Astronomy & Astrophysics最新文献

{"title":"The transport of large near-Earth objects into the Centaur region","authors":"R. A. N. Araujo, L. Liberato, O. C. Winter","doi":"10.1051/0004-6361/202556155","DOIUrl":"https://doi.org/10.1051/0004-6361/202556155","url":null,"abstract":"<i>Context<i/>. Near-Earth objects (NEOs) and Centaurs are minor bodies that orbit the Sun in the terrestrial and giant-planet regions, respectively. Recent studies show that approximately 9% of the known large NEOs that leave the terrestrial planet region are transported to the Centaur region, where they can remain for at least 5000 years.<i>Aims<i/>. We present a detailed analysis of the transport of NEOs to the Centaur region. We refer to these objects as NEO-Centaurs.<i>Methods<i/>. We analyzed numerical integrations of the <i>N<i/>-body gravitational problem, including the Sun, the eight planets, and a sample of 839 known NEOs larger than 1 km (absolute magnitude <i>H<i/> < 18). We also conducted a statistical analysis based on 8390 clones to quantify the likelihood of NEO transport to the Centaur region.<i>Results<i/>. A significant fraction of NEOs is likely transported to the Centaur region over an average timescale of approximately 7.8 Myr. The median residence time in the Centaur region is estimated to be 20 000 years. The average residence time is 2.3 Myr. We also identify one case in which the NEO-Centaur reached the trans-Neptunian objects (TNOs) region. The statistical analysis confirms a significant likelihood that NEOs are transported to the Centaur region. The probabilistic measure based on clone statistics indicates that only 13% of NEOs larger than 1 km have no successful clones reaching the Centaur region, while 14% have a probability greater than or equal to 50% of becoming NEO-Centaurs.<i>Conclusions<i/>. We infer that NEO-Centaurs comprise 0.01-1% of the population of Centaurs larger than 1 km and are likely composed of bodies smaller than 5 km in diameter.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"5 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147755069","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":"Ammonia deuteration mechanism in interstellar conditions","authors":"O. E. Hernández Alvarez, D. Rednyk, Š. Roučka, I. Bondari, S. Soboli, P. Dohnal, R. Plašil, J. Glosík","doi":"10.1051/0004-6361/202659362","DOIUrl":"https://doi.org/10.1051/0004-6361/202659362","url":null,"abstract":"<i>Aims<i/>. We investigate the reaction mechanism of deuterium transfer in the D<sub>3<sub/><sup>+<sup/> + NH<sub>3<sub/> reaction. The distinction between proton hop and full scrambling mechanisms is critical for accurate modeling of deuterated ammonia isotopologs.<i>Methods<i/>. The reaction rate coefficients and product branching fractions were measured in a cryogenic 22-pole radiofrequency ion trap between 110 and 300 K. The D<sub>3<sub/><sup>+<sup/> ions were stored in helium buffer gas at number densities of 10<sup>13<sup/>−10<sup>14<sup/> cm<sup>−3<sup/> and reacted with ammonia at controlled number densities of 10<sup>10<sup/>−10<sup>11<sup/> cm<sup>−3<sup/>.<i>Results<i/>. The reaction proceeds with reaction rate coefficients decreasing from (5.4 ± 1.1) × 10<sup>−9<sup/> cm<sup>3<sup/>s<sup>−1<sup/> at 149 K to (3.9 ± 0.8) × 10<sup>−9<sup/> cm<sup>3<sup/>s<sup>−1<sup/> at 293 K, close to the capture rate coefficient predicted by the average dipole orientation theory. The measured reaction rate coefficients exhibit a systematic isotope effect compared to the analogous H<sub>3<sub/><sup>+<sup/> + NH<sub>3<sub/> system, with D<sub>3<sub/><sup>+<sup/> reacting slightly more slowly. The product branching fractions reveal that NH<sub>3<sub/>D<sup>+<sup/> is the dominant product throughout the temperature range, with a branching fraction greater than 99.5% at low temperatures. This observation confirms that the reaction proceeds via the proton hop mechanism rather than full scrambling.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"16 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147755070","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":"Spin-up and spin distribution of stellar black holes grown by gas accretion in proto-stellar clusters","authors":"Zacharias Roupas","doi":"10.1051/0004-6361/202558435","DOIUrl":"https://doi.org/10.1051/0004-6361/202558435","url":null,"abstract":"Proto-stellar clusters, likely progenitors of globular clusters, are extremely compact with typical masses of ~10<sup>6<sup/> M<sub>⊙<sub/> and sizes of ~1 pc, as has recently been revealed by James Webb Space Telescope observations at <i>z<i/> ~ 10. Sufficiently high compactness can provide a time window for early-formed stellar black holes (BHs) to accrete primordial gas. We developed a semi-analytic model to follow BH spin-up and determine the final spin distribution of stellar BHs that grow in mass via gas accretion within compact gaseous protostellar clusters. The velocity shear within a BH’s sphere of influence induces the formation of an accretion disk that is repeatedly disrupted by stochastic perturbations to the BH motion. We assumed low initial BH spins of <i>a<i/><sub>*,ini<sub/> = 0.01, consistent with stellar-evolution models with efficient angular-momentum transport, and we restricted initial BH masses to values below the upper BH mass gap, <i>m<i/><sub>BH,ini<sub/> < 55 M<sub>⊙<sub/>. Our analysis shows a strong BH spin-mass correlation, obtained within ~10 Myr when gas is depleted. Low-spin BHs, <i>a<i/><sub>*<sub/> ≤ 0.3, are predominantly low-mass, <i>m<i/><sub>BH<sub/> ≲ 25 M<sub>⊙<sub/>, in contrast to high-spin BHs, <i>a<i/><sub>*<sub/> ≥ 0.7, which are predominantly high-mass, <i>m<i/><sub>BH<sub/> ≳ 65 M<sub>⊙<sub/>. Notably, there exist also low-spin, high-mass outliers with ~1 mass-gap BH per cluster expected to have <i>a<i/><sub>*<sub/> ~ 0.1. The general trend, however, expressed by the median spin as a function of final BH mass, is well fit by a high-spin saturating exponential with a transition mass of ~50 M<sub>⊙<sub/>. For <i>m<i/><sub>BH<sub/> ≥ 100 M<sub>⊙<sub/> the median spin is , with the central 68% of the distribution spanning <i>a<i/><sub>*<sub/> ~ 0.70–0.96, in striking agreement with the estimated spins of the BH components of the gravitational-wave signal GW231123. These spin values persist up to the highest masses generated by our mechanism, <i>m<i/><sub>BH<sub/> ~ 10<sup>3<sup/> M<sub>⊙<sub/>.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"2 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147755102","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 mmax-Mecl relation in the LEGUS clusters","authors":"Marie Zinnkann, Tereza Jerabkova, Zhiqiang Yan, Pavel Kroupa, Yannik Ostermann, Eda Gjergo, Akram Hasani Zonoozi, Hosein Haghi, Jan Pflamm-Altenburg","doi":"10.1051/0004-6361/202556969","DOIUrl":"https://doi.org/10.1051/0004-6361/202556969","url":null,"abstract":"The relation between the maximum stellar mass in a very young cluster (<i>m<i/><sub>max<sub/>) and the total stellar mass of the cluster (<i>M<i/><sub>ecl<sub/>), known as the <i>m<i/><sub>max<sub/> − <i>M<i/><sub>ecl<sub/> relation, remains debated in the literature. To test the validity of this relation, we modelled young star clusters with masses between 10<sup>2.5<sup/> and 10<sup>5.0<sup/><i>M<i/><sub>⊙<sub/> and ages of 1–4 Myr using the galIMF code, in which stellar masses are optimally sampled from a varying initial stellar mass function. We compared the results with literature observations of extragalactic young star clusters. We incorporated stellar evolution via PARSEC and COLIBRI tracks and computed H<i>α<i/> luminosities using the Pégase code. To account for dynamical ejections, we stochastically removed stars based on their spectral type, following previous <i>N<i/>-body simulations. Additional sources of scatter, including uncertainties in age determination and contamination by field stars, were considered. Our results indicate that, under the assumptions explored here, optimal sampling is consistent with the extragalactic star cluster observations considered, whereas purely random sampling produces distributions that are not in agreement. These findings support a highly self-regulated interpretation of cluster formation in which stellar masses align optimally with the initial mass function rather than being drawn independently at random.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"139 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147755183","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":"Coronal mass ejection plasma diagnostics using Metis coronagraph","authors":"S. Jejčič, P. Heinzel, G. Russano, V. Andretta, P. Schwartz, J. Štěpán, R. Susino, M. Romoli, A. Burtovoi, Y. De Leo, G. Jerse, F. Landini, G. Nicolini, M. Pancrazzi, C. Sasso","doi":"10.1051/0004-6361/202557268","DOIUrl":"https://doi.org/10.1051/0004-6361/202557268","url":null,"abstract":"<i>Context.<i/> We investigate the physical conditions of erupting prominences embedded in coronal mass ejection (CME) cores.<i>Aims.<i/> The physical parameters of interest were derived by combining the hydrogen Lyman <i>α<i/> (L<i>α<i/>) and visible-light (VL) images simultaneously observed by Solar Orbiter/Metis. In particular, we focus on the bright CME event that occurred on April 25-26, 2021.<i>Methods.<i/> Our method is based on 2D non-LTE (i.e. non-local thermodynamic equilibrium) modeling of moving structures to derive the integrated intensity of the L<i>α<i/> line (<i>E<i/><sub>L<sub/><i>α<i/>), together with VL emission. Our method is based on a novel diagnostic tool that combines the emission measure (<i>EM<i/>) at a given temperature derived from the observed L<i>α<i/> intensity with the electron column density (<i>N<i/><sub>e<sub/>) obtained from VL Stokes <i>I<i/> and <i>Q<i/> data. This approach determines the electron density (<i>n<i/><sub>e<sub/>) and the effective thickness (<i>D<i/><sub>eff<sub/>) inside the prominence structure. Here, we use a similar diagnostic tool to the one that we proposed for solar eclipses by combining hydrogen Balmer <i>α<i/> (H<i>α<i/>) and VL data in previous studies.<i>Results.<i/> We analyzed 32 spatial points within the northern part of the prominence. We ran a 2D non-LTE transfer code for these points by assuming a uniform prominence temperature. The results are presented as 2D maps of the electron density and effective thickness at a given temperature. For the brightest pixel, we also estimated the temperature by assuming collisional ionization equilibrium and compared the result with our value obtained using the emission-measure method.<i>Conclusions.<i/> We demonstrate how <i>n<i/><sub>e<sub/> and <i>D<i/><sub>eff<sub/> inferences depend on the temperature of the structure. The higher the temperature, the lower the effective thickness, and the higher the electron density. This study creates foundation for future diagnostics of eruptive prominences with the Solar Orbiter/Metis coronagraph. It shows that combined UV and VL diagnostics provides a powerful tool for analyzing such events. But it also confirms that the consideration of the helium D<sub>3<sub/> line emission within the VL channel is essential to obtain accurate results.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"151 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147751720","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 kinematic cosmic dipole beyond Ellis and Baldwin","authors":"Albert Bonnefous","doi":"10.1051/0004-6361/202659275","DOIUrl":"https://doi.org/10.1051/0004-6361/202659275","url":null,"abstract":"The cosmic dipole anomaly–currently detected at a significance exceeding 5<i>σ<i/> in several independent surveys poses a significant challenge to the standard model of cosmology. The Ellis and Baldwin formula provides a theoretical link between the intrinsic dipole anisotropy in the sky distribution of extragalactic light sources and the observer’s velocity relative to the cosmic rest frame, under the assumptions that the sources follow a power-law luminosity function and exhibit power-law spectral energy distributions. Even though for a monochromatic survey fitting a power law on the spectra at the flux limit is always sufficient, it fails for the case of sources with more complicated spectra in photometric surveys, such as galaxies in the visible and near-infrared, which can feature emission lines or breaks. In this work, we demonstrate that the Ellis and Baldwin formula can be generalized to arbitrary luminosity distributions and spectral profiles in particular for photometric surveys. We derived the corresponding expression for the effective spectral index and applied it to a sample of quasars observed in the W1 band of the CatWISE survey. We show that the anomalous cosmic dipole persists beyond the power-law assumption in this sample. These results provide a more general and robust framework to interpret measurements of the cosmic dipole in future photometric large-scale surveys.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"12 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147751722","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":"Radial modes of pressure bumps and dips in astrophysical discs","authors":"Armand Leclerc, Guillaume Laibe, Elliot Lynch, Nicolas Perez","doi":"10.1051/0004-6361/202558428","DOIUrl":"https://doi.org/10.1051/0004-6361/202558428","url":null,"abstract":"<i>Aims.<i/> We investigate signatures of pressure extrema on global oscillations in discs.<i>Methods.<i/> We used the framework of wave topology to establish a generalised local dispersion relation that includes pressure gradients. We highlight the influence of a previously unrecognised epicyclic–acoustic frequency, and we derive an analytical criterion for the existence of a branch of modes transiting between the inertial and the pressure bands, known as topological modes.<i>Results.<i/> We find that pressure extrema consist of wave guides in which such topological modes propagate. The fundamental mode trapped at a pressure bump can propagate at any frequency, allowing it to resonate with any temporal forcing. Conversely, the fundamental mode associated with a pressure dip propagates at any vertical phase velocity. These specific features make them attractive candidates for future discoseismology.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"6 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147751717","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":"Not all nitrogen-rich field stars originate from globular clusters","authors":"E. I. Leitinger, A. Miglio, J. Montalbán, D. Massari, A. Bragaglia, W. E. van Rossem, K. Brogaard, A. Mazzi, J. S. Thomsen, E. Willett","doi":"10.1051/0004-6361/202558003","DOIUrl":"https://doi.org/10.1051/0004-6361/202558003","url":null,"abstract":"Globular clusters (GCs) are important tracers of the early Galactic assembly process, with some of their stars showing distinct chemical abundance patterns. When such stars are found in the Galactic field rather than within GCs, they are assumed to have originated from clusters. We expand the search for these chemically enriched stars in the <i>Kepler<i/> field, targeting stars located in the halo, thin and thick disc, to show the potential in using asteroseismology to link the inferred masses, and hence, ages, with chemical abundances and kinematics. Using data from APOGEE DR17, <i>Gaia<i/> DR3, and the <i>Kepler<i/> mission, we identify primordial stars as those with chemical signatures typical of field stars, and enriched stars as those exhibiting strong nitrogen enrichment, with corresponding carbon and oxygen depletion. We present our sample of 133 red giant branch and core-He-burning stars, 92 of which have measured masses and inferred age estimates from asteroseismology. Of the 20 enriched stars we identified, 13 have precise asteroseismic ages, of which 3 at most are old enough (>8 Gyr) to plausibly originate from globular clusters. The inferred asteroseismic ages indicate that most enriched stars found in the field appear too young to have originated from GCs; however, these apparently young ages are likely the result of assuming single-star evolution, rather than accounting for binary interactions or mergers. This indicates alternative enrichment and evolutionary scenarios, such as mass transfer or coalescence, rather than a globular-cluster origin for most field nitrogen-rich stars.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"23 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147751718","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 full evolution of the type-C quasi-periodic oscillations in MAXI J1348–630 revealed by Insight-HXMT","authors":"X.-L. Wang, Z. Yan, F.-G. Xie, J.-F. Wang, Y.-X. Li, Z.-Y. Liu, R.-Y. Ma","doi":"10.1051/0004-6361/202558220","DOIUrl":"https://doi.org/10.1051/0004-6361/202558220","url":null,"abstract":"<i>Context.<i/> Type-C quasi-periodic oscillations (QPOs) in black hole X-ray binaries serve as sensitive probes of accretion geometry and variability, although their full evolution throughout the entire outburst and the physics driving the evolution are not yet fully understood.<i>Aims.<i/> Utilizing the intensive, broadband observations by Insight-HXMT of MAXI J1348−630, we aim to comprehensively investigate the properties and evolution of type-C QPOs during both its main 2019 outburst and subsequent mini-outbursts.<i>Methods.<i/> We performed a comprehensive timing and spectral analysis of Insight-HXMT data. The evolution of QPO frequency, fractional rms, and energy dependence was tracked across spectral states, and correlations with X-ray flux and spectral shape were examined.<i>Results.<i/> (1) The type-C QPO frequency rose from 0.24 Hz to 7.28 Hz during the main outburst rise and subsequently exhibited a nearly constant value of ∼7 Hz when the QPOs reappeared across different spectral states. (2) The fractional rms spectrum underwent a pronounced hardening following the transition from the hard to the hard-intermediate state. (3) The correlation between QPO frequency and X-ray flux exhibited strong hysteresis between the rise and decay phases; notably, the hysteresis loop reversed direction between the main and mini-outbursts. (4) In contrast, the frequency and hardness followed a tight, nearly single-track anticorrelation.<i>Conclusions.<i/> Our results provide a complete picture of type-C QPO evolution. The stable reappearance frequency at ∼7 Hz indicates that the Compton region may reform at a consistent characteristic scale across different spectral states. Results (3) and (4) suggest that the type-C QPO frequency evolution is governed more by spectral shape than by X-ray luminosity, while the reversed hysteresis provides a new perspective on the differences between the main and mini-outbursts, possibly originating from variations in the initial conditions.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"6 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147751727","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":"A comparison of pendulum models for large-amplitude longitudinal prominence oscillations","authors":"Iñigo Arregui","doi":"10.1051/0004-6361/202659882","DOIUrl":"https://doi.org/10.1051/0004-6361/202659882","url":null,"abstract":"Large-amplitude prominence oscillations offer diagnostic information relevant to understanding the magnetic and plasma structure of solar prominences. Accurate prominence seismology requires the use of reliable models. The so-called pendulum model for large-amplitude longitudinal prominence oscillations has demonstrated robustness against observations and numerical simulations. Recent improvements have extended the model to situations with non-uniform gravity, thus leading to corrections that have implications for the inference of the magnetic field strength. In this study we quantify how the different model predictions given by the original and extended pendulum models impact the inference of the minimum magnetic field strength derived from the observed periods of large-amplitude longitudinal prominence oscillations. The analysis we conducted follows a Bayesian approach to solve the inference problem and assess the absolute and relative plausibilities of the two considered models in explaining the observed data, with their uncertainty. We find that the Bayesian solution to the inference problem provides well-constrained posteriors for the minimum magnetic field strength. However, the solutions from each adopted model differ, with differences increasing with the oscillation period. A model comparison analysis results in the extended model being more plausible in the full range of observed periods. However, the magnitude of the Bayes factor is not large enough to determine whether there is positive evidence supporting any of the models. We suggest computing model-averaged posteriors as the most reasonable solution to the inference problem.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"69 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147751723","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}