Astronomische Nachrichten最新文献

{"title":"Cover Picture: Astron. Nachr. 11/2025","authors":"","doi":"10.1002/asna.70065","DOIUrl":"https://doi.org/10.1002/asna.70065","url":null,"abstract":"<p>\u0000 \u0000 <figure>\u0000 <div><picture>\u0000 <source></source></picture><p></p>\u0000 </div>\u0000 </figure></p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 10","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-12-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70065","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145772316","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Issue Information: Astron. Nachr. 11/2025","authors":"","doi":"10.1002/asna.70066","DOIUrl":"https://doi.org/10.1002/asna.70066","url":null,"abstract":"","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 10","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-12-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70066","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145779369","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Investigating Circumstellar Atomic Radiation-Driven Dynamics","authors":"Alexandra Lehtmets,&nbsp;Mihkel Kama,&nbsp;Luca Fossati,&nbsp;Anna Aret","doi":"10.1002/asna.70071","DOIUrl":"https://doi.org/10.1002/asna.70071","url":null,"abstract":"<div>\u0000 \u0000 <p>The interactions between stars and their orbiting planets, driven by forces such as stellar radiation and gravity, play an essential role in shaping exoplanetary atmospheres and gas-rich debris discs. One way to look into the composition of these environments is to observe how they can contaminate the stellar photospheres. For that, we examine how stellar radiation pressure and gravity influence atomic species and analyze their effects across various stellar effective temperatures. Using the radiative-to-gravitational force ratio, we determined the atomic movement direction and assessed the velocity boost imparted to neutral atoms escaping from exoplanet atmospheres or debris discs. Incorporating the solar far ultraviolet/extreme ultraviolet spectrum to address flux discrepancies in the ATLAS9 model, we find that radiation affects atoms differently according to their ionization state, with highly ionized species less affected by stellar radiation. Our results conclude that the stars most suitable for observing stellar contamination are those between 6500 and 8000 K, with neutral noble gases and ionized iron-peak elements as the most likely contaminants.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 2","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-12-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146223927","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Unveiling the Cosmos: XMM-Newton's Scientific Strategy","authors":"Norbert Schartel,&nbsp;Maria Santos-Lleo","doi":"10.1002/asna.70063","DOIUrl":"https://doi.org/10.1002/asna.70063","url":null,"abstract":"<div>\u0000 \u0000 <p>In December 2024, the European Space Agency's (ESA) XMM-Newton X-ray Observatory celebrated the 25th anniversary of its launch. The annual number of peer-reviewed articles utilising XMM-Newton data has exhibited a consistent upward trajectory over the past two and a half decades, attaining more than 400 in 2022. The annual call for observing time proposals continues to experience a high level of oversubscription, typically ranging from a factor of 6–7. In order to enhance the scientific discovery space, XMM-Newton, primarily through the Project Scientist and Science Operations Centre, has pursued a strategy of expansion, which can be grouped into three phases: Large Projects with long observing time (2006–2009), Joint Observations (2011–2016) and Targets of Opportunity (2016–2024), respectively. A salient feature of XMM-Newton's time allocation is the systematic removal of biases from the second call onwards, a strategy that has enabled the attainment of comparable gender success rates and high acceptance rates for young scientists over 25 years, a feat only recently accomplished by similar missions through the introduction of double-anonymous review. XMM-Newton research is conducted by an active community of 4300 scientists, of which approximately 570 are leading (1st author). The foundation of this community and its research is predicated on XMM-Newton data, with the project's policy of user support and calibration being fundamental constituents, as well as the project's active engagement and communication with its members.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 2","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146216810","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Confirmation of a Non-Transiting Planet in the Habitable Zone of the Nearby M Dwarf L 98-59","authors":"Paul I. Schwarz,&nbsp;Stefan Dreizler,&nbsp;René Heller","doi":"10.1002/asna.70059","DOIUrl":"https://doi.org/10.1002/asna.70059","url":null,"abstract":"&lt;p&gt;Only 40 exoplanetary systems with five or more planets are currently known. These systems are crucial for our understanding of planet formation and planet-planet interaction. The M dwarf L 98-59 has previously been found to show evidence of five planets, three of which are transiting. Our aim is to confirm the fifth planet in this system and to refine the system characteristics namely minimum masses, radii and the orbital parameters of the planets around L 98-59. We reanalysed RV and activity data from HARPS and ESPRESSO alongside TESS and HST transit data using a joint model. The parameter space was sampled using the dynesty nested sampler. We confirm the previously known fifth planet in the system's habitable zone with an orbital period of &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msubsup&gt;\u0000 &lt;mn&gt;23.069&lt;/mn&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;0.082&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;mn&gt;0.081&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/msubsup&gt;\u0000 &lt;mspace&gt;&lt;/mspace&gt;\u0000 &lt;mtext&gt;days&lt;/mtext&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {23.069}_{-0.082}^{+0.081}kern0.5em mathrm{days} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;, a minimum mass of &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msubsup&gt;\u0000 &lt;mn&gt;2.97&lt;/mn&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;0.48&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;mn&gt;0.46&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/msubsup&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;M&lt;/mi&gt;\u0000 &lt;mo&gt;⊕&lt;/mo&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {2.97}_{-0.48}^{+0.46}{M}_{oplus } $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; and an equilibrium temperature of 284 K. We find an additional planet candidate in the RV data with an orbital period of &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mn&gt;1.736&lt;/mn&gt;\u0000 &lt;mspace&gt;&lt;/mspace&gt;\u0000 &lt;msubsup&gt;\u0000 &lt;mn&gt;15&lt;/mn&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;0.000&lt;/mn&gt;\u0000 &lt;mspace&gt;&lt;/mspace&gt;\u0000 &lt;mn&gt;76&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;mn&gt;0.000&lt;/mn&gt;\u0000 &lt;mspace&gt;&lt;/mspace&gt;\u0000 &lt;mn&gt;74&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 ","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 2","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-11-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70059","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146217523","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Commissioning an Inexpensive Off-The-Shelf Spectrograph for Radial-Velocity Studies","authors":"Lukas Stock,&nbsp;Andreas Schrimpf","doi":"10.1002/asna.70067","DOIUrl":"https://doi.org/10.1002/asna.70067","url":null,"abstract":"<p>We present a way to set up an inexpensive out of the shelf spectrograph at a local observatory. Stability and resolution of the spectrograph are high enough for radial velocity determination of binary stars or determination of stellar characteristics. Even some exoplanets might be detectable via the radial velocity method.</p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 2","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-11-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70067","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146217522","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"PERICLES: A Set of Empirical Rotational Isochrones Modeled on Cool Dwarfs in Open Clusters and Wide Binaries","authors":"David Gruner,&nbsp;Sydney A. Barnes","doi":"10.1002/asna.70056","DOIUrl":"10.1002/asna.70056","url":null,"abstract":"<p>Isochrones, equal-age curves, are widely used in astrophysics to estimate stellar ages. Classical stellar parameters are, however, very limited in their usability for main sequence stars because of their weak age-dependence. Here, rotation period measurements provide complementary information. We construct and present a set of rotational isochrones, named the Potsdam Empirical Rotational Isochrones from CLustEr Stars (<span>Pericles</span>), that leverage rotation periods. They are constructed empirically using stars in well-studied open clusters and a small number of complementary field stars. The rotational isochrones span the main sequence stars from late-F type near the Kraft break to the fully-convective boundary around M3 stars, and are available for ages ≤ 6 Gyr. We also discuss a limitation to such color- or temperature based rotational isochrones, together with ideas to overcome it.</p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 1","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-11-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70056","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146083332","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"SN 2021adlw: Supernova or LBV Outburst?","authors":"D. Yu. Tsvetkov,&nbsp;N. N. Pavlyuk,&nbsp;N. P. Ikonnikova,&nbsp;M. A. Burlak,&nbsp;A. A. Belinski,&nbsp;A. V. Dodin,&nbsp;S. A. Potanin,&nbsp;N. I. Shatsky,&nbsp;V. A. Echeistov","doi":"10.1002/asna.70069","DOIUrl":"10.1002/asna.70069","url":null,"abstract":"<div>\u0000 \u0000 <p>We present low-resolution optical spectroscopic and photometric observations of SN 2021adlw. The photometric monitoring in <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>U</mi>\u0000 <mspace></mspace>\u0000 <mi>BV</mi>\u0000 <mspace></mspace>\u0000 <mi>gri</mi>\u0000 </mrow>\u0000 <annotation>$$ Ukern0.5em BVkern0.5em gri $$</annotation>\u0000 </semantics></math> filters continued for 122 days and 2 spectra were collected. The early spectrum allowed to classify the transient as SN IIn, but later it was supposed that it was an outburst of LBV. The spectra and color curves of SN 2021adlw reveal high extinction in the host galaxy, for which we give an estimate <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>E</mi>\u0000 <mrow>\u0000 <mo>(</mo>\u0000 <mrow>\u0000 <mi>B</mi>\u0000 <mo>−</mo>\u0000 <mi>V</mi>\u0000 </mrow>\u0000 <mo>)</mo>\u0000 </mrow>\u0000 <mo>=</mo>\u0000 <mn>0.56</mn>\u0000 <mo>±</mo>\u0000 <mn>0.15</mn>\u0000 </mrow>\u0000 <annotation>$$ Eleft(B-Vright)=0.56pm 0.15 $$</annotation>\u0000 </semantics></math> mag. The spectra before maximum show lines of HI with narrow peaks and wide wings, with FWHM about 350 and 3000 km·s⁻¹, respectively. SN 2021adlw displays typical for most of SNe IIn photometric evolution: long rise to the maximum and slow, nearly linear brightness decline. The peak absolute magnitude is <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>M</mi>\u0000 <mi>V</mi>\u0000 </msub>\u0000 <mo>=</mo>\u0000 <mo>−</mo>\u0000 <mn>16.8</mn>\u0000 <mo>±</mo>\u0000 <mn>0.45</mn>\u0000 <mspace></mspace>\u0000 <mi>mag</mi>\u0000 </mrow>\u0000 <annotation>$$ {M}_V=-16.8pm 0.45 mathrm{mag} $$</annotation>\u0000 </semantics></math>. We propose SN 2021adlw is a low-luminosity type IIn supernova.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 1","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-11-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146091535","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Cover Picture: Astron. Nachr. 9/2025","authors":"","doi":"10.1002/asna.70058","DOIUrl":"https://doi.org/10.1002/asna.70058","url":null,"abstract":"<p>In this Original Article L.R. Bedin et. al. present groundbreaking observations made possible by the James Webb Space Telescope: https://onlinelibrary.wiley.com/doi/10.1002/asna.70042\u0000 \u0000 <figure>\u0000 <div><picture>\u0000 <source></source></picture><p></p>\u0000 </div>\u0000 </figure></p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 9","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70058","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145476375","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Barium Abundances of A–F–G Type Stars in the Hyades Cluster","authors":"Yoichi Takeda","doi":"10.1002/asna.70060","DOIUrl":"https://doi.org/10.1002/asna.70060","url":null,"abstract":"&lt;div&gt;\u0000 \u0000 &lt;p&gt;With an aim of clarifying the extent and parameter-dependence of compositional anomaly of barium in A-type stars, Ba abundances were spectroscopically determined based on Ba &lt;span&gt;ii&lt;/span&gt; 6141/6496 lines for 89 (23 A-type and 66 F–G-type) main-sequence stars belonging to the members of Hyades cluster by taking into account the non-LTE effect and the hyper-fine-structure effect. While the non-LTE effect tends to strengthen lines in G stars, it acts in the direction of line weakening in the regime of A stars due to increasing importance of overionization. The Ba abundances of G stars turned out almost constant (&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;⟨&lt;/mo&gt;\u0000 &lt;mi&gt;A&lt;/mi&gt;\u0000 &lt;mo&gt;⟩&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mo&gt;=&lt;/mo&gt;\u0000 &lt;mn&gt;2.33&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ leftlangle Arightrangle =2.33 $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;), indicating that the primordial composition of Ba in Hyades is mildly supersolar by &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;≃&lt;/mo&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;mn&gt;0.2&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ simeq +0.2 $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; dex. In contrast, A-type stars show Ba overabundances of considerably large dispersion (0 &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;≲&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ lesssim $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; [Ba/H] &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;≲&lt;/mo&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ lesssim 2 $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;). Since this Ba excess tends to increase with an increase/decrease in &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;T&lt;/mi&gt;\u0000 &lt;mi&gt;eff&lt;/mi&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {T}_{mathrm{eff}} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;/&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;v&lt;/mi&gt;\u0000 &lt;mi&gt;e&lt;/mi&gt;\u0000 &lt;/msub&gt;\u0000 &lt;mi&gt;sin&lt;/mi&gt;\u0000 &lt;mi&gt;i&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {v}_{mathrm{e}}sin i $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;, these two parameters may be essential for producing or controlling the anomaly. Regarding Hyades F-type stars, their Ba abundances are not uniform but show a broad depression (by &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;≲&lt;/mo&gt;\u0000 &lt;mn&gt;0.3&lt;/mn&gt;\u0000 &lt;/mr","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 1","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146091118","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}