Astronomische Nachrichten最新文献

{"title":"Searching for Rotational X-Ray Modulation on TIC 277539431","authors":"Desmond Dsouza,&nbsp;Katja Poppenhäger,&nbsp;Ekaterina Ilin","doi":"10.1002/asna.70085","DOIUrl":"https://doi.org/10.1002/asna.70085","url":null,"abstract":"<p>TIC 277539431, a fast rotating M7 dwarf, was detected to host the highest latitude flare to date at <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mn>81</mn>\u0000 <mo>°</mo>\u0000 </msup>\u0000 </mrow>\u0000 <annotation>$$ {81}^{{}^{circ}} $$</annotation>\u0000 </semantics></math>. Magnetic activity like stellar flares occurring at high latitude indicate occurrence of coronal loops at these latitudes on fully-convective M dwarfs. In contrast, sunspots usually occur below <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mn>30</mn>\u0000 <mo>°</mo>\u0000 </msup>\u0000 </mrow>\u0000 <annotation>$$ {30}^{{}^{circ}} $$</annotation>\u0000 </semantics></math>. In our study we look for modulation on the X-ray signal occurring due to occultation of coronal loops by the star due to stellar rotation. We report an updated rotation period for this star as <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>P</mi>\u0000 <mi>rot</mi>\u0000 </msub>\u0000 <mo>=</mo>\u0000 <mn>273.593</mn>\u0000 </mrow>\u0000 <annotation>$$ {P}_{mathrm{rot}}=273.593 $$</annotation>\u0000 </semantics></math> min based on TESS sectors 12, 37, 39, 64 and 65. We conducted <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msubsup>\u0000 <mi>χ</mi>\u0000 <mi>red</mi>\u0000 <mn>2</mn>\u0000 </msubsup>\u0000 </mrow>\u0000 <annotation>$$ {chi}_{mathrm{red}}^2 $$</annotation>\u0000 </semantics></math> fits by varying the amplitude and the phase of a sinusoidally modulated signal derived from the new rotation period. We find no evidence of rotational modulation in the X-ray signal. This could be due to multiple scenarios, such as lack of a stable coronal loop during observation or the modulated signal being too weak, however given the dataset, individual scenarios cannot be distinguished.</p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 3","pages":""},"PeriodicalIF":1.0,"publicationDate":"2026-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70085","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147562790","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. 03/2026","authors":"","doi":"10.1002/asna.70091","DOIUrl":"https://doi.org/10.1002/asna.70091","url":null,"abstract":"","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 3","pages":""},"PeriodicalIF":1.0,"publicationDate":"2026-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70091","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147564207","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":"The Bochum Survey of the Southern Galactic Disk: III. Complete Data Release","authors":"Julia Blex,&nbsp;Moritz Hackstein,&nbsp;Christian Westhues,&nbsp;Michael Ramolla,&nbsp;Markus Demleitner,&nbsp;Dominik J. Bomans,&nbsp;Kerstin Weis,&nbsp;Christofer Fein,&nbsp;Rolf Chini","doi":"10.1002/asna.70087","DOIUrl":"https://doi.org/10.1002/asna.70087","url":null,"abstract":"&lt;p&gt;The Southern Galactic Disk Survey (GDS) monitored a mosaic of 268 fields along a &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msup&gt;\u0000 &lt;mn&gt;6&lt;/mn&gt;\u0000 &lt;mo&gt;°&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {6}^{{}^{circ}} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;-wide stripe in the southern Galactic disk with simultaneous observations in &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;r&lt;/mi&gt;\u0000 &lt;mo&gt;′&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {r}^{prime } $$&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;msup&gt;\u0000 &lt;mi&gt;i&lt;/mi&gt;\u0000 &lt;mo&gt;′&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {i}^{prime } $$&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;msup&gt;\u0000 &lt;mn&gt;7&lt;/mn&gt;\u0000 &lt;mi&gt;m&lt;/mi&gt;\u0000 &lt;/msup&gt;\u0000 &lt;mo&gt;≲&lt;/mo&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;r&lt;/mi&gt;\u0000 &lt;mo&gt;′&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;mo&gt;,&lt;/mo&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;i&lt;/mi&gt;\u0000 &lt;mo&gt;′&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;mo&gt;≲&lt;/mo&gt;\u0000 &lt;msup&gt;\u0000 &lt;mn&gt;18&lt;/mn&gt;\u0000 &lt;mi&gt;m&lt;/mi&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {7}^{mathrm{m}}lesssim {r}^{prime },{i}^{prime}lesssim {18}^{mathrm{m}} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;) from September 2010 to September 2019. The survey design and data characteristics, as well as first results in &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;r&lt;/mi&gt;\u0000 &lt;mo&gt;′&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;mspace&gt;&lt;/mspace&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;i&lt;/mi&gt;\u0000 &lt;mo&gt;′&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {r}^{prime};{i}^{prime } $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;, were presented by Haas et al. (2012; Paper I). Hackstein et al. (2015; Paper II) extended the photometry and analysis process, and introduced the first catalogue including photometry of all 268 fields in &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;mspace&gt;&lt;/mspace&gt;\u0000 &lt;mi&gt;BV&lt;/mi&gt;\u0000 ","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 3","pages":""},"PeriodicalIF":1.0,"publicationDate":"2026-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70087","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147566765","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":"Discovery and Initial Investigation of a New Low Surface Brightness Planetary Nebula Candidate at High Galactic Latitude","authors":"W. E. Celnik,&nbsp;P. Köchling,&nbsp;S. Kotov,&nbsp;J. Kozok,&nbsp;Y. Galata,&nbsp;L. Magrini,&nbsp;A. Moiseev,&nbsp;M. Nischang,&nbsp;C. Reese,&nbsp;P. Remmel,&nbsp;P. Riepe,&nbsp;T. Zilch,&nbsp;K. Werner","doi":"10.1002/asna.70078","DOIUrl":"https://doi.org/10.1002/asna.70078","url":null,"abstract":"<p>Planetary nebulae represent a late evolutionary phase of low- to intermediate-mass stars. In this article, we present the serendipitous discovery of a previously unknown, faint potential Galactic planetary nebula (PN) in the constellation Camelopardalis, identified during a survey-inspection, aiming at the detection of dwarf companions of the spiral galaxy NGC 2403. Narrow-band imaging and spectroscopic observations of the nebula and its potential central star were obtained using a combination of amateur and professional telescopes. Our observations revealed a compact, dense, triangular structure—hereafter referred to as the Triangle Nebula—embedded within a broader elliptical region, which we call the Cam Nebula. Both are enclosed by an even fainter, nearly circular outer shell detectable only in deep, long-exposure images. This Shell Nebula and the Cam Nebula may be superpositions by chance, but we will assume they are connected. We designate the entire complex as TBG-N1. This is the first TBG nebula to avoid confusion with previously discovered TBG-DWs (dwarf galaxies). A candidate for the central star was identified near the geometric centre of the outer shell. Spectroscopic analysis provided estimates of the nebular electron temperature and density. The combined evidence from imaging, spectroscopy, and the photometric properties of the central star candidate supports the classification of TBG-N1 as a planetary nebula located at a distance of approximately 1 kpc. This discovery highlights the important role that collaborations between amateur and professional astronomers can play in uncovering and characterizing previously unrecognized celestial objects.</p>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 3","pages":""},"PeriodicalIF":1.0,"publicationDate":"2026-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70078","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147567557","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":"Bright Spectroscopic Binaries: IV. Additional Binary Systems With \u0000 \u0000 \u0000 P\u0000 <\u0000 1000\u0000 \u0000 $$ P<1000 $$\u0000 Days","authors":"Dennis Jack,&nbsp;Missael Alejandro Hernández Huerta,&nbsp;Faiber Rosas-Portilla,&nbsp;Klaus-Peter Schröder","doi":"10.1002/asna.70076","DOIUrl":"https://doi.org/10.1002/asna.70076","url":null,"abstract":"<div>\u0000 \u0000 <p>In this fourth publication of our series, we present the analysis of a further nine bright spectroscopic binaries (HD 9728, HD 21835, HD 32575, HD 41118, HD 59539, HD 88748, HD 148434, HD 177698, HD 189985) discovered with the TIGRE telescope. We obtained intermediate resolution spectra, which we used to determine the radial velocity variations and then the orbital parameters of the binary systems. The results were compared with Gaia DR3 orbits that are available for some of the binary stars. They are in good agreement, but with our analysis we could improve the orbital solutions and parameters. We further used the spectra to determine the stellar parameters of the primary stars. A comparison with evolution tracks allowed us to obtain an estimate of their masses and ages. All primaries turn out to be evolved, bright K giants, ascending on the RGB, Helium burning, or at the foot of the AGB. We were also able to estimate the minimum masses of the secondary stars. For some cases, we could determine the actual mass of the secondary using the inclinations from the Gaia DR3 non-single stars catalogue. We found that the secondary stars of these systems are all low-mass stars.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 3","pages":""},"PeriodicalIF":1.0,"publicationDate":"2026-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147570251","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 Cosmological Mass Varying Neutrino Model in the Late Universe","authors":"Olga Avsajanishvili","doi":"10.1002/asna.70084","DOIUrl":"https://doi.org/10.1002/asna.70084","url":null,"abstract":"&lt;div&gt;\u0000 \u0000 &lt;p&gt;The cosmological Mass Varying Neutrino (MaVaN) model is considered, where the interaction between a fermionic field and a scalar field with a Ratra–Peebles potential via a Yukawa coupling is investigated. Observational constraints on the flat and non-flat MaVaN models, as well as on the standard &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;ΛCDM&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ Lambda mathrm{CDM} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; model, are derived from 32 &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;(&lt;/mo&gt;\u0000 &lt;mi&gt;z&lt;/mi&gt;\u0000 &lt;mo&gt;)&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ H(z) $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; measurements using MCMC analysis. Comparison with the &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;ΛCDM&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ Lambda mathrm{CDM} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; model using the criteria &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;Δ&lt;/mi&gt;\u0000 &lt;msubsup&gt;\u0000 &lt;mi&gt;χ&lt;/mi&gt;\u0000 &lt;mi&gt;min&lt;/mi&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/msubsup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ Delta {chi}_{mathrm{min}}^2 $$&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;mtext&gt;AICc&lt;/mtext&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ mathrm{AICc} $$&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;BIC&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ mathrm{BIC} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; shows no statistically significant improvement for MaVaN models. Deviations in the expansion history remain well below &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mn&gt;1&lt;/mn&gt;\u0000 &lt;mi&gt;σ&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ 1sigma $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;, indicating that the &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;(&lt;/mo&gt;\u0000 &lt;mi&gt;z&lt;/mi&gt;\u0000 &lt;mo&gt;)&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ H(z) $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; data alone do not provide sufficient constraining power to distinguish MaVaN models from the &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;ΛCDM&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ Lambda m","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 3","pages":""},"PeriodicalIF":1.0,"publicationDate":"2026-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147562694","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. 02/2026","authors":"","doi":"10.1002/asna.70086","DOIUrl":"https://doi.org/10.1002/asna.70086","url":null,"abstract":"","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 2","pages":""},"PeriodicalIF":1.0,"publicationDate":"2026-02-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70086","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146224159","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. 01/2026","authors":"","doi":"10.1002/asna.70075","DOIUrl":"10.1002/asna.70075","url":null,"abstract":"","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.70075","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146049382","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. 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 &amp; 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}

{"title":"Measuring the Precise Photometric Period of the Probable Intermediate Polar 1RXS J014549.6+514314 Based on Extensive Photometry","authors":"V. P. Kozhevnikov","doi":"10.1002/asna.70073","DOIUrl":"https://doi.org/10.1002/asna.70073","url":null,"abstract":"<div>\u0000 \u0000 <p>Recently, in the VSX database, G. Murawski reported the discovery of an oscillation with a period of about 40 min in the probable cataclysmic variable 1RXS J014549.6+514314. To confirm this oscillation and precisely measure its period, I conducted extensive photometry of the object over 25 nights between 2022 and 2024. The total duration of these observations was 139 h. The observations revealed the oscillation on each observation night. This oscillation was coherent throughout all the observations covering 18 months. Due to the large coverage of observations, I was able to determine the oscillation period with high precision. It was found to be <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>41.485867</mn>\u0000 <mo>±</mo>\u0000 <mn>0.000026</mn>\u0000 </mrow>\u0000 <annotation>$$ 41.485867pm 0.000026 $$</annotation>\u0000 </semantics></math> min. The semi-amplitude of the oscillation was large, averaging 0.154(2) mag. The pulse profile of the oscillation did not change during the observations and followed a perfect sinusoidal pattern. With the high precision of the period, I created an ephemeris for the oscillation with a validity time of 30 years. This ephemeris can be used in future studies of changes in the oscillation period. Although short-period X-ray oscillations have not yet been detected in 1RXS J014549.6+514314, the high coherence of its 41-min oscillation suggests that this object is most likely to be an intermediate polar.</p>\u0000 </div>","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"347 2","pages":""},"PeriodicalIF":1.0,"publicationDate":"2025-12-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146224489","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}