Astronomische Nachrichten最新文献

{"title":"Editor's Note: The X-Ray Mysteries of Neutron Stars and White Dwarfs","authors":"Norbert Schartel","doi":"10.1002/asna.20240093","DOIUrl":"https://doi.org/10.1002/asna.20240093","url":null,"abstract":"","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 1","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-10-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143120180","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":"Probing the Propeller Regime With Wide Neutron Star Binaries","authors":"M. D. Afonina,&nbsp;S. B. Popov","doi":"10.1002/asna.20240096","DOIUrl":"https://doi.org/10.1002/asna.20240096","url":null,"abstract":"<div>\u0000 \u0000 <p>We model the duration of the propeller stage in wide binary systems with neutron stars and calculate the time of accretion onset for various propeller models. We apply our modeling to the symbiotic X-ray binary SWIFT J0850.8-4219. Unless a propeller with a very slow spin-down is operating, it is very improbable to find a system similar to SWIFT J0850.8-4219 at the propeller stage. Then we model the evolution of a neutron star in a binary with a solar-like companion. We calculate for which orbital separations and magnetic fields a neutron star can start to accrete while the companion is still on the Main sequence. We demonstrate that for the magnetic field <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>B</mi>\u0000 <mo>≲</mo>\u0000 <msup>\u0000 <mn>10</mn>\u0000 <mn>12</mn>\u0000 </msup>\u0000 </mrow>\u0000 <annotation>$$ Blesssim {10}^{12} $$</annotation>\u0000 </semantics></math> G neutron stars at the orbital separation <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>a</mi>\u0000 <mo>≳</mo>\u0000 <mn>1</mn>\u0000 </mrow>\u0000 <annotation>$$ agtrsim 1 $$</annotation>\u0000 </semantics></math> AU do not reach the propeller stage. In the case of a slow propeller spin-down, neutron stars never start to accrete. For the more rapid propeller spin-down, a neutron star can start to accrete or spend a long time at the propeller stage depending on the parameters.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 1","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-10-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143120179","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":"Issue Information: Astron. Nachr. 07/2024","authors":"","doi":"10.1002/asna.20249007","DOIUrl":"https://doi.org/10.1002/asna.20249007","url":null,"abstract":"","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 8","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.20249007","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142443503","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":"Cover Picture: Astron. Nachr. 8/2024","authors":"Hikmet Çakmak,&nbsp;Talar Yontan,&nbsp;Selçuk Bilir,&nbsp;Timothy S. Banks,&nbsp;Raúl Michel,&nbsp;Esin Soydugan,&nbsp;Seliz Koç,&nbsp;Hülya Erçay","doi":"10.1002/asna.20249016","DOIUrl":"https://doi.org/10.1002/asna.20249016","url":null,"abstract":"<p>Vector-Point Diagrams (left panels) and proper-motion component vectors (right panels) for identified member stars in the open clusters Ruprecht 1 and Ruprecht 171. These two previously little-studied open clusters, both at a distance of approximately 1.5 kpc, have been characterized and studied in some detail in the related paper by Çakmak and collaborators, published in this issue e240054.\u0000 <figure>\u0000 <div><picture>\u0000 <source></source></picture><p></p>\u0000 </div>\u0000 </figure></p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 8","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.20249016","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142443544","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":"Denoising Medium Resolution Stellar Spectra With Neural Networks","authors":"Balázs Pál,&nbsp;László Dobos","doi":"10.1002/asna.20240049","DOIUrl":"https://doi.org/10.1002/asna.20240049","url":null,"abstract":"<div>\u0000 \u0000 <p>We trained denoiser autoencoding neural networks on medium resolution simulated optical spectra of late-type stars to demonstrate that the reconstruction of the original flux is possible at a typical relative error of a fraction of a percent down to a typical signal-to-noise ratio of <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>10</mn>\u0000 </mrow>\u0000 <annotation>$$ 10 $$</annotation>\u0000 </semantics></math> per pixel. We show that relatively simple networks are capable of learning the characteristics of stellar spectra while still flexible enough to adapt to different values of extinction and fluxing imperfections that modifies the overall shape of the continuum, as well as to different values of Doppler shift. Denoised spectra can be used to find initial values for traditional stellar template fitting algorithms and—since evaluation of pretrained neural networks is significantly faster than traditional template fitting—denoiser networks can be useful when a fast analysis of the noisy spectrum is necessary, for example during observations, between individual exposures.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 9-10","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143187007","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":"HX Velorum: Ellipsoidal/Rotational Binary With β Cep Type Component","authors":"B. Gürol","doi":"10.1002/asna.20240028","DOIUrl":"https://doi.org/10.1002/asna.20240028","url":null,"abstract":"&lt;div&gt;\u0000 \u0000 &lt;p&gt;We present the Transiting Exoplanet Survey Satellite (TESS) light curve analysis of HX Velorum, located in the Southern Hemisphere, where one of the components is found for the first time to be a &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;β&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ beta $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; Cep (BCEP) type pulsator. The TESS observations of HX Velorum were published in a total of 6 sectors. Fourier analysis of the observations reveals that the frequencies can be divided into two categories, one of which is related to the orbital period and the other related to the &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;β&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ beta $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; Cep-type pulsation. Its non-eclipsing light curve was analyzed with the well-known Wilson–Devinney code, and we obtained the geometric and physical parameters of the components using published radial velocity and light curve data by making some assumptions. We obtained plausible masses and radii of the primary and secondary components as &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;M&lt;/mi&gt;\u0000 &lt;mn&gt;1&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;mo&gt;=&lt;/mo&gt;\u0000 &lt;mn&gt;9.48&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.27&lt;/mn&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;$$ {M}_1=9.48pm 0.27{M}_{odot } $$&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;M&lt;/mi&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;mo&gt;=&lt;/mo&gt;\u0000 &lt;mn&gt;5.92&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.17&lt;/mn&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;$$ {M}_2=5.92pm 0.17{M}_{odot } $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; and &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;R&lt;/mi&gt;\u0000 &lt;mn&gt;1&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;mo&gt;=&lt;/mo&gt;\u0000 &lt;mn&gt;3.93&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.04&lt;/mn&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;R&lt;/mi&gt;\u0000 &lt;mo&gt;⊙&lt;/mo&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {R}_1=3.93pm 0.04{R}_{odot } $$&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 ","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 8","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142443557","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":"Red Quasars: Estimation of SMBH Spin, Mass, and Accretion Disk Inclination Angle","authors":"M. Yu. Piotrovich,&nbsp;S. D. Buliga,&nbsp;T. M. Natsvlishvili","doi":"10.1002/asna.20240058","DOIUrl":"https://doi.org/10.1002/asna.20240058","url":null,"abstract":"<div>\u0000 \u0000 <p>We estimated values of spin, mass, and inclination angle for sample of 42 red quasars. Our estimations show that two objects: F2MS J1113+1244 and F2MS J1434+0935 with the highest Eddington ratios may have geometrically thick disk. Six objects: SDSS J0036-0113, S82X 0040+0058, S82X 0118+0018, S82X 0303-0115, FBQS J1227+3214, S82X 2328-0028 may have “retrograde” rotation. Analysis of estimated spin values shows that red quasar population may contain Seyfert galaxies and NLS1.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 8","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142443411","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":"Photometric and Kinematic Studies of Open Clusters Ruprecht 1 and Ruprecht 171","authors":"Hikmet Çakmak,&nbsp;Talar Yontan,&nbsp;Selçuk Bilir,&nbsp;Timothy S. Banks,&nbsp;Raúl Michel,&nbsp;Esin Soydugan,&nbsp;Seliz Koç,&nbsp;Hülya Erçay","doi":"10.1002/asna.20240054","DOIUrl":"https://doi.org/10.1002/asna.20240054","url":null,"abstract":"&lt;div&gt;\u0000 \u0000 &lt;p&gt;This study outlines a detailed investigation using CCD &lt;i&gt;UBV&lt;/i&gt; and &lt;i&gt;Gaia&lt;/i&gt; DR3 data sets of the two open clusters Ruprecht 1 (Rup-1) and Ruprecht 171 (Rup-171). Fundamental astrophysical parameters such as color excesses, photometric metallicities, ages, and isochrone distances were based on &lt;i&gt;UBV&lt;/i&gt;-data analyses, whereas membership probability calculations, structural and astrophysical parameters, as well as the kinematic analyses were based on &lt;i&gt;Gaia&lt;/i&gt; DR3-data. We identified 74 and 596 stars as the most probable cluster members with membership probabilities over 50% for Rup-1 and Rup-171, respectively. The color excesses &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;E&lt;/mi&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;(&lt;/mo&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;B&lt;/mi&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mi&gt;V&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mo&gt;)&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ Eleft(B-Vright) $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; were obtained as &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mn&gt;0.166&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.022&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ 0.166pm 0.022 $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; and &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mn&gt;0.301&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.027&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ 0.301pm 0.027 $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; mag for Rup-1 and Rup-171, respectively. Photometric metallicity analyses were performed by considering F-G type main-sequence member stars and found to be &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;mrow&gt;\u0000 &lt;mi&gt;Fe&lt;/mi&gt;\u0000 &lt;mo&gt;/&lt;/mo&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mo&gt;]&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mo&gt;=&lt;/mo&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;0.09&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.16&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ left[mathrm{Fe}/mathrm{H}right]=-0.09pm 0.16 $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; and &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;mrow&gt;\u0000 &lt;mi&gt;Fe&lt;/mi&gt;\u0000 &lt;mo&gt;/&lt;/mo&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mo&gt;]&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mo&gt;=&lt;/mo&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;0.20&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 ","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 8","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142443404","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. 7/2024","authors":"Klaus G. Strassmeier,&nbsp;Ilya Ilyin,&nbsp;Manfred Woche,&nbsp;Frank Dionies,&nbsp;Michael Weber,&nbsp;Arto Järvinen,&nbsp;Carsten Denker,&nbsp;Ekaterina Dineva,&nbsp;Meetu Verma,&nbsp;Thomas Granzer,&nbsp;Wilbert Bittner,&nbsp;Svend-Marian Bauer,&nbsp;Jens Paschke,&nbsp;Hakan Önel","doi":"10.1002/asna.20249015","DOIUrl":"https://doi.org/10.1002/asna.20249015","url":null,"abstract":"<p>First-light spectra of the Sun as a star taken by SDI-POL, the Solar Disk Integration POLarimeter feeding the PEPSI night-time spectrograph at the LBT. The <i>top panel</i> shows the full wavelength range (383 - 907 nm) covered by SDI-POL. The color of the Stokes <i>I</i> spectra indicates the individual cross dispersers; dark blue (=CD 1) to dark red (=CD 6). The line at the bottom represents the normalized Stokes <i>V Q &amp; U</i> signal on the same intensity scale as Stokes <i>I</i>. The <i>bottom panel</i> is a zoom into the spectral region around the sodium D lines. The top spectrum is again Stokes <i>I</i> (plotted are dots per CCD pixel connected by a line), the bottom spectra are Stokes <i>V Q U</i> shifted by -0.10 in intensity and expanded by a factor 200 in scale with respect to Stokes <i>I</i>. The <i>I Q U</i> spectrum was taken on UT May 20, 2022, the <i>V</i>-spectrum on UT June 22, 2023. The first-light application detects a clear Stokes <i>V/I</i> profile indicative of a tiny but significant solar disk-averaged line-of-sight net magnetic field of +0.37±0.02 Gauß on Oct. 13, 2023, as reported in the article by Strassmeier <i>et al</i>., this issue, e240033.\u0000 <figure>\u0000 <div><picture>\u0000 <source></source></picture><p></p>\u0000 </div>\u0000 </figure></p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 6-7","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-08-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.20249015","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142021732","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. 07/2024","authors":"","doi":"10.1002/asna.20249006","DOIUrl":"https://doi.org/10.1002/asna.20249006","url":null,"abstract":"","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 6-7","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-08-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.20249006","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142021722","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}