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}
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 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.
{"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}
Alexandra Lehtmets, Mihkel Kama, Luca Fossati, Anna Aret
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.
{"title":"Investigating Circumstellar Atomic Radiation-Driven Dynamics","authors":"Alexandra Lehtmets, Mihkel Kama, Luca Fossati, 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}
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.
{"title":"Unveiling the Cosmos: XMM-Newton's Scientific Strategy","authors":"Norbert Schartel, 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}
<p>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 <span></span><math> <semantics> <mrow> <msubsup> <mn>23.069</mn> <mrow> <mo>−</mo> <mn>0.082</mn> </mrow> <mrow> <mo>+</mo> <mn>0.081</mn> </mrow> </msubsup> <mspace></mspace> <mtext>days</mtext> </mrow> <annotation>$$ {23.069}_{-0.082}^{+0.081}kern0.5em mathrm{days} $$</annotation> </semantics></math>, a minimum mass of <span></span><math> <semantics> <mrow> <msubsup> <mn>2.97</mn> <mrow> <mo>−</mo> <mn>0.48</mn> </mrow> <mrow> <mo>+</mo> <mn>0.46</mn> </mrow> </msubsup> <msub> <mi>M</mi> <mo>⊕</mo> </msub> </mrow> <annotation>$$ {2.97}_{-0.48}^{+0.46}{M}_{oplus } $$</annotation> </semantics></math> and an equilibrium temperature of 284 K. We find an additional planet candidate in the RV data with an orbital period of <span></span><math> <semantics> <mrow> <mn>1.736</mn> <mspace></mspace> <msubsup> <mn>15</mn> <mrow> <mo>−</mo> <mn>0.000</mn> <mspace></mspace> <mn>76</mn> </mrow> <mrow> <mo>+</mo> <mn>0.000</mn> <mspace></mspace> <mn>74</mn> </mrow>
{"title":"Confirmation of a Non-Transiting Planet in the Habitable Zone of the Nearby M Dwarf L 98-59","authors":"Paul I. Schwarz, Stefan Dreizler, René Heller","doi":"10.1002/asna.70059","DOIUrl":"https://doi.org/10.1002/asna.70059","url":null,"abstract":"<p>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 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msubsup>\u0000 <mn>23.069</mn>\u0000 <mrow>\u0000 <mo>−</mo>\u0000 <mn>0.082</mn>\u0000 </mrow>\u0000 <mrow>\u0000 <mo>+</mo>\u0000 <mn>0.081</mn>\u0000 </mrow>\u0000 </msubsup>\u0000 <mspace></mspace>\u0000 <mtext>days</mtext>\u0000 </mrow>\u0000 <annotation>$$ {23.069}_{-0.082}^{+0.081}kern0.5em mathrm{days} $$</annotation>\u0000 </semantics></math>, a minimum mass of <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msubsup>\u0000 <mn>2.97</mn>\u0000 <mrow>\u0000 <mo>−</mo>\u0000 <mn>0.48</mn>\u0000 </mrow>\u0000 <mrow>\u0000 <mo>+</mo>\u0000 <mn>0.46</mn>\u0000 </mrow>\u0000 </msubsup>\u0000 <msub>\u0000 <mi>M</mi>\u0000 <mo>⊕</mo>\u0000 </msub>\u0000 </mrow>\u0000 <annotation>$$ {2.97}_{-0.48}^{+0.46}{M}_{oplus } $$</annotation>\u0000 </semantics></math> and an equilibrium temperature of 284 K. We find an additional planet candidate in the RV data with an orbital period of <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>1.736</mn>\u0000 <mspace></mspace>\u0000 <msubsup>\u0000 <mn>15</mn>\u0000 <mrow>\u0000 <mo>−</mo>\u0000 <mn>0.000</mn>\u0000 <mspace></mspace>\u0000 <mn>76</mn>\u0000 </mrow>\u0000 <mrow>\u0000 <mo>+</mo>\u0000 <mn>0.000</mn>\u0000 <mspace></mspace>\u0000 <mn>74</mn>\u0000 </mrow>\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}
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.
{"title":"Commissioning an Inexpensive Off-The-Shelf Spectrograph for Radial-Velocity Studies","authors":"Lukas Stock, 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}
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