Astronomy & Astrophysics最新文献

{"title":"Machine learning the gap between real and simulated nebulae","authors":"Francesco Belfiore, Michele Ginolfi, Guillermo Blanc, Mederic Boquien, Melanie Chevance, Enrico Congiu, Simon C. O. Glover, Brent Groves, Ralf S. Klessen, J. Eduardo Méndez-Delgado, Thomas G. Williams","doi":"10.1051/0004-6361/202451934","DOIUrl":"https://doi.org/10.1051/0004-6361/202451934","url":null,"abstract":"Classifying ionised nebulae in nearby galaxies is crucial to studying stellar feedback mechanisms and understanding the physical conditions of the interstellar medium. This classification task is generally performed by comparing observed line ratios with photoionisation simulations of different types of nebulae (H II regions, planetary nebulae, and supernova remnants). However, due to simplifying assumptions, such simulations are generally unable to fully reproduce the line ratios in observed nebulae. This discrepancy limits the performance of the classical machine-learning approach, where a model is trained on the simulated data and then used to classify real nebulae. For this study, we used a domain-adversarial neural network (DANN) to bridge the gap between photoionisation models (source domain) and observed ionised nebulae from the PHANGS-MUSE survey (target domain). The DANN is an example of a domain-adaptation algorithm, whose goal is to maximise the performance of a model trained on labelled data in the source domain on an unlabelled target domain by extracting domain-invariant features. Our results indicate a significant improvement in classification performance in the target domain when employing the DANN framework compared to a classical neural network (NN) classifier. Additionally, we investigated the impact of adding noise to the source dataset, finding that noise injection acts as a form of regularisation, further enhancing the performances of both the NN and DANN models on the observational data. The combined use of domain adaptation and noise injection improved the classification accuracy in the target domain by 23%. This study highlights the potential of domain adaptation methods in tackling the domain-shift challenge when using theoretical models to train machine-learning pipelines in astronomy.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"5 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143427463","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":"GJ 2126 b: A highly eccentric Jovian exoplanet","authors":"A. Schorr, A. Binnenfeld, S. Zucker","doi":"10.1051/0004-6361/202452563","DOIUrl":"https://doi.org/10.1051/0004-6361/202452563","url":null,"abstract":"We report the discovery of GJ 2126 b, a highly eccentric (<i>e<i/> = 0.85) Jupiter-like planet orbiting its host star every 272.7 days. The planet was detected and characterized using 112 radial velocity (RV) measurements from HARPS (High Accuracy Radial velocity Planet Searcher), provided by HARPS-RVBank. This planet orbits a low-mass star and ranks among the most eccentric exoplanets discovered, placing it in a unique region of the parameter space of the known exoplanet population. This makes it a valuable addition to the exoplanet demographics, helping to refine our understanding of planetary formation and evolution theories.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"64 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143427414","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":"Possible contributions of two nearby blazars to the NGC 4151 neutrino hotspot","authors":"A. Omeliukh, S. Barnier, Y. Inoue","doi":"10.1051/0004-6361/202452992","DOIUrl":"https://doi.org/10.1051/0004-6361/202452992","url":null,"abstract":"<i>Context.<i/> The origin of the high-energy astrophysical neutrinos discovered by IceCube remains unclear, with both blazars and Seyfert galaxies emerging as potential sources. Recently, the IceCube Collaboration reported a ∼3<i>σ<i/> neutrino signal from the direction of the nearby Seyfert galaxy NGC 4151. However, two gamma-ray-loud BL Lac objects, 4FGL 1210.3+3928 and 4FGL J1211.6+3901, lie close to NGC 4151, at angular distances of 0.08° and 0.43°, respectively.<i>Aims.<i/> We investigated the potential contribution of these two blazars to the observed neutrino signal from the direction of NGC 4151 and assessed their detectability with future neutrino observatories.<i>Methods.<i/> We modeled the multiwavelength spectral energy distributions (SEDs) of both blazars using a self-consistent numerical radiation code, AM<sup>3<sup/>. We calculated their neutrino spectra and compared them to the measured NGC 4151 neutrino spectrum and future neutrino detector sensitivities.<i>Results.<i/> The SED of 4FGL 1210.3+3928 revealed a feature that cannot be explained with a purely leptonic model, suggesting the presence of protons in the jet. Our model predicts neutrino emission peaking above ∼10<sup>17<sup/> eV with fluxes of ∼10<sup>−12<sup/> erg cm<sup>−2<sup/> s<sup>−1<sup/> for this source. The SED of 4FGL J1211.6+3901 can be explained with both leptonic and leptohadronic models. The contribution of these two blazars to the ∼10 TeV neutrino signal observed from the direction of NGC 4151 can only be minor. Still, future radio-based neutrino telescopes such as IceCube-Gen2’s radio array and GRAND may be able to detect high-energy neutrinos from these two potential neutrino sources.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"64 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143427444","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":"Detecting clusters and groups of galaxies populating the local Universe in large optical spectroscopic surveys","authors":"I. Marini, P. Popesso, K. Dolag, M. Bravo, A. Robotham, E. Tempel, Q. Li, X. Yang, B. Csizi, P. Behroozi, V. Biffi, A. Biviano, G. Lamer, N. Malavasi, D. Mazengo, V. Toptun","doi":"10.1051/0004-6361/202452028","DOIUrl":"https://doi.org/10.1051/0004-6361/202452028","url":null,"abstract":"<i>Context.<i/> With the advent of wide-field cosmological surveys, samples of hundreds of thousands of spectroscopically confirmed galaxy groups and clusters are becoming available. While these large datasets offer a valuable tool to trace the baryonic matter distribution, controlling systematics in the identification of host dark-matter halos and estimating their properties remains crucial.<i>Aims.<i/> We intend to evaluate the predictions of retrieving the population of cluster and group of galaxies using three group-detection methods on a simulated dataset replicating the GAMA survey selection. Our goal is to understand the systematics and selection effects of each group finder, which will be instrumental for interpreting the unprecedented volume of spectroscopic data from SDSS, GAMA, DESI, and WAVES, and for leveraging optical catalogues in the (X-ray) eROSITA era to quantify the baryonic mass in galaxy groups.<i>Methods.<i/> We simulated a spectroscopic galaxy survey in the local Universe (down to <i>z<i/> < 0.2 and stellar mass completeness <i>M<i/><sub>⋆<sub/> ≥ 10<sup>9.8<sup/> <i>M<i/><sub>⊙<sub/>) using a lightcone based on the cosmological hydrodynamical simulation Magneticum. We assessed the completeness and contamination levels of the reconstructed halo catalogues and analysed the reconstructed membership. Finally, we evaluated the halo-mass recovery rate of the group finders and explored potential improvements.<i>Results.<i/> All three group finders demonstrate high completeness levels (> 80%) on the galaxy group and cluster scales, confirming that optical selection is suitable for probing dense regions in the Universe. Contamination at the low-mass end (<i>M<i/><sub>200<sub/> < 10<sup>13<sup/> <i>M<i/><sub>⊙<sub/>) is caused by interlopers and fragmentation. Galaxy membership is at least 70% accurate above the group-mass scale; however, inaccuracies can lead to systematic biases in halo-mass determination using the velocity dispersion of galaxy members. We recommend using other halo-mass proxies less affected by contamination – such as total stellar luminosity or mass – to recover accurate halo masses. Further analysis of the cumulative luminosity function of the galaxy members has shown remarkable accuracy in the group finders’ predictions of the galaxy population.<i>Conclusions.<i/> These results confirm the reliability and completeness of the spectroscopic catalogues compiled by these state-of-the-art group finders. This paves the way for studies that require large sets of spectroscopically confirmed galaxy groups and clusters or studies of galaxy evolution in different environments.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"63 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143427462","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":"The kinematics of 30 Milky Way globular clusters and the multiple stellar populations within","authors":"E. I. Leitinger, H. Baumgardt, I. Cabrera-Ziri, M. Hilker, J. Carbajo-Hijarrubia, M. Gieles, T. O. Husser, S. Kamann","doi":"10.1051/0004-6361/202452477","DOIUrl":"https://doi.org/10.1051/0004-6361/202452477","url":null,"abstract":"<i>Aims<i/>. The spectroscopic and photometric classification of multiple stellar populations (MPs) in Galactic globular clusters (GCs) has enabled comparisons between contemporary observations and formation theories regarding the initial spatial configurations of the MPs. However, the kinematics of these MPs is an aspect that requires more attention. We investigated the 3D kinematics of 30 Galactic GCs, extending to 3–5 half-light radii, as well as their MPs, in order to uncover clues of the initial conditions of GCs and the MPs within.<i>Methods<i/>. We have combined Hubble Space Telescope and <i>Gaia<i/> DR3 proper motions together with a comprehensive set of line-of- sight velocities to determine the 3D rotation amplitudes, rotation axes, and anisotropy profiles of the clusters. We include additional radial velocities from new IFU observations of NGC 5024 and an analysis of archival MUSE data of NGC 6101. We compare our kinematic results with structural and orbital parameters of each cluster, reporting the most significant correlations and common features.<i>Results<i/>. We find significant (>3<i>σ<i/>) rotation in 21 GCs, with no significant differences between the total rotational amplitudes of the MPs, except for NGC 104. We find no significant differences in the position angles of the rotation axis or inclination angles. We find that the 3D rotational amplitude of the clusters in our sample is strongly correlated with their mass, relaxation time, enriched star fraction, and concentration. We determined the anisotropy profiles of each cluster and the MPs where possible. We investigated correlations with the structural parameters, orbital parameters, and accretion history of the clusters from their progenitor systems, finding that the dynamically young clusters with the highest central concentrations of primordial stars exhibit radial anisotropy in their outer regions (>2 half-light radii). The dynamically young clusters with a central concentration of enriched stars show significant tangential anisotropy or isotropy in their outer regions.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"3 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143418367","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":"Multi-scale analysis of the Monoceros OB 1 star-forming region","authors":"R. Bőgner, J. Montillaud, C. Vastel, M. Juvela, L. V. Tóth","doi":"10.1051/0004-6361/202348883","DOIUrl":"https://doi.org/10.1051/0004-6361/202348883","url":null,"abstract":"&lt;i&gt;Context&lt;i/&gt;. Young massive clumps are relatively rare objects and are typically found at large distances. The G202.02+2.85 (hereafter, G202) massive clump was identified in the Monoceros OB 1 molecular complex at a distance of about 700 pc. It was found to be undergoing active star formation and located at the junction point between two colliding filaments.&lt;i&gt;Aims&lt;i/&gt;. We aim to further clarify the evolutionary stage of the clump and the nature of the collision and of six dense cores in the area; specifically, we investigate whether the clump is collapsing as a whole and/or whether it shows signs of shocks.&lt;i&gt;Methods&lt;i/&gt;. To this end, we examined the dense gas properties, notably through NH&lt;sub&gt;3&lt;sub/&gt; and N&lt;sub&gt;2&lt;sub/&gt;H&lt;sup&gt;+&lt;sup/&gt; and their deuterated counterparts. We examined the evolutionary stages of the cores through deuterium fractionation values. We performed a mapping of the clump and deeper pointed molecular line observations towards the dense cores with the IRAM 30-m and Effelsberg 100-m telescopes in the 3-mm and centimetre ranges, respectively. The clump internal dynamics was examined using tracers of various gas densities (CO isotopologues, CS, ammonia, and diazenylium), along with a classical infall diagnosis with HCO&lt;sup&gt;+&lt;sup/&gt; and diazenylium. Furthermore, SiO and methanol were used to characterise the shock properties. The evolutionary stages of the dense cores were evaluated from the deuterium fractionation of ammonia and diazenylium.&lt;i&gt;Results&lt;i/&gt;. The clump seen in dust continuum emission was detected in all dense-gas molecular tracers, including deuterated ammonia and diazenylium, contrasting with the distributions in shock tracers SiO and CH&lt;sub&gt;3&lt;sub/&gt;OH. These latter include both features compatible with protostellar outflows and a more diffuse emission in the clump, all with SiO line width corresponding to relatively low velocity shocks (≲10 km s&lt;sup&gt;−1&lt;sup/&gt;). This could arise from multiple, blended outflows or be a signature of the filament collision. All the dense cores, except for the source 1446, were found to be in early evolutionary stages, the most massive one, the source 1450, being at most a Class 0 object. This is consistent with the idea that they originate in the same clump-compression event. They all present virial parameters indicating gravitational instability, while source 1450 and its surroundings show blue-shift asymmetry in HCO&lt;sup&gt;+&lt;sup/&gt; compatible with gravitational infall, suggesting that this star formation activity came out of the collision. We find that, in contrast to NH&lt;sub&gt;3&lt;sub/&gt; deuterium fractionation, the N&lt;sub&gt;2&lt;sub/&gt;H&lt;sup&gt;+&lt;sup/&gt; deuterium fractionation values are likely to be correlated with the source evolutionary stage.&lt;i&gt;Conclusions&lt;i/&gt;. Our results provide additional evidence that the star-forming cores in the G202 clump originate in the clump compression due to filament collision or convergence. Based on its physical parameters, we find that the source 1454 in the northern cl","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"7 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143417397","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":"New insights with XRISM and Cloudy: A novel column density diagnostic","authors":"Chamani M. Gunasekera, Peter A. M. van Hoof, Masahiro Tsujimoto, Gary J. Ferland","doi":"10.1051/0004-6361/202453133","DOIUrl":"https://doi.org/10.1051/0004-6361/202453133","url":null,"abstract":"<i>Aims.<i/> We present a simple yet powerful column density diagnostic for plasmas enabled by X-ray microcalorimeter observations.<i>Methods.<i/> With the recent developments of the spectral simulation code CLOUDY, inspired by the high spectral resolution of the X-Ray Imaging and Spectroscopy Mission (XRISM) and the Advanced Telescope for High Energy Astrophysics (Athena), we make predictions for the intensity ratio of the resolved fine-structure lines Ly<i>α<i/><sub>1<sub/> and Ly<i>α<i/><sub>2<sub/> of H-like ions.<i>Results.<i/> We show that this ratio can be observationally constrained and used as a plasma column density indicator. We demonstrate this with an XRISM observation of the high-mass X-ray binary Centaurus X-3.<i>Conclusions.<i/> This diagnostic is useful for a wide range of X-ray emitting plasmas that are either collisionally or radiatively ionized.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"4 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143417396","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":"The impact of interplanetary magnetic field intensity on the Martian ionosphere","authors":"Yihui Song, Yun Li, Haoyu Lu, Jinbin Cao, Shibang Li","doi":"10.1051/0004-6361/202453085","DOIUrl":"https://doi.org/10.1051/0004-6361/202453085","url":null,"abstract":"<i>Context.<i/> The interplanetary magnetic field (IMF) is one of the important external drivers that controls the Martian-induced magnetosphere and ionosphere. Previous studies have shown that the ion escape process is highly influenced by both the direction and intensity of the IMF. The enhanced IMF may decrease the ion escape rate by inducing a stronger magnetosphere that protects the Martian ionosphere, but the mechanisms have not been investigated thoroughly. Further studies are needed to reveal the response of ionospheric heavy ions to IMF variation as well as the underlying physical mechanism.<i>Aims.<i/> This study aims to investigate the influence the IMF strength has on the Martian ionosphere. We adopted a multifluid magnetohydrodynamic model in this study, which can self-consistently simulate the interaction between solar wind and Mars. By comparing different cases, we analyzed the ionospheric structure on the dayside and near nightside as well as the ion transport process. We aim to obtain a deeper understanding of how the IMF intensity variation impacts the Martian ionosphere and the escape of planetary ions.<i>Methods.<i/> A three-dimensional multifluid MHD model was used to simulate the interaction between the upstream solar wind and Mars. Four major species in the Martian ionosphere, H<sup>+<sup/>, O<sub>2<sub/><sup>+<sup/>, O<sup>+<sup/>, and CO<sub>2<sub/><sup>+<sup/>, are considered in the model, with the chemical reactions and particle collisions included to calculate ion distribution and ion motions. We analyzed three cases where the IMF strength was set to 1 nT, 3 nT, and 5 nT.<i>Results.<i/> The enhancement of the IMF produces a stronger electromagnetic field in the Martian plasma environment. Both the electric field and magnetic field intensity increase, which provides a shielding effect to the Martian ionosphere, hindering the intrusion of solar wind particles. Thus, less planetary ions are produced by the chemical reactions between the solar wind and the Martian neutral particles, leading to shrinkage of the ionospheric upper boundary. As the IMF strength increases, both the day-to-night plasma transport and the ion outflow decreases. Thus, a more depleted nightside ionosphere is formed, and the tailward ion escape may be weakened, decreasing the global ion escape rate. Moreover, the strong crustal fields in the southern hemisphere enhance the electromagnetic field on the southern dayside, which withstand the penetration of solar wind plasma more effectively, resulting in asymmetry structures in the ionosphere.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"20 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143401445","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":"Wavelength-dependent far-infrared polarization of HL Tau observed with SOFIA/HAWC+","authors":"Moritz Lietzow-Sinjen, Sebastian Wolf, Robert Brunngräber","doi":"10.1051/0004-6361/202450165","DOIUrl":"https://doi.org/10.1051/0004-6361/202450165","url":null,"abstract":"We present the first polarimetric observations of a circumstellar disk in the far-infrared wavelength range. We report flux and linear polarization measurements of the young stellar object HL Tau in the bands A (53 μm), C (89 μm), D (155 μm), and E (216 μm) with the High-resolution Airborne Wideband Camera-plus (HAWC+) on board of the Stratospheric Observatory for Infrared Astronomy (SOFIA). The orientation of the polarization vectors is strongly wavelength-dependent and can be attributed to different wavelength-dependent polarization mechanisms in the disk and its local environment. In bands A, C, and D (53 μm to 155 μm), the orientation of the polarization is roughly consistent with a value of 114° at the maximum emission. Hereby, the magnetic field direction is close to that of the spin axis of the disk. In contrast, in band E (216 μm), the orientation is nearly parallel to the minor axis of the projection of the inclined disk. Based on a viscous accretion disk model combined with a surrounding envelope, we performed polarized three-dimensional Monte Carlo radiative transfer simulations. In particular, we considered polarization due to emission and absorption by aligned dust grains, and polarization due to scattering of the thermal reemission (self-scattering). At wavelengths of 53 μm, 89 μm, and 155 μm, we were able to reproduce the observed orientation of the polarization vectors. Here, the origin of polarization is consistent with polarized emission by aligned non-spherical dust grains. In contrast, at a wavelength of 216 μm, the polarization pattern could not be fully matched, however, applying self-scattering and assuming dust grain radii up to 35 μm, we were able to reproduce the flip in the orientation of polarization. We conclude that the polarization is caused by dichroic emission of aligned dust grains in the envelope, while at longer wavelengths, the envelope becomes transparent and the polarization is dominated by self-scattering in the disk.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"63 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143401447","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":"Hybrid simulation method for agglomerate evolution in driven granular gases","authors":"F. Führer, J. Schwaak, L. Brendel, G. Wurm, D. E. Wolf","doi":"10.1051/0004-6361/202451459","DOIUrl":"https://doi.org/10.1051/0004-6361/202451459","url":null,"abstract":"<i>Aims.<i/> We present a new hybrid simulation method for protoplanetary dust evolution that is efficient and takes into account the complex fragmentation and agglomeration dynamics. We applied it to simulate the evolution of agglomerate size distributions for turbulent, charged systems.<i>Methods.<i/> The hybrid method combines kinetic Monte Carlo and discrete element simulations in such a way that the expensive latter is only deployed when two agglomerates collide. This method can easily be extended to include additional driving mechanisms, interactions, and the effects of inhomogeneities.<i>Results.<i/> Our simulations reveal an emerging steady state in the size distribution. Due to the efficiency of our method, we are able to extend previous results with improved statistics for the size distribution of large agglomerates; in addition to the previously reported power law, we find a regime with an exponential decay.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"161 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-02-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143401446","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}