4357/adf960","DOIUrl":"https://doi.org/10.3847/1538-4357/adf960","url":null,"abstract":"To model the temperature evolution of optically thin astrophysical environments at MHD scales, radiative and collisional cooling rates are typically either pretabulated or fit into a functional form and then input into MHD codes as a radiative loss function. Thermal balance requires estimates of the analogous heating rates, which are harder to calculate, and due to uncertainties in the underlying dissipative heating processes these rates are often simply parameterized. The resulting net cooling function defines an equilibrium curve that varies with density and temperature. Such cooling functions can make the gas prone to thermal instability (TI), which will cause departures from equilibrium. There has been no systematic study of thermally unstable parameter space for nonequilibrium states. Motivated by our recent finding that there is a related linear instability, catastrophic cooling instability, that can dominate over TI, here we carry out such a study. We show that Balbus instability criteria for TI can be used to define a critical cooling rate, Λc, that permits a nonequilibrium analysis of cooling functions through the mapping of TI zones. We furthermore illustrate how thermal conduction modifies the shape of TI zones. Upon applying a Λc-based stability analysis to coronal loop simulations, we find that loops undergoing periodic episodes of coronal rain formation are linearly unstable to catastrophic cooling instability, while TI is stabilized by thermal conduction.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"86 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246739","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