The Potsdam Empirical Rotational Isochrones from CLustEr Stars (PERICLES) shown in a GAIA color period diagram. Such isochrones can be used to apply gyrochronology, the method of deriving the age of a late-type main sequence stars from its observed color and rotation period, to individual field stars, enabling the construction of Galactic chronologies. The PERICLES isochrones are applicable across the color range of GKM stars, up to, and beyond solar age. The isochrones are based on the observed rotational sequences of stars in a series of open stellar clusters with known ages. Details are available in the associated publication in this issue by Gruner & Barnes (e70056)
{"title":"Cover Picture: Astron. Nachr. 01/2026","authors":"","doi":"10.1002/asna.70079","DOIUrl":"10.1002/asna.70079","url":null,"abstract":"<p>The Potsdam Empirical Rotational Isochrones from CLustEr Stars (PERICLES) shown in a GAIA color period diagram. Such isochrones can be used to apply gyrochronology, the method of deriving the age of a late-type main sequence stars from its observed color and rotation period, to individual field stars, enabling the construction of Galactic chronologies. The PERICLES isochrones are applicable across the color range of GKM stars, up to, and beyond solar age. The isochrones are based on the observed rotational sequences of stars in a series of open stellar clusters with known ages. Details are available in the associated publication in this issue by Gruner & Barnes (e70056)\u0000\u0000 <figure>\u0000 <div><picture>\u0000 <source></source></picture><p></p>\u0000 </div>\u0000 </figure></p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 1","pages":""},"PeriodicalIF":1.0,"publicationDate":"2026-01-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70079","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146096526","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}
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 (Pericles), 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.
{"title":"PERICLES: A Set of Empirical Rotational Isochrones Modeled on Cool Dwarfs in Open Clusters and Wide Binaries","authors":"David Gruner, 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}
D. Yu. Tsvetkov, N. N. Pavlyuk, N. P. Ikonnikova, M. A. Burlak, A. A. Belinski, A. V. Dodin, S. A. Potanin, N. I. Shatsky, V. A. Echeistov
We present low-resolution optical spectroscopic and photometric observations of SN 2021adlw. The photometric monitoring in 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 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 . We propose SN 2021adlw is a low-luminosity type IIn supernova.
{"title":"SN 2021adlw: Supernova or LBV Outburst?","authors":"D. Yu. Tsvetkov, N. N. Pavlyuk, N. P. Ikonnikova, M. A. Burlak, A. A. Belinski, A. V. Dodin, S. A. Potanin, N. I. Shatsky, 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<sup>−1</sup>, 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}
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
{"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}
<div> <p>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 <span>ii</span> 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 (<span></span><math> <semantics> <mrow> <mrow> <mo>⟨</mo> <mi>A</mi> <mo>⟩</mo> </mrow> <mo>=</mo> <mn>2.33</mn> </mrow> <annotation>$$ leftlangle Arightrangle =2.33 $$</annotation> </semantics></math>), indicating that the primordial composition of Ba in Hyades is mildly supersolar by <span></span><math> <semantics> <mrow> <mo>≃</mo> <mo>+</mo> <mn>0.2</mn> </mrow> <annotation>$$ simeq +0.2 $$</annotation> </semantics></math> dex. In contrast, A-type stars show Ba overabundances of considerably large dispersion (0 <span></span><math> <semantics> <mrow> <mo>≲</mo> </mrow> <annotation>$$ lesssim $$</annotation> </semantics></math> [Ba/H] <span></span><math> <semantics> <mrow> <mo>≲</mo> <mn>2</mn> </mrow> <annotation>$$ lesssim 2 $$</annotation> </semantics></math>). Since this Ba excess tends to increase with an increase/decrease in <span></span><math> <semantics> <mrow> <msub> <mi>T</mi> <mi>eff</mi> </msub> </mrow> <annotation>$$ {T}_{mathrm{eff}} $$</annotation> </semantics></math>/<span></span><math> <semantics> <mrow> <msub> <mi>v</mi> <mi>e</mi> </msub> <mi>sin</mi> <mi>i</mi> </mrow> <annotation>$$ {v}_{mathrm{e}}sin i $$</annotation> </semantics></math>, 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 <span></span><math> <semantics> <mrow> <mo>≲</mo> <mn>0.3</mn> </mr
为了阐明a型恒星中钡成分异常的程度和参数依赖性，利用Ba ii 6141/6496谱线，考虑非lte效应和超精细结构效应，对Hyades星团89颗（23颗a型和66颗f - g型）主序星的Ba丰度进行了光谱测定。虽然非lte效应倾向于增强G星中的谱线，但由于过电离的重要性日益增加，它在A星谱线减弱的方向上起作用。G星的Ba丰度几乎是恒定的（⟨A⟩= 2.33 $$ leftlangle Arightrangle =2.33 $$），表明Hyades中Ba的原始成分为轻度超太阳成分，指数为≤0.2 $$ simeq +0.2 $$。相比之下，a型恒星显示出相当大色散的Ba过丰度（0 > $$ lesssim $$ [Ba/H] > 2 $$ lesssim 2 $$）。由于Ba过剩倾向于随着T / f $$ {T}_{mathrm{eff}} $$ / v / sin i $$ {v}_{mathrm{e}}sin i $$的增加/减少而增加，这两个参数对于产生或控制异常可能是必不可少的。对于毕宿座f型恒星，它们的Ba丰度并不均匀，而是在T ～ 6500 $$ {T}_{mathrm{eff}}sim 6500 $$ K附近出现了一个广泛的下降（下降了约0.3 $$ lesssim 0.3 $$指数）。有趣的是与Li-dip的位置一致。
{"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":"<div>\u0000 \u0000 <p>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 <span>ii</span> 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 (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mrow>\u0000 <mo>⟨</mo>\u0000 <mi>A</mi>\u0000 <mo>⟩</mo>\u0000 </mrow>\u0000 <mo>=</mo>\u0000 <mn>2.33</mn>\u0000 </mrow>\u0000 <annotation>$$ leftlangle Arightrangle =2.33 $$</annotation>\u0000 </semantics></math>), indicating that the primordial composition of Ba in Hyades is mildly supersolar by <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≃</mo>\u0000 <mo>+</mo>\u0000 <mn>0.2</mn>\u0000 </mrow>\u0000 <annotation>$$ simeq +0.2 $$</annotation>\u0000 </semantics></math> dex. In contrast, A-type stars show Ba overabundances of considerably large dispersion (0 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≲</mo>\u0000 </mrow>\u0000 <annotation>$$ lesssim $$</annotation>\u0000 </semantics></math> [Ba/H] <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≲</mo>\u0000 <mn>2</mn>\u0000 </mrow>\u0000 <annotation>$$ lesssim 2 $$</annotation>\u0000 </semantics></math>). Since this Ba excess tends to increase with an increase/decrease in <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>T</mi>\u0000 <mi>eff</mi>\u0000 </msub>\u0000 </mrow>\u0000 <annotation>$$ {T}_{mathrm{eff}} $$</annotation>\u0000 </semantics></math>/<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>v</mi>\u0000 <mi>e</mi>\u0000 </msub>\u0000 <mi>sin</mi>\u0000 <mi>i</mi>\u0000 </mrow>\u0000 <annotation>$$ {v}_{mathrm{e}}sin i $$</annotation>\u0000 </semantics></math>, 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 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≲</mo>\u0000 <mn>0.3</mn>\u0000 </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}
<div> <p>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 <span>ii</span> 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 (<span></span><math> <semantics> <mrow> <mrow> <mo>⟨</mo> <mi>A</mi> <mo>⟩</mo> </mrow> <mo>=</mo> <mn>2.33</mn> </mrow> <annotation>$$ leftlangle Arightrangle =2.33 $$</annotation> </semantics></math>), indicating that the primordial composition of Ba in Hyades is mildly supersolar by <span></span><math> <semantics> <mrow> <mo>≃</mo> <mo>+</mo> <mn>0.2</mn> </mrow> <annotation>$$ simeq +0.2 $$</annotation> </semantics></math> dex. In contrast, A-type stars show Ba overabundances of considerably large dispersion (0 <span></span><math> <semantics> <mrow> <mo>≲</mo> </mrow> <annotation>$$ lesssim $$</annotation> </semantics></math> [Ba/H] <span></span><math> <semantics> <mrow> <mo>≲</mo> <mn>2</mn> </mrow> <annotation>$$ lesssim 2 $$</annotation> </semantics></math>). Since this Ba excess tends to increase with an increase/decrease in <span></span><math> <semantics> <mrow> <msub> <mi>T</mi> <mi>eff</mi> </msub> </mrow> <annotation>$$ {T}_{mathrm{eff}} $$</annotation> </semantics></math>/<span></span><math> <semantics> <mrow> <msub> <mi>v</mi> <mi>e</mi> </msub> <mi>sin</mi> <mi>i</mi> </mrow> <annotation>$$ {v}_{mathrm{e}}sin i $$</annotation> </semantics></math>, 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 <span></span><math> <semantics> <mrow> <mo>≲</mo> <mn>0.3</mn> </mr
为了阐明a型恒星中钡成分异常的程度和参数依赖性，利用Ba ii 6141/6496谱线，考虑非lte效应和超精细结构效应，对Hyades星团89颗（23颗a型和66颗f - g型）主序星的Ba丰度进行了光谱测定。虽然非lte效应倾向于增强G星中的谱线，但由于过电离的重要性日益增加，它在A星谱线减弱的方向上起作用。G星的Ba丰度几乎是恒定的（⟨A⟩= 2.33 $$ leftlangle Arightrangle =2.33 $$），表明Hyades中Ba的原始成分为轻度超太阳成分，指数为≤0.2 $$ simeq +0.2 $$。相比之下，a型恒星显示出相当大色散的Ba过丰度（0 > $$ lesssim $$ [Ba/H] > 2 $$ lesssim 2 $$）。由于Ba过剩倾向于随着T / f $$ {T}_{mathrm{eff}} $$ / v / sin i $$ {v}_{mathrm{e}}sin i $$的增加/减少而增加，这两个参数对于产生或控制异常可能是必不可少的。对于毕宿座f型恒星，它们的Ba丰度并不均匀，而是在T ～ 6500 $$ {T}_{mathrm{eff}}sim 6500 $$ K附近出现了一个广泛的下降（下降了约0.3 $$ lesssim 0.3 $$指数）。有趣的是与Li-dip的位置一致。
{"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":"<div>\u0000 \u0000 <p>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 <span>ii</span> 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 (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mrow>\u0000 <mo>⟨</mo>\u0000 <mi>A</mi>\u0000 <mo>⟩</mo>\u0000 </mrow>\u0000 <mo>=</mo>\u0000 <mn>2.33</mn>\u0000 </mrow>\u0000 <annotation>$$ leftlangle Arightrangle =2.33 $$</annotation>\u0000 </semantics></math>), indicating that the primordial composition of Ba in Hyades is mildly supersolar by <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≃</mo>\u0000 <mo>+</mo>\u0000 <mn>0.2</mn>\u0000 </mrow>\u0000 <annotation>$$ simeq +0.2 $$</annotation>\u0000 </semantics></math> dex. In contrast, A-type stars show Ba overabundances of considerably large dispersion (0 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≲</mo>\u0000 </mrow>\u0000 <annotation>$$ lesssim $$</annotation>\u0000 </semantics></math> [Ba/H] <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≲</mo>\u0000 <mn>2</mn>\u0000 </mrow>\u0000 <annotation>$$ lesssim 2 $$</annotation>\u0000 </semantics></math>). Since this Ba excess tends to increase with an increase/decrease in <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>T</mi>\u0000 <mi>eff</mi>\u0000 </msub>\u0000 </mrow>\u0000 <annotation>$$ {T}_{mathrm{eff}} $$</annotation>\u0000 </semantics></math>/<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>v</mi>\u0000 <mi>e</mi>\u0000 </msub>\u0000 <mi>sin</mi>\u0000 <mi>i</mi>\u0000 </mrow>\u0000 <annotation>$$ {v}_{mathrm{e}}sin i $$</annotation>\u0000 </semantics></math>, 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 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≲</mo>\u0000 <mn>0.3</mn>\u0000 </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":"146091117","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}
扫码关注我们
求助内容：
应助结果提醒方式：
京公网安备 11010802042870号