Astronomy & Astrophysics最新文献

{"title":"V4141 Sgr: Outflows and repeated outbursts","authors":"Jaroslav Merc, Joanna Mikołajewska, Thomas Petit, Berto Monard, Stéphane Charbonnel, Olivier Garde, Pascal Le Dû, Lionel Mulato, Tadashi Kojima","doi":"10.1051/0004-6361/202554734","DOIUrl":"https://doi.org/10.1051/0004-6361/202554734","url":null,"abstract":"In this work, we analyze the ongoing brightening of the poorly studied symbiotic star V4141 Sgr and examine its long-term variability. We present new low-resolution spectroscopic observations of the system in its bright state and combine them with multi-color photometric data from our observations, as well as ASAS-SN, ATLAS, and <i>Gaia<i/> DR3. To investigate its long-term evolution, we also incorporated historical data, including photographic plates, constructing a light curve spanning more than a century. Our analysis reveals that V4141 Sgr has undergone multiple outbursts, with at least one exhibiting characteristics that are typical of “slow” symbiotic novae. The current outburst is characterized by the ejection of optically thick material and possibly bipolar jets, a phenomenon observed in only a small fraction of symbiotic stars. These findings establish V4141 Sgr as an intriguing target for continued monitoring.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"167 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165111","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Enhancing MHD model accuracy and CME forecasting by constraining coronal plasma properties with Faraday rotation","authors":"Salvatore Mancuso","doi":"10.1051/0004-6361/202553738","DOIUrl":"https://doi.org/10.1051/0004-6361/202553738","url":null,"abstract":"Accurate forecasting and modeling of coronal mass ejections (CMEs) and their associated shocks are pivotal for understanding space weather and its impact on Earth. This requires a detailed understanding of CMEs’ 3D morphology and the properties of the pre-eruption coronal plasma, which are usually inferred from global 3D numerical magnetohydrodynamic (MHD) simulations. Refining MHD models is thus crucial for improving our understanding of CME-driven shocks and their effects on space weather. Faraday rotation measurements of extragalactic radio sources occulted by the solar corona serve as a powerful complementary tool for probing the pre-eruption electron density and magnetic field structure. These measurements thereby allow us to refine predictions from global MHD models. In this paper, we discuss our recent study of the morphological evolution of a CME-driven shock event that occurred on August 3, 2012. Our analysis used white-light coronagraphic observations from three different vantage points in space: the Solar and Heliospheric Observatory (SOHO) and the twin Solar Terrestrial Relations Observatory (STEREO) spacecraft A and B. Obtaining data from these spacecraft, we derived key parameters such as the radius of curvature of the driving flux rope, the shock speed, and the standoff distance from the CMEs’ leading edge. A notable feature of this event was the availability of rare Faraday rotation measurements of a group of extragalactic radio sources occulted by the solar corona, which were obtained a few hours before the eruption. These observations from the Very Large Array (VLA) radio interferometer provide independent information on the integrated product of the line-of-sight (LOS) magnetic field component and electron density. By modeling the shock standoff distance and using constraints from the Faraday rotation measurements, we achieve a high level of agreement between the fast-mode Mach number predicted by the Magnetohydrodynamic Algorithm outside a Sphere (MAS) code in its thermodynamic mode and the value deduced from the analysis of the 3D reconstruction of coronagraphic data, provided that appropriate correction factors (<i>f<i/><sub><i>b<i/><sub/>≃2.4 and <i>f<i/><sub><i>n<i/><sub/>≃0.5) are applied in advance to scale the simulated magnetic field and electron density, respectively. Our results are consistent with previous estimates and provide critical information for fine-tuning future MHD simulations.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"240 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144164765","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cyclic variability of the accretion disk in the eclipsing binary OGLE-LMC-DPV-065","authors":"R. E. Mennickent, G. Djurašević","doi":"10.1051/0004-6361/202452959","DOIUrl":"https://doi.org/10.1051/0004-6361/202452959","url":null,"abstract":"<i>Context.<i/> The long photometric cycle observed in Algol OGLE-LMC-DPV-065 (OGLE05200407-6936391), and other similar systems, still challenges explanation. It is currently thought that a variable mass transfer rate could modify the structure of the accretion disk surrounding the more massive star, producing modulations of the global system brightness.<i>Aims.<i/> We revisited <i>I<i/>-band Optical Gravitational Lensing Experiment (OGLE) photometric time series spanning 20 years, with the aim of detecting and analyzing possible changes in the accretion disk properties, namely, radial and vertical extension and also temperature, and explored the existence of shock regions.<i>Methods.<i/> We solved the inverse problem yielding the best configuration of stellar and disk parameters for explaining the variability of the light curve on the orbital as well as the long-cycle timescales. A simple model allowed us to estimate the relative mass transfer rate, and the disk parameters were analyzed to evaluate their dependence and variability.<i>Results.<i/> We find that changes in the accretion disk properties reproduce the light curve variability patterns observed on the orbital and long-term cycle timescales. The mass transfer rate is highest and the disk thickness minimum at the maximum of the long-term cycle. The large vertical thicknesses suggest motions at scales beyond the classic scale height dominating the disk vertical structure while the disk almost always remains within the tidal radius.<i>Conclusions.<i/> We conclude that the long-term cycle can be explained by a variable disk and that the mass transfer rate plays a fundamental role in establishing these changes.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"34 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165210","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Study of the 2024 major Vela glitch at the Argentine Institute of Radioastronomy","authors":"Ezequiel Zubieta, Ryan Missel, Susana B. Araujo Furlan, Carlos O. Lousto, Federico García, Santiago del Palacio, Guillermo Gancio, Jorge A. Combi, Linwei Wang","doi":"10.1051/0004-6361/202554098","DOIUrl":"https://doi.org/10.1051/0004-6361/202554098","url":null,"abstract":"<i>Context.<i/> We report here on new results of the systematic monitoring of southern glitching pulsars at the Argentine Institute of Radioastronomy. In particular, we study in this work the new major glitch in the Vela pulsar (PSR J0835−4510) that occurred on 2024 April 29.<i>Aims.<i/> We aim to thoroughly characterise the rotational behaviour of the Vela pulsar around its last major glitch and investigate the statistical properties of its individual pulses around the glitch.<i>Methods.<i/> We characterise the rotational behaviour of the pulsar around the glitch through the pulsar timing technique. We measured the glitch parameters by fitting timing residuals to the data collected during the days surrounding the event. In addition, we study Vela individual pulses during the days of observation just before and after the glitch. We selected nine days of observations around the major glitch on 2024 April 29 and studied their statistical properties with the Self-Organizing Maps (SOM) technique. We used Variational AutoEncoder (VAE) reconstruction of the individual pulses to separate them clearly from the noise.<i>Results.<i/> We obtain a precise timing solution for the glitch. We find two recovery terms of ∼3 days and ∼17 days. We find a correlation of high amplitude with narrower pulses while not finding notable qualitative systematic changes before and after the glitch.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"7 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165104","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"viper: High-precision radial velocities from the optical to the infrared","authors":"J. Köhler, M. Zechmeister, A. Hatzes, S. Chamarthi, E. Nagel, U. Seemann, P. Ballester, P. Bristow, P. Chaturvedi, R. J. Dorn, E. Guenther, V. D. Ivanov, Y. Jung, O. Kochukhov, T. Marquart, L. Nortmann, R. Palsa, N. Piskunov, A. Reiners, F. Rodler, J. V. Smoker","doi":"10.1051/0004-6361/202553919","DOIUrl":"https://doi.org/10.1051/0004-6361/202553919","url":null,"abstract":"<i>Context<i/>. High-precision radial velocity (RV) measurements with slit spectrographs require the instrument profile (IP) and Earth’s atmospheric spectrum to be known and to be incorporated into the RV calculation.<i>Aims<i/>. We developed an RV pipeline, called Velocity and IP EstimatoR (viper), to achieve high-precision RVs in the near-infrared (NIR). The code is able to process observations taken with a gas cell and includes modelling of the IP and telluric lines.<i>Methods<i/>. We utilised least-square fitting and telluric forward modelling to account for instrument instabilities and atmospheric absorption lines. As part of this process, we demonstrate the creation of telluric-free stellar spectra.<i>Results<i/>. By applying viper to observations obtained with the upgraded CRyogenic high-resolution InfraRed Echelle Spectrograph (CRIRES<sup>+<sup/>) and a gas absorption cell in the <i>K<i/> band, we are able to reach an RV precision of around 3 m/s over a time span of 2.5 years. For observations using telluric lines for the wavelength reference, an RV precision of 10 m/s is achieved.<i>Conclusions<i/>. We demonstrate that despite telluric contamination, a high RV precision is possible at NIR wavelengths, even for a slit spectrograph with varying IP. Furthermore, we show that CRIRES<sup>+<sup/> performs well and is an excellent choice for science studies requiring precise stellar RV measurements in the infrared.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"479 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144153635","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Formation and nature of “Huntsman” binary pulsars","authors":"O. G. Benvenuto, M. A. De Vito, M. Echeveste, M. L. Novarino, N. D. Pires, L. M. de Sá, J. E. Horvath","doi":"10.1051/0004-6361/202554549","DOIUrl":"https://doi.org/10.1051/0004-6361/202554549","url":null,"abstract":"<i>Context.<i/> “Spider” systems are a class of close binaries in which a neutron star first accretes from a normal companion, and later ablates it in some cases. New observations have expanded this category, with the addition of a “Huntsman” group, tentatively linked to a short donor phase along the red bump along the secondary evolutionary track.<i>Aims.<i/> We present here explicit evolutionary tracks that support the Huntsman nature recently suggested, and also discuss how the whole class of spiders emerge from the full consideration of irradiation and ablating winds. We address the irradiation feedback (IFB) effects and the hydrogen-shell burning detachment (HSBD) simultaneously, and show that they act independently and do not interfere with each other, supporting a physical picture of the Huntsman group.<i>Methods.<i/> We employed our binary evolution code to compute a suite of binary systems formed by a donor star together with a neutron star for different initial orbital periods, for the case of solar composition and also for <i>Z<i/> = 10<sup>−3<sup/>. Although many models do not consider IFB, we also present the evolution with IFB for one system as an example.<i>Results.<i/> We found that the recently suggested association of Huntsman pulsar with the evolutionary stage where (as consequence of the dynamics of HSBD) the system remains detached for a few million years is truly plausible. However, this feature alone is unable to account for the occurrence of the Redback spider pulsars. Meanwhile, models including IFB, with pulsed mass transfer, display detachment episodes that can be naturally associated with the Redback stage. Irradiation feedback does not preclude or modify HSBD and in fact, the latter were implicit in our earlier calculations, but not addressed explicitly. That is, Huntsman systems were already present as an “implicit prediction” in these former works.<i>Conclusions.<i/> We conclude that Huntsman is an expected stage of these spider systems under quite general conditions. This is another step towards a unified picture of spider pulsars as a group.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"16 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144153623","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Gravitational instability and spatial regularity of the gas clouds and young stellar population in spiral arms of NGC 628","authors":"V. S. Kostiuk, A. S. Gusev, A. A. Marchuk, E. V. Shimanovskaya","doi":"10.1051/0004-6361/202554886","DOIUrl":"https://doi.org/10.1051/0004-6361/202554886","url":null,"abstract":"<i>Context.<i/> There is a clear contradiction between the characteristic spacings in observed regular chains of star-forming regions in the spiral arms of galaxies (∼500 pc) and the estimates of the wavelength of gravitational instability in them (> 1 kpc).<i>Aims.<i/> We aim to calculate the scales of regularity in the grand-design galaxy NGC 628 in terms of gravitational instability by using modern high-quality observational data and comparing them with scales of spatial regularity of the star-forming regions and molecular clouds in the spiral arms of the galaxy.<i>Methods.<i/> We investigated two mechanisms of gravitational instability against radial and azimuthal perturbations in a multicomponent disk with a finite thickness. We obtained a map of the instability wavelength distribution and compared its median value with the typical scale of observed regularity.<i>Results.<i/> The maps of instability parameters <i>Q<i/> and <i>S<i/>, which are related to the radial and azimuthal perturbations, respectively, show a good alignment between gravitationally unstable regions and areas of recent star formation. By analyzing the distribution of giant molecular clouds along the spiral arms of NGC 628, we found a similar regularity of about 500−600 pc that had previously been observed for star-forming regions. Additionally, the distribution of the wavelength most unstable to azimuthal perturbations yields a median value of about 700 pc, which is close to the observed scale regularity. This latter finding helps resolve the discrepancy between theoretically predicted and observed scales of star-forming regions in terms of regularity.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"58 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144153637","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Feasibility of interferometric observations and characterization of planet-induced structures at sub au to au scales in protoplanetary disks","authors":"L. Hildebrandt, A. Krieger, H. Klahr, J. Kobus, A. Bensberg, S. Wolf","doi":"10.1051/0004-6361/202452153","DOIUrl":"https://doi.org/10.1051/0004-6361/202452153","url":null,"abstract":"<i>Context<i/>. Interferometric observations of protoplanetary disks by VLTI and ALMA have greatly improved our understanding of the detailed structure of these planetary birthplaces. These observations have revealed a variety of large-scale disk substructures, including rings, gaps, and spirals, spanning tens to hundreds of au, supporting the predictions of planet formation models. Recent instruments, such as MATISSE at the VLTI, allow one to resolve and investigate the inner few au of protoplanetary disks in nearby star formation regions, shedding light on the traces of planet formation and evolution at these small scales.<i>Aims<i/>. The aim of this work is to assess the feasibility of interferometric observations of small-scale planet-induced substructures in protoplanetary disks in nearby star-forming regions. We aim to characterize these substructures in multi-wavelength and multi-epoch observations and subsequently differentiate between simulation parameters.<i>Methods<i/>. On the basis of 3D hydrodynamic simulations of embedded planetary companions and subsequent 3D Monte Carlo radiative transfer simulations, we calculated and analyzed interferometric observables, assuming observations with the VLTI in the K, L, M, and N bands.<i>Results<i/>. The hydrodynamic simulations exhibit mass-dependent planet-induced density waves that create observable substructures, most notably for the considered case of a 300 M<sub>⊕<sub/> planet. These substructures share similarities with observed large-scale structures and feature a prominent accretion region around the embedded planet. The visibilities show a detectable variability for multi-epoch VLTI/GRAVITY and VLTI/MATISSE observations, caused by the orbital motion of the planet, that are distinguishable from other sources of variability due to their unique combination of timescale and amplitude. Additionally, the non-uniform change of the visibilities at different baselines can be used to identify asymmetric structures. Furthermore, we show that multi-wavelength observations provide an approach to identify the fainter substructures and the signal of the accretion region.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"4 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144153638","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Revisiting the energy distribution and formation rate of CHIME fast radio bursts","authors":"K. J. Zhang, Z. B. Zhang, A. E. Rodin, V. A. Fedorova, Y. F. Huang, D. Li, X. F. Dong, P. Wang, Q. M. Li, C. Du, F. Xu, C. T. Hao","doi":"10.1051/0004-6361/202450727","DOIUrl":"https://doi.org/10.1051/0004-6361/202450727","url":null,"abstract":"Based on the first CHIME/FRB catalogue, three volume-limited samples of fast radio bursts (FRBs) are built, with samples 1, 2, and 3 corresponding to a fluence cut of 5, 3, and 1, respectively. The Lynden-Bell’s c<sup>−<sup/> method was applied to study their energy function and event rate evolution with redshift (<i>z<i/>). Using the non-parametric Kendall’s <i>τ<i/> statistics, it is found that the FRB energy (<i>E<i/>) strongly evolves with redshift as <i>E<i/>(<i>z<i/>)∝(1 + <i>z<i/>)<sup>1.24<sup/> for sample 1, <i>E<i/>(<i>z<i/>)∝(1 + <i>z<i/>)<sup>0.98<sup/> for sample 2, and <i>E<i/>(<i>z<i/>)∝(1 + <i>z<i/>)<sup>1.99<sup/> for sample 3. After removing the redshift dependence, the local energy distributions of the three samples can be well described by a broken power-law form with a broken energy of ∼10<sup>40<sup/> erg. Meanwhile, the redshift distributions of samples 1 and 2 are identical but different from that of sample 3. Interestingly, we find that the event rates of samples 1 and 2 are independent of redshift, and sample 3 decreases as a single power-law form with an index of −2.41. The local event rates of the three samples of CHIME FRBs are found to be consistently close to ∼10<sup>4<sup/> Gpc<sup>−3<sup/> yr<sup>−1<sup/>, which is comparable with some previous estimates. In addition, we notice that the event rate of sample 3 FRBs with lower energies not only exceeds the star formation rate at the lower redshifts but also always declines with the increase in redshift. We suggest that the excess of FRB rates compared with the star formation rate at low redshift mainly results from the low-energy FRBs that could originate in the older stellar populations.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"63 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144137248","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Dust-void evolution driven by turbulent dust flux can induce runaway migration of Earth-mass planets","authors":"R. O. Chametla, O. Chrenko, F. S. Masset, G. D’Angelo, D. Nesvorný","doi":"10.1051/0004-6361/202451869","DOIUrl":"https://doi.org/10.1051/0004-6361/202451869","url":null,"abstract":"Torques from asymmetric dust structures (so-called dust-void and filamentary structures) formed around low-mass planets embedded in a nonturbulent dust-gas disk can exceed the torques produced by the gas disk component and then go on to dominate the planet’s orbital dynamics. Here, we investigate how these structures (hence the dust torque) change when the effect of turbulent dust diffusion and dust feedback are included, along with the direct implications on the migration of Earth-like planets. Using the FARGO3D code, we performed 2D and 3D multifluid hydrodynamic simulations, focusing on a non-migrating planet with a mass of <i>M<sub>p<sub/><i/> = 1.5 <i>M<i/><sub>⊕<sub/> in 2D and on migrating planets with <i>M<sub>p<sub/><i/> ∈ [1.5, 12] <i>M<i/><sub>⊕<sub/> in 3D. We varied the <i>δ<i/>-dimensionless diffusivity parameter in the range [0, 3 × 10<sup>−3<sup/>] and considered three different Stokes numbers, St = {0.04, 0.26, 0.55}, which are representative of the gas-dominated, the transitional, and the gravity-dominated regimes, respectively. In our 2D models, we find that turbulent diffusion of dust prevents the formation of the dust-void and filamentary structures when <i>δ<i/> > 3 × 10<sup>−4<sup/>. Otherwise, dust structures survive turbulent diffusion flow. However, dust and total torques become positive only in transitional and gravity-dominated regimes. In our 3D models, we find that the dust-void is drastically modified and the high-density ring-shaped barrier delineating the dust-void disappears if <i>δ<i/> ≳ 10<sup>−4<sup/>, due to the effect of dust turbulent diffusion along with the back-reaction of the dust. For all values of <i>δ<i/>, the filament in front of the planet is replaced by a low-density trench. Remarkably, as we have allowed the planets to migrate, the evolving dust-void can drive either runaway migration or outward (inward) oscillatory-torque migration. Our study thus suggests that low-mass Earth-like planets can undergo runaway migration in dusty disks.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"16 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144137222","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}