Astronomische Nachrichten最新文献

{"title":"Letter From the Editor","authors":"Klaus G. Strassmeier","doi":"10.1002/asna.20240141","DOIUrl":"https://doi.org/10.1002/asna.20240141","url":null,"abstract":"<p>With the present first issue of volume 346 in 2025, we enter the 204th year of continuous appearance of Astronomische Nachrichten/Astronomical Notes (AN). The continuing complexity of worldwide scientific publishing had kept us busy over the years; it also impacts AN. The tricky part for our comparably small journal is maintaining a high standard, but also being openly accessible at the same time, preferably without costs. The end product shall be a peer-reviewed, content-oriented, and thus user-oriented, widely distributed and easily accessible journal with original research papers that one is happy to cite.</p><p>This is achieved with accompanying editorial changes. While we currently still rely on the ScholarOne submission platform for user interaction, it will be replaced with the new editorial system Research Exchange (ReX) that is being rolled out as a peer-review tool to all Wiley journals during the course of this year. eLocators instead of the sequential page numbers for easy identification, a modern web appearance where you can find the latest but also all historical volumes of AN, and open access as part of the European DEAL treaty remain cornerstones. AN's most recent Journal Impact Factor (Clarivate) is 1.1.</p><p>As before, the Leibniz-Institute for Astrophysics Potsdam (AIP) continues hosting the editorial office in close collaboration with Wiley. The editorial team can be contacted through <span>[email protected]</span>. Papers are welcomed in all fields of astronomy, astrophysics, and solar-system research, as well as related aspects in instrumentation, astrobiologic, and historic studies. Many thanks in advance. We are looking forward to another year of submissions.</p><p>The author declares no conflicts of interest.</p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 1","pages":""},"PeriodicalIF":1.1,"publicationDate":"2025-01-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.20240141","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143112296","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":"Stellar Physics and General Relativity","authors":"Shuichi Yokoyama","doi":"10.1002/asna.20240127","DOIUrl":"https://doi.org/10.1002/asna.20240127","url":null,"abstract":"<p>The general theory of relativity is currently established as the most precise theory of gravity supported by observations, and its application is diverse ranging from astronomy to cosmology, while its application to astrophysics has been restricted only to compact stars due to the assumption that the Newtonian approximation is sufficient for celestial bodies with medium density such as the sun. Surprisingly, the recent research of the author has implied that this long-held assumption is not valid, and that nonperturbative effects significantly change relevant results obtained by Newtonian gravity. In particular, local physical quantities inside the sun are newly predicted to exhibit power law differently from the so-called standard solar model. This surprising result is reviewed including brief discussion of physics behind the discrepancy and a little new application.</p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 3-4","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-12-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.20240127","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144206988","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":"Concluding Remarks to the IWARA 2024","authors":"J. E. Horvath","doi":"10.1002/asna.20240137","DOIUrl":"https://doi.org/10.1002/asna.20240137","url":null,"abstract":"<div>\u0000 \u0000 <p>A brief discussion of the science presented at the IWARA 2024 (with emphasis in Cosmology) is given as a summary of the workshop held in Machu Picchu, Peru.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 3-4","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-12-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144206982","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":"Carl Wirtz' Article From 1924 in Astronomische Nachrichten on the Radial Motions of Spiral Nebulae","authors":"Tom Richtler","doi":"10.1002/asna.20240062","DOIUrl":"https://doi.org/10.1002/asna.20240062","url":null,"abstract":"<div>\u0000 \u0000 <p>In the year 1924, a paper by Carl Wirtz appeared in ‘<i>Astronomische Nachrichten</i>’, entitled ‘De Sitter's cosmology and the radial motion of spiral galaxies’. This paper and its author remained largely unnoticed by the community, but it seems to be the first cosmological interpretation of the redshift of galaxies as a time dilation effect and the expansion of the Universe. Edwin Hubble knew Wirtz' publications quite well. The modern reader would find Wirtz' own understanding diffuse and contradictory in some aspects, but that reflected the early literature on nebulae, to which he himself made important contributions. The 100th anniversary provides a good opportunity to present an English transcription to the community, which can be found in the appendix. This anniversary also provokes to ask for the present status of cosmology which many authors see in a crisis. From an observational viewpoint, it shall be illustrated that until today there is no consistent/convincing understanding of how the Universe evolved.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 9-10","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-12-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143187084","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":"The Surprising Long-Term Evolution of the ULXP NGC 7793 P13","authors":"Felix Fürst,&nbsp;Dominic J. Walton,&nbsp;Matteo Bachetti,&nbsp;Hannah Earnshaw,&nbsp;Murray Brightman","doi":"10.1002/asna.20240106","DOIUrl":"https://doi.org/10.1002/asna.20240106","url":null,"abstract":"<div>\u0000 \u0000 <p>The ultra-luminous x-ray pulsar (ULXP) NGC 7793 P13 has been regularly monitored with <i>XMM-Newton</i>, <i>NuSTAR</i>, and <i>Swift</i> for the last 8 years. Here, we present the latest results of this monitoring campaign with respect to the pulse period evolution and spectral variability. We find that since the source recovered from an x-ray low state in 2020–2022 the spin-up rate has increased significantly compared with before the off-state, even though the x-ray luminosity has not shown an equivalent increase. We find that the x-ray and optical/UV flux are anti-correlated, and speculate that this variability might be driven by a large accretion disk, precessing at a super-orbital period of 7–8 years. We study the spectral behavior in the <i>XMM-Newton</i> and <i>NuSTAR</i> data, and find very little changes in the spectral shape, despite the large flux variability. This spectral consistency provides further indication that the observed flux variability is a geometric effect and not due to intrinsic changes of the accretion rate.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 1","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-12-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143117877","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":"Exploring Dark Photon Production and Kinetic Mixing Constraints in Heavy-Ion Collisions","authors":"Adrian William Romero Jorge,&nbsp;Elena Bratkovskaya,&nbsp;Taesoo Song,&nbsp;Laura Sagunski","doi":"10.1002/asna.20240132","DOIUrl":"https://doi.org/10.1002/asna.20240132","url":null,"abstract":"&lt;p&gt;Vector &lt;i&gt;U&lt;/i&gt;-bosons, often referred to as “dark photons,” are potential candidates for mediating dark matter interactions. In this study, we outline a procedure to derive theoretical constraints on the upper bound of the kinetic mixing parameter &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;ϵ&lt;/mi&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/msup&gt;\u0000 &lt;mfenced&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;M&lt;/mi&gt;\u0000 &lt;mi&gt;U&lt;/mi&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mfenced&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {upvarepsilon}^2left({M}_Uright) $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; using dilepton data from heavy-ion from SIS to RHIC energies. The analysis is based on the microscopic Parton–Hadron–String Dynamics (PHSD) transport model, which successfully reproduces the measured dilepton spectra in &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;p&lt;/mi&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;mi&gt;p&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ p+p $$&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;mi&gt;p&lt;/mi&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;mi&gt;A&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ p+A $$&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;mi&gt;A&lt;/mi&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;mi&gt;A&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ A+A $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; collisions. Besides the dilepton channels resulting from interactions and decays of Standard Model particles (such as mesons and baryons), we extend the PHSD approach to include the decay of hypothetical &lt;i&gt;U&lt;/i&gt;-bosons into dileptons, &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;U&lt;/mi&gt;\u0000 &lt;mo&gt;→&lt;/mo&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;e&lt;/mi&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;e&lt;/mi&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ Uto {e}^{+}{e}^{-} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;. The production of these &lt;i&gt;U&lt;/i&gt;-bosons occurs via Dalitz decays of pions, &lt;i&gt;η&lt;/i&gt;-mesons, &lt;i&gt;ω&lt;/i&gt;-mesons, Delta resonances, as well as from the decays of vector mesons and &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;K&lt;/mi&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 ","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 3-4","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-12-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.20240132","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144207033","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":"Particle Acceleration in Solar Flares From Radio and Hard X-Ray Spectra","authors":"Adriana Valio,&nbsp;Douglas F. da Silva,&nbsp;Hui Li","doi":"10.1002/asna.20240134","DOIUrl":"https://doi.org/10.1002/asna.20240134","url":null,"abstract":"<div>\u0000 \u0000 <p>For a deeper understanding of the physical processes at play in solar flares, it is necessary to analyze the flare emissions at multiple wavelengths. This multifrequency approach enables the characterization of energetic electrons accelerated from hundreds of keV and up to several tens of MeV. This study reports on the observation of 10 solar flares, in which the spectral parameters were determined for the cm/mm and x-ray bands. The radio spectrum was fitted using gyrosynchrotron emission whereas the hard x-rays fit considered a model of thermal plus nonthermal emission of accelerated electrons. The results show that the spectral indices of the energy distribution of nonthermal electrons emitting in millimeter and hard x-rays do not agree, with the millimeter spectral index being approximately 2 units harder than that of hard x-rays. These findings are consistent with previous research and suggest the existence of a break in the energy spectrum of accelerated electrons. Moreover, for the only flare where photons exceeding 1 MeV were detected, the hard x-ray spectra exhibited a broken power-law where the index of the electron distribution above ~500 keV agreed with the inferred radio spectral index.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 3-4","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-12-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144207029","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":"Accretion Onto Weakly Magnetized Neutron Stars: Polarization Theory and Its Application to X-Ray Burster GX 13+1","authors":"Anna Bobrikova,&nbsp;Sofia V. Forsblom","doi":"10.1002/asna.20240128","DOIUrl":"https://doi.org/10.1002/asna.20240128","url":null,"abstract":"<p>Observations show that the x-ray emission of the accreting weakly magnetized neutron stars (WMNSs) is polarized. In this article, we summarize the analytical models for the polarized emission of various components of the WMNSs. We introduce a missing theoretical model, where we assume the emission comes from the spreading layer, the extension of the boundary layer between the accretion disk and the neutron star. We show how these models and the results of the simulations provide new insights into the x-ray polarization from weakly magnetized neutron stars observed with the imaging x-ray polarimetry explorer (IXPE). We specifically focus on the most peculiar case of the X-ray burster GX 13+1.</p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 1","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-12-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.20240128","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143115699","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":"Semi-Stable Active Region Around the Co-Rotation Latitude of Low-Mass Close Binary KIC 7671594","authors":"N. Ö. Kaya,&nbsp;H. A. Dal","doi":"10.1002/asna.20240115","DOIUrl":"https://doi.org/10.1002/asna.20240115","url":null,"abstract":"<div>\u0000 \u0000 <p>We present the new findings from the light variation of KIC 7671594. We have analyzed the light curve of the system, which is likely a low-mass eclipsing close binary. We have detected a spotted active region migration on the active component. This spotted active region on the stellar surface appears to be stable during the first 2.70 years, but it exhibits rapid migration during the last 0.85 years of the observing season. The OPEA model was derived using 1128 flares and their corresponding parameters. In the model, the <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mtext>Plateau</mtext>\u0000 </mrow>\u0000 <annotation>$$ Plateau $$</annotation>\u0000 </semantics></math> value was found to be 2.46703 ± 0.25234 s, and the <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mtext>half</mtext>\u0000 <mo>−</mo>\u0000 <mtext>life</mtext>\u0000 </mrow>\u0000 <annotation>$$ half- life $$</annotation>\u0000 </semantics></math> was calculated as 7332.28 s. The flare <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>N</mi>\u0000 <mn>1</mn>\u0000 </msub>\u0000 </mrow>\u0000 <annotation>$$ {N}_1 $$</annotation>\u0000 </semantics></math> frequency was determined to be 0.03719 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mi>h</mi>\u0000 <mrow>\u0000 <mo>−</mo>\u0000 <mn>1</mn>\u0000 </mrow>\u0000 </msup>\u0000 </mrow>\u0000 <annotation>$$ {h}^{-1} $$</annotation>\u0000 </semantics></math>, while <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>N</mi>\u0000 <mn>2</mn>\u0000 </msub>\u0000 </mrow>\u0000 <annotation>$$ {N}_2 $$</annotation>\u0000 </semantics></math> was found to be 0.00028. We have concluded that KIC 7671594 is likely a low-mass eclipsing binary system with a main sequence component that possesses an active region covered by some cool spots around its co-rotation latitude.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 9-10","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-12-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143186945","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":"Radial Metallicity Gradients for the Chemically Selected Galactic Thin Disc Main-Sequence Stars","authors":"F. Akbaba,&nbsp;T. Ak,&nbsp;S. Bilir,&nbsp;O. Plevne,&nbsp;Ö. Önal Taş,&nbsp;G. M. Seabroke","doi":"10.1002/asna.20240052","DOIUrl":"https://doi.org/10.1002/asna.20240052","url":null,"abstract":"&lt;div&gt;\u0000 \u0000 &lt;p&gt;We present the radial metallicity gradients within the Galactic thin disc population through main-sequence stars selected on the chemical plane using GALAH DR3 accompanied with &lt;i&gt;Gaia&lt;/i&gt; DR3 astrometric data. The [Fe/H], [&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;α&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ alpha $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;/Fe] and [Mg/H] radial gradients are estimated for guiding radius as &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;0.074&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.006&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ -0.074pm 0.006 $$&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;mo&gt;+&lt;/mo&gt;\u0000 &lt;mn&gt;0.004&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.002&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ +0.004pm 0.002 $$&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;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;0.074&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.006&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ -0.074pm 0.006 $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; dex kpc&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msup&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt; &lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;1&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {}^{-1} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; and for the traceback early orbital radius as &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;0.040&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.002&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ -0.040pm 0.002 $$&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;mo&gt;+&lt;/mo&gt;\u0000 &lt;mn&gt;0.003&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.001&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ +0.003pm 0.001 $$&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;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;0.039&lt;/mn&gt;\u0000 &lt;mo&gt;±&lt;/mo&gt;\u0000 &lt;mn&gt;0.002&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ -0.039pm 0.002 $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; dex kpc&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msup&gt;\u0000 &lt;mrow&gt;\u0000 ","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"345 9-10","pages":""},"PeriodicalIF":1.1,"publicationDate":"2024-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143186450","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}