Astronomy & Astrophysics最新文献_第7页

Edge-on galaxies relative to the edge-on view of the Local Supercluster 相对于本超星系团的正面视图，星系的正面

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-29 DOI: 10.1051/0004-6361/202554906

P. Dolgosheeva, D. Makarov, N. Libeskind

引用次数: 0

Line-of-sight velocity projection impact on Local Group mass determinations 视距速度投影对局部群质量测定的影响

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-28 DOI: 10.1051/0004-6361/202553846

David Benisty, David Mota

{"title":"Line-of-sight velocity projection impact on Local Group mass determinations","authors":"David Benisty, David Mota","doi":"10.1051/0004-6361/202553846","DOIUrl":"https://doi.org/10.1051/0004-6361/202553846","url":null,"abstract":"The mass of the Local Group (LG), which includes the Milky Way, Andromeda (M31), and their satellites, is crucial for validating galaxy formation and cosmological models. Traditional virial mass estimates, which rely on line-of-sight (LoS) velocities and simplified infall assumptions, are prone to systematic biases due to unobserved velocity components and anisotropic kinematics. Using the TNG cosmological simulation, we examined two limiting cases: the minor infall model – which ignores velocities perpendicular to LoS directions – and the major infall model – which assumes purely radial motion toward the center of mass (CoM). Our simulations demonstrate that geometric corrections are vital: the minor infall model underestimates the true mass, while the major infall model overestimates it. By applying these calibrated corrections to observed dwarf galaxy kinematics within 1 Mpc of the LG’s CoM, we derived a refined LG mass of MLG = (2.99 ± 0.60)×1012 M⊙. This finding resolves previous discrepancies as it aligns with predictions from the Λ cold dark matter model, timing arguments, and independent mass estimates. Our analysis highlights the importance of correcting for velocity anisotropy and offers a robust framework for dynamical mass estimations of galaxy groups.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"153 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165110","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}

引用次数: 0

The Pristine Dwarf-Galaxy survey 原始矮星系调查

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-28 DOI: 10.1051/0004-6361/202452323

Nicolas Longeard, Pascale Jablonka, Giuseppina Battaglia, Khyati Malhan, Nicolas F. Martin, Julio F. Navarro, Federico Sestito

{"title":"The Pristine Dwarf-Galaxy survey","authors":"Nicolas Longeard, Pascale Jablonka, Giuseppina Battaglia, Khyati Malhan, Nicolas F. Martin, Julio F. Navarro, Federico Sestito","doi":"10.1051/0004-6361/202452323","DOIUrl":"https://doi.org/10.1051/0004-6361/202452323","url":null,"abstract":"Aims. The Milky Way has a large population of dwarf galaxy satellites. Their properties are sensitive to both cosmology and the physical processes underlying galaxy formation, but these properties are still not properly characterised for the entire satellite population.Methods. We aim to provide the most accurate systemic dynamical and metallicity properties of the dwarf galaxy Boötes II (Boo II).Results. We use a new spectroscopic sample of 39 stars in the field of Boo II (heliocentric distance of ∼66 kpc) with data from the Fiber Large Array Multi Element Spectrograph (FLAMES) mounted on the Very Large Telescope (VLT). The target selection is based on a combination of broadband photometry, proper motions from Gaia, and the metallicity-sensitive narrow-band photometry from the Pristine survey that is ideal for removing obvious Milky Way contaminants.Conclusions. We found nine new members, including five also found by recent works in the literature, and the farthest member to date (5.7 half-light radii from Boo II centroid), extending the spectroscopic spatial coverage of this system. Our metallicity measurements based on the Calcium triplet lines leads to the detection of the two first Extremely Metal-poor stars ([Fe/H] < −3.0) in Boo II. Combining this new dataset with literature data refines Boo II’s velocity dispersion ( km s−1), systemic velocity ( km s−1), and shows that it does not show any sign of a significant velocity gradient (d⟨v⟩/d km s−1 arcmin−1, or −0.5/1.9 km s−1 arcmin−1 as 3σ upper limits). We are thus able to confirm the kinematic and metallicity properties of the satellite as well as identify new members for future high-resolution analyses.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"58 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165106","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}

引用次数: 0

SN 2023xqm: A gradually fading Ia supernova exhibiting isolated high-velocity signatures SN 2023xqm：一颗逐渐褪色的Ia超新星，显示出孤立的高速特征

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-28 DOI: 10.1051/0004-6361/202452864

Xiangyun Zeng, Yijing Luo, Xiaofeng Wang, Xin Li, Yi Yang, Sheng Zheng, Shuguang Zeng, Yao Huang, Sai Li, D. Andrew Howell, K. Azalee Bostroem, Curtis McCully, Ali Esamdin, Moira Andrews, Joseph R. Farah, Megan Newsome, Haonan Zhang, Peng Zhang, Lei Hu

{"title":"SN 2023xqm: A gradually fading Ia supernova exhibiting isolated high-velocity signatures","authors":"Xiangyun Zeng, Yijing Luo, Xiaofeng Wang, Xin Li, Yi Yang, Sheng Zheng, Shuguang Zeng, Yao Huang, Sai Li, D. Andrew Howell, K. Azalee Bostroem, Curtis McCully, Ali Esamdin, Moira Andrews, Joseph R. Farah, Megan Newsome, Haonan Zhang, Peng Zhang, Lei Hu","doi":"10.1051/0004-6361/202452864","DOIUrl":"https://doi.org/10.1051/0004-6361/202452864","url":null,"abstract":"We conducted an exhaustive analysis combining optical photometry and spectroscopy of the type Ia supernova designated SN 2023xqm. Our observational period spanned from the two weeks preceding to 88 days after the B-band peak luminosity time. We determined the peak brightness in the B-band to be −18.90 ± 0.50 mag, and it is accompanied by a moderately slow decay rate of 0.90 ± 0.07 mag. The maximum quasi-bolometric luminosity was estimated to be 1.52 × 1043 erg s−1 and correlated with a calculated 56Ni mass of 0.74 ± 0.05 M⊙, aligning with the modestly reduced rate of light curve decay. A plateau that can be observed in the r − i color curve might correlate with the minor elevation noted between the principal and secondary peaks of the i-band light curve. An initial spectral analysis of SN 2023xqm revealed distinct high-velocity features (HVFs) in Ca II that contrast with the subdued HVFs observed in Si II. Such attributes may stem from variations in ionization or temperature or from scenarios involving enhanced element abundance, suggesting a naturally lower photospheric temperature for SN 2023xqm, which could be indicative of incomplete burning during the white dwarf’s detonation. The observed traits in the light curve and the spectral features offer significant insights into the variability among type Ia supernovae and their explosion dynamics.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"25 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165116","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}

引用次数: 0

Multi-scale exploration of SMACS J0723.3–7327’s intracluster light and past dynamical history SMACS J0723.3-7327星团内光和过去动力学历史的多尺度探索

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-28 DOI: 10.1051/0004-6361/202553716

Amaël Ellien

{"title":"Multi-scale exploration of SMACS J0723.3–7327’s intracluster light and past dynamical history","authors":"Amaël Ellien","doi":"10.1051/0004-6361/202553716","DOIUrl":"https://doi.org/10.1051/0004-6361/202553716","url":null,"abstract":"We present an analysis of the intracluster light (ICL) in the galaxy cluster SMACS J0723.3–7327 (hereafter, SMACS J0723) using JWST/NIRCam deep imaging in six filters (F090W to F444W). We processed images for low surface brightness (LSB) science, applying additional corrections for instrumental scattering in the short-wavelength channels. We analysed the images using wavelet-based decomposition and extracted and modelled the ICL, brightest cluster galaxy (BCG), and satellite galaxies, generating 2D maps for each component. The ICL and ICL + BCG fractions, computed in all filters within a 400 kpc radius, exhibit a flat trend with wavelength, averaging 28% and 34%, respectively. Flux ratios between the BCG and the next brightest members (M12, M13, and M14) also display minimal wavelength dependence. These results indicate that SMACS J0723 is a dynamically evolved cluster with a dominant BCG and well-developed ICL. We analysed five prominent ICL substructures that contribute 10–12% of the total ICL+BCG flux budget, slightly exceeding simulation predictions. Their short dynamical timescales suggest an instantaneous ICL injection rate of several 103 L⊙ yr−1, consistent with active dynamical assembly. These findings support a scenario where SMACS J0723’s ICL growth is currently driven by galaxy mergers involving the BCG and other bright satellites, rather than by the accretion of pre-processed ICL from a recent cluster merger. However, extrapolating the current injection rate to the cluster’s lifetime indicates that additional mechanisms are required to match the growth observed in other clusters over cosmic timescales.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"33 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165109","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}

引用次数: 0

The impact of ram pressure on cluster galaxies, insights from GAEA and TNG 撞击压力对星系团的影响，来自GAEA和TNG的见解

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-28 DOI: 10.1051/0004-6361/202553915

Lizhi Xie, Gabriella De Lucia, Matteo Fossati, Fabio Fontanot, Michaela Hirschmann

{"title":"The impact of ram pressure on cluster galaxies, insights from GAEA and TNG","authors":"Lizhi Xie, Gabriella De Lucia, Matteo Fossati, Fabio Fontanot, Michaela Hirschmann","doi":"10.1051/0004-6361/202553915","DOIUrl":"https://doi.org/10.1051/0004-6361/202553915","url":null,"abstract":"Ram pressure stripping (RPS) has a non-negligible impact on the gas content of cluster galaxies. We used the semi-analytic model GAEA and the hydro-simulation TNG to investigate whether cluster galaxies suffer from strong RPS that is sufficient to remove a significant fraction of their gas during the first pericentric passage. We estimated that a ram pressure of 10−10.5, 10−12, 10−13.5g cm−1 s−2 can remove 90%, 50%, and 20% of the cold gas reservoir from low-mass galaxies with 9 < log M⋆/M⊙ < 9.5, assuming the gas can be stripped instantaneously. We then used this information to divide the phase space diagram into “strong”, “moderate”, “weak”, and “no” RPS zones. By tracing the orbit of galaxies since 2.5Rvir, we find in both GAEA and TNG that about half of the galaxies in Virgo-like halos ( log Mh/M⊙ ∼ 14) did not suffer strong RPS during the first pericentric passage. In Coma-like halos ( log Mh/M⊙ ∼ 15), almost all galaxies have suffered strong RPS during the first pericentric passage, which can remove all gas from low-mass galaxies but is insufficient to significantly reduce the gas content of more massive galaxies. In general, results from TNG and GAEA are consistent, with the RPS being only slightly stronger in TNG than in GAEA. Our findings suggest that most cluster galaxies maintain a notable fraction of their gas and continue forming stars after the first pericentric passage, except for those with a low stellar mass ( log M⋆/M⊙ < 9.5) in very massive halos ( log Mh/M⊙ > 15).","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"40 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165117","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}

引用次数: 0

Driven two-fluid Alfvén waves in a solar magnetic flux tube with a realistic ionization rate 太阳磁通量管中具有实际电离率的驱动双流体alfvsamn波

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-28 DOI: 10.1051/0004-6361/202554085

J. Kraśkiewicz, K. Murawski

{"title":"Driven two-fluid Alfvén waves in a solar magnetic flux tube with a realistic ionization rate","authors":"J. Kraśkiewicz, K. Murawski","doi":"10.1051/0004-6361/202554085","DOIUrl":"https://doi.org/10.1051/0004-6361/202554085","url":null,"abstract":"Context. This study was performed in the context of the chromosphere and low corona heating.Aims. We considered the evolution of driven Alfvén waves in the solar atmosphere, whose initial state was modeled with a realistic ionization profile. We discuss their potential role in plasma heating.Methods. Two- and half-dimensional (2.5 D) numerical simulations of the solar atmosphere were performed with the use of the code JOANNA. The dynamics of the atmosphere was described by the two-fluid equations (and ionization and recombination terms were taken into account) for ions (protons) combined with electrons and neutrals (hydrogen atoms). The initial atmosphere was described by a hydrostatic background supplemented by the Saha equation and embedded in a magnetic flux tube. This background was perturbed by a monochromatic driver that operated in the transversal components of the ion and neutral velocities.Results. We demonstrated that as a result of ion-neutral collisions, Alfvén waves are damped. The damping length grows with the wave period. This is anticipated based on the linear theory for a homogeneous medium. The developed flux-tube model results at higher temperatures rise for shorter periods of the driving wave, and the effect is stronger than for the pure hydrostatic state.Conclusions. We highlight the importance of taking the realistic background plasma into account in the evolution of two-fluid Alfvén waves that participate in the thermal energy release and in the heating in the solar chromosphere and low corona.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"48 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165107","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}

引用次数: 0

Discovery of a bimodal luminosity distribution in the persistent Be/X-ray pulsar 2RXP J130159.6–635806 在持续的Be/ x射线脉冲星2RXP J130159.6-635806中发现双峰光度分布

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-28 DOI: 10.1051/0004-6361/202453378

Alexander Salganik, Sergey S. Tsygankov, Maria Chernyakova, Denys Malyshev, Juri Poutanen

{"title":"Discovery of a bimodal luminosity distribution in the persistent Be/X-ray pulsar 2RXP J130159.6–635806","authors":"Alexander Salganik, Sergey S. Tsygankov, Maria Chernyakova, Denys Malyshev, Juri Poutanen","doi":"10.1051/0004-6361/202453378","DOIUrl":"https://doi.org/10.1051/0004-6361/202453378","url":null,"abstract":"We present a comprehensive analysis of 2RXP J130159.6−635806, a persistent low-luminosity Be/X-ray pulsar, focusing on its transition to a spin equilibrium state and the discovery of a bimodal luminosity distribution that possibly reveals a new accretion regime. Using data from the NuSTAR, Swift, XMM-Newton, and Chandra observatories, we investigated changes in the pulsar’s timing and spectral properties. After more than 20 years of continuous spin-up, the pulsar’s spin period has stabilized, marking the onset of spin equilibrium. This transition was accompanied by the emergence of a previously unobserved accretion regime at erg s−1, an order of magnitude lower than its earlier quiescent state. After that, the source occasionally switched between these regimes, remaining in each state for extended periods, with the transition from a luminosity of 1035 erg s−1 to 1034 erg s−1 taking less than 2.3 days. The analysis of the spectral data collected during this new low-luminosity state revealed a two-hump shape that is different from the cutoff power-law spectra observed at higher luminosities. The discovery of pulsations in this state, together with the hard spectral shape, indicates ongoing accretion. We estimate the magnetic field strength to be ∼1013 G based on indirect methods. Additionally, we report a hint of a previously undetected ∼90-day orbital period in the system.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"16 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165108","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}

引用次数: 0

Quasi-periodic pulsations in extreme-ultraviolet brightenings 极紫外光增亮中的准周期脉动

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-28 DOI: 10.1051/0004-6361/202554587

Daye Lim, Tom Van Doorsselaere, David Berghmans, Laura A. Hayes, Cis Verbeeck, Nancy Narang, Marie Dominique, Andrew R. Inglis

{"title":"Quasi-periodic pulsations in extreme-ultraviolet brightenings","authors":"Daye Lim, Tom Van Doorsselaere, David Berghmans, Laura A. Hayes, Cis Verbeeck, Nancy Narang, Marie Dominique, Andrew R. Inglis","doi":"10.1051/0004-6361/202554587","DOIUrl":"https://doi.org/10.1051/0004-6361/202554587","url":null,"abstract":"Context. Extreme-ultraviolet (EUV) observations have revealed small-scale transient brightenings that may be caused by the same physical mechanisms as larger-scale solar flares. A notable feature of solar and stellar flares is the presence of quasi-periodic pulsations (QPPs), which are a potentially intrinsic characteristic.Aims. We investigated the properties of QPPs detected in EUV brightenings, which are considered to be small-scale flares, and compared their statistical properties with those observed in solar and stellar flares.Methods. We extracted integrated light curves of 22 623 EUV brightenings in two quiet Sun regions observed by the Solar Orbiter/Extreme Ultraviolet Imager and identified QPPs in their light curves using Fourier analysis.Results. Approximately 2.7% of the EUV brightenings exhibited stationary QPPs. The QPP occurrence rate increased with the surface area, lifetime, and peak brightness of the EUV brightenings. The detected QPP periods ranged from approximately 15 to 260 seconds, which is comparable to the periods observed in solar and stellar flares. Consistent with observations of QPPs in solar and stellar flares, no correlation was found between the QPP period and peak brightness. However, unlike the trend observed in solar flares, no correlation was found between the QPP period and the lifetime or length scale.Conclusions. The presence of QPPs in EUV brightenings supports the interpretation that these events may be small-scale manifestations of flares, and the absence of period scaling with loop length further suggests that standing waves may not be the primary driver of QPPs in these events.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"48 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165118","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}

引用次数: 0

Tidal interaction can stop galactic bars: On the LMC non-rotating bar 潮汐的相互作用可以阻止星系棒：在LMC非旋转棒上

IF 6.5 2区物理与天体物理

Astronomy & Astrophysics Pub Date : 2025-05-28 DOI: 10.1051/0004-6361/202555019

Ó. Jiménez-Arranz, S. Roca-Fàbrega

{"title":"Tidal interaction can stop galactic bars: On the LMC non-rotating bar","authors":"Ó. Jiménez-Arranz, S. Roca-Fàbrega","doi":"10.1051/0004-6361/202555019","DOIUrl":"https://doi.org/10.1051/0004-6361/202555019","url":null,"abstract":"Context. The bar pattern speed of the LMC has been computed based on data from Gaia DR3 using three different methods. One method suggested that the LMC might be hosting a bar that barely rotates, and is slightly counter-rotating with respect to the disc of the LMC, with a pattern speed of Ωp = −1.0 ± 0.5 km s−1 kpc−1.Aims. We aim to confirm that tidal interactions might prevent the bar hosted by the LMC from rotating as a result of its interaction with the SMC. This might cause the bar in the LMC to slow down significantly until it (momentarily) stops.Methods. We analysed a subset of models (K9 and K21) from the KRATOS suite in which we detected non-rotating bars. We used two different methods to track the evolution of the bar pattern speed: the program patternSpeed.py and temporal finite-differences of the change in the rate in the major axis of the phase angle of the bar.Results. In the second LMC–SMC-like pericenter passage of K9, the bar of the LMC-like galaxy weakens so much as to almost disappear and regenerates with a pattern speed that slows down from Ωp ∼ 20 km s−1 kpc−1 to Ωp ∼ 0 km s−1 kpc−1 in less than 75 Myr. Then, the bar rotates at less than Ωp ∼ 3 − 5 km s−1 kpc−1 for about 100 Myr, until it recovers the initial (before the interaction) pattern speed of Ωp ∼ 10 km s−1 kpc−1. The results for the K21 simulation are similar.Conclusions. We show that galactic bars can be slowed down or even stopped by tidal interaction. This strengthens the hypothesis that the LMC hosts a non-rotating bar, and it can be an alternative formation scenario for other observed slowly rotating bars.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"35 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144165105","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}

引用次数: 0