Astrophysics最新文献

{"title":"Activity of the Spectral Class K2V Dwarf HD 189733 in a Hot-Jupiter Type Exoplanet","authors":"I. S. Savanov","doi":"10.1007/s10511-024-09824-3","DOIUrl":"10.1007/s10511-024-09824-3","url":null,"abstract":"<p>Results are presented from an analysis of manifestations of the activity of the spectral class K2V dwarf HD189733, which has one of the best studied exoplanets of the hot-Jupiter type. Including the activity of the star makes analysis of the characteristics of the planet considerably more complicated (in particular, cool spots on the star’s surface introduce an additional signal in the relation between the depth of a transit and the size of the planet and prevent an exact determination of the radius of the planet). Photometric data for HD189733 in the archive of the TESS mission are analyzed and conclusions are reached on the values of the rotation period P_rot of the star, for which we estimated values of 12.5 and 11.3 days for sectors 41 and 54, respectively. A comparison of these with previous estimates based on earthbound photometric observations suggests that the differences in P_rot at different times are related to the fact of different observation times spots located at different latitudes on the surface of the differentially rotating star predominated. According to the TESS data the amplitude of the brightness variation of HD189733 is 1.6 and 0.9% of the mean brightness level of the star (for sectors 41 and 54, respectively). The standard method was used to estimate the spottedness parameter of the star (2.0 and 1.2% of the star’s surface area) and values of the area of the spotted surface A of the star in absolute terms (9200 MSH and 5400 MSH for sectors 41 and 54, respectively) were obtained. Based on 771 estimates of the star’s brightness in the V band presented in the Kamogata Wide-field Survey, an analysis was made of the long-term activity of HD189733 which yielded indications of the possible existence of activity cycles of duration 1140 and 4220 days (3.1 and 11.6 years, respectively). Based on an analysis of published data it has been concluded that the level of chromospheric activity of HD189733 exceeds the average values typical of other cool dwarfs with analogous values of the color index (B-V) and is higher than the solar value. It is concluded that HD189733 has a moderate (or somewhat higher than average) activity typical of analogous dwarfs in spectral class K but, nevertheless, requires that the properties and evolution of the planet formed around this star be taken into detailed account during modeling, regardless of whether a simplified method or an exact magnetohydrodynamic model is used to estimate them. It should also be noted that the activity of the star is a variable over time (on a time scale comparable to P_rot) and requires estimates that are made simultaneously with the main studies of the exoplanet’s atmosphere.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 2","pages":"140 - 148"},"PeriodicalIF":0.6,"publicationDate":"2024-07-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141869722","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":"Classification of BLL Blazars by Optical Activity Types","authors":"A. M. Mickaelian,&nbsp;H. V. Abrahamyan,&nbsp;G. M. Paronyan,&nbsp;G. A. Mikayelyan,&nbsp;A. G. Sukiasyan,&nbsp;V. K. Mkrtchyan","doi":"10.1007/s10511-024-09822-5","DOIUrl":"10.1007/s10511-024-09822-5","url":null,"abstract":"<p>We have carried out a spectral classification by the Activity Types for a subsample of Blazars from the BZCAT v.5 Catalogue, namely the BL Lac (BLL, Lacertids) candidates, designated in the Catalogue as BZB subtype objects. The classification is based on the Sloan Digital Sky Survey (SDSS) homogeneous medium-resolution optical spectroscopy and along with the standard BPT-type diagnostic diagrams, we have applied our newly introduced fine classification scheme with subtypes of Quasars and considering many more features. Out of 1151 BZB objects, 552 having SDSS spectra were classified. After new classification, 259 (46.1%) of 552 have not changed their optical class, and 293 (53.1%) of these objects have changed their optical class. Having this new information on the optical classification we suggest to change the classification of some objects in BZCAT: for 130 BZB objects to BZG, for 18 BZB objects to BZQ and for 145 BZB objects to BZU.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 2","pages":"119 - 127"},"PeriodicalIF":0.6,"publicationDate":"2024-07-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141869725","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":"Isospin-Asymmetric Cold Nuclear Matter in the Relativistic Mean-Field Theory with a Scalar-Isovector Interaction Channel","authors":"G. B. Alaverdyan,&nbsp;A. G. Alaverdyan","doi":"10.1007/s10511-024-09829-y","DOIUrl":"10.1007/s10511-024-09829-y","url":null,"abstract":"<p>The properties of isospin-asymmetric cold nuclear matter are studied in terms of the relativistic mean-field theory in which, besides the fields of σ, ω, and ρ mesons, and the isovector, Lorentz-scalar field of the δ-meson is also taken into account. The properties of purely nucleonic <i>np</i> matter are studied as a function of the baryon density <i>n</i>_<i>B</i> and the asymmetry parameter α, as well as the properties of electrically neutral β-equilibrium <i>npe</i> μ matter as a function of the baryon density <i>n</i>_<i>B</i><i>.</i> For different values of <i>n</i>_<i>B</i> and a, such characteristics of <i>np</i> matter as the energy per baryon, the specific energy owing to isospin asymmetry, the effective proton and neutron masses, and the specific binding energy, are determined. It is shown that the energy owing to the asymmetry for a fixed value of α is a monotonically increasing function of the baryon density <i>n</i>_<i>B</i>. For <i>npe</i>m matter, the effective proton and neutron masses <span>({M}_{p}^{left(effright)},{M}_{n}^{left(effright)},)</span> the specific binding energy <i>E</i>_<i>bind</i>, the symmetry energy <i>E</i>_<i>sym</i>, the quantitative fraction of protons <i>Y</i>_<i>p</i> = <i>n</i>_<i>p</i>/<i>n</i>_<i>B</i> are studied, as well as the average meson fields <span>(widetilde{upsigma },widetilde{upomega },widetilde{updelta },)</span> and <span>(widetilde{uprho })</span> as functions of the baryon density <i>n</i>_<i>B</i><i>.</i></p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 2","pages":"215 - 230"},"PeriodicalIF":0.6,"publicationDate":"2024-07-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141869721","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":"Reconstruction of the Quintessence Dark Energy Potential from a Gaussian Process","authors":"E. Elizalde,&nbsp;M. Khurshudyan,&nbsp;K. Myrzakulov,&nbsp;S. Bekov","doi":"10.1007/s10511-024-09828-z","DOIUrl":"10.1007/s10511-024-09828-z","url":null,"abstract":"<p>This paper presents the reconstruction of the quintessence dark energy potential in a model- independent way. Reconstruction relies on a Gaussian process and on available expansion rate data. Specifically, 40-point values of H(z) are used, consisting of a 30-point sample deduced from a differential age method and an additional 10-point sample obtained from the radial BAO method. Results are obtained for two kernel functions and for three different values of H₀. This sheds light on the H₀ tension problem indicating that it is not just a numerical problem. The model-independent reconstruction of the potential can serve as a reference to constraint available models and construct new ones. Various possibilities, including V(ϕ) ~ e^-λϕ , are compared with the reconstructions here obtained, which is notably the first truly model-independent reconstruction of the quintessence dark energy potential. This allows the selection of new models that can be interesting for cosmology. The method can be extended to reconstruct the potential of related dark energy models, to be considered in future work.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 2","pages":"192 - 214"},"PeriodicalIF":0.6,"publicationDate":"2024-07-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141869716","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":"Electromagnetic Properties of Stellar Matter. I. Dielectric Permeability of a Hot Rarefied Plasma with Abundant Production of Electron-Positron Pairs","authors":"G. S. Hajyan,&nbsp;A. S. Harutyunyan","doi":"10.1007/s10511-024-09827-0","DOIUrl":"10.1007/s10511-024-09827-0","url":null,"abstract":"<p>The Vlasov equations are used to determine the transverse and longitudinal dielectric permeabilities of a hot, rarefied ultrarelativistic electron-positron plasma. The Fermi distribution is used as the unperturbed distribution function of the electrons and positrons. It is shown that, owing to the abundant production of electron-positron pairs, the plasma frequency of the ultrarelativistic plasma increases linearly with rising temperature. Here the ratio of the frequency at which the spectral density of the equilibrium emission is maximal to the plasma frequency remains fixed and equals 28. It is shown that in this sort of plasma, in particular in the matter of the early universe in the ultrarelativistic electronpositron epoch, the spectrum of the radiation differs very little from black-body radiation.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 2","pages":"178 - 191"},"PeriodicalIF":0.6,"publicationDate":"2024-07-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141869718","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 Study of the Asynchronous Polar IGR J19552+0044 in 2019-2022","authors":"Ju. V. Babina,&nbsp;E. P. Pavlenko,&nbsp;N. V. Pit,&nbsp;K. A. Antonyuk,&nbsp;A. A. Sosnovskij,&nbsp;V. G. Godunova,&nbsp;I. A. Izviekova,&nbsp;G. I. Kokhirova,&nbsp;F. D. Rakhmatullaeva,&nbsp;A. O. Simon,&nbsp;M. V. Chupira","doi":"10.1007/s10511-024-09825-2","DOIUrl":"10.1007/s10511-024-09825-2","url":null,"abstract":"<p>This paper is an analysis of data from multicolor photometric observations of the asynchronous polar IGR J19552+0044 obtained over 59 nights from 2019-2022 at the Crimean Astrophysical Observatory, as well as at the Terskol Peak, Sanglokh, and Lesniki Observatories, and data from the TESS space telescope obtained on 27 days in 2022. It is shown that the maximum amplitude of the brightness oscillations at the rotation period of the white dwarf (~2^m.5-3^m) is observed in the Ic band and is essentially close to zero in the B band. The rotation period of the white dwarf is refined to 0.05645350(14) days. A dependence of the amplitude of the brightness curve of the rotation period on the phase of the synodic period is detected.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 2","pages":"149 - 160"},"PeriodicalIF":0.6,"publicationDate":"2024-07-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141869717","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":"BSN: First Light Curve Study of the Low Mass Contact Binary V0610 Vir","authors":"A. Alizadehsabegh,&nbsp;F. Lomoz,&nbsp;A. Poro,&nbsp;A. Narimani","doi":"10.1007/s10511-024-09823-4","DOIUrl":"10.1007/s10511-024-09823-4","url":null,"abstract":"<p>Photometric data were used to perform the first light curve analysis of the V0610 Vir binary system. Observations and analysis were done in the form of the Binary Systems of South and North (BSN) Project. We extracted the minima from our observations and compiled the literature, which was few. Therefore, we performed computations using the reference ephemeris and presented a new ephemeris and O-C diagram with a linear fit. Light curve analysis was performed using the PHOEBE Python code and the Markov chain Monte Carlo (MCMC) approach. The assumption of a hot starspot was required due to the asymmetry in the light curve’s maxima. The analysis shows that V0610 Vir is a contact binary system with a fillout factor of 0.085, a mass ratio of 0.998, and an inclination of 70°.65. The absolute parameters of the system were estimated based on the Gaia DR3 parallax method. The results show that the system is a low-mass contact binary with a total mass lower than 0.8 M_⨀. The location of the stars was shown in the M - L and M - R diagrams.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 2","pages":"128 - 139"},"PeriodicalIF":0.6,"publicationDate":"2024-07-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141869720","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":"Transverse Gradients of Longitudinal Magnetic Field in Active Regions with Different Levels of Flare Productivity. II. Statistical Analysis","authors":"Yu. A. Fursyak","doi":"10.1007/s10511-024-09818-1","DOIUrl":"10.1007/s10511-024-09818-1","url":null,"abstract":"<p>Here, we performed a statistical analysis of the parameters describing the transverse component of the longitudinal magnetic field gradient (∇ _⊥ <b><i>B </i></b>_<i>z</i> ) in the active regions of the AR – the AR-averaged transverse component of the longitudinal magnetic field gradient &lt;∇ _⊥ <b><i>B z</i></b> &gt;, the average transverse component of the longitudinal magnetic field gradient in the vicinity of a point with its maximum value &lt;max∇ _⊥ <b><i>B z</i></b> &gt;, the maximum value of the transverse component of the longitudinal magnetic field gradient between pairs of spots in the AR max(∇ _⊥ <b><i>B </i></b>_<i>z</i> ) _<i>sp</i> . For calculating the denoted parameters, magnetograms of the <b><i>B</i></b> _z -components of the magnetic field vector at the level of the Sun’s photosphere obtained by the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) are used. The statistical sample contains data on 75 ARs. The values of the analyzed parameters obtained over the time of monitoring are compared with the level of flare productivity of the AR (the flare index FI). It is shown that: 1. The <span>(langle overline{{nabla }_{perp }{{varvec{B}}}_{z}}rangle )</span> -FI dependence (the overhead line denotes averaging over the time of monitoring the AR) is quadratic with a correlation coefficient k = 0.54 while the spread in values of the quantity <span>(langle overline{{nabla }_{perp }{{varvec{B}}}_{z}}rangle )</span> is small (lying within a a range of 0.08-0.12 G km^-1 for the overwhelming majority of the studied regions) and differs very little for regions with low and high flare productivity, which may be explained by the dependence of ∇ _⊥ <b><i>B </i></b>_<i>z</i> on the area of the AR. 2. The dependence <span>(langle overline{{text{max}}{nabla }_{perp }{{varvec{B}}}_{z}}rangle )</span> -FI is quasilinear with a correlation coefficient k = 0.61. 3. The dependence <span>(overline{{text{max}}{nabla }_{perp }{{varvec{B}}}_{z}})</span> -FI is linear with a correlation coefficient k = 0.63. 4. The threshold values of the analyzed parameters are found: for <span>(langle overline{{nabla }_{perp }{{varvec{B}}}_{z}}rangle )</span> ≥ 0.078 G km^-1, for <span>(langle overline{{text{max}}{nabla }_{perp }{{varvec{B}}}_{z}}rangle )</span> ≥ 0.983 G km^-1, and for the parameter max(∇ _⊥ <b><i>B </i></b>_<i>z</i>) _<i>sp</i> ≥ 0.118G km^-1. For lower values of the analyzed parameters, no x-ray flares were recorded in any of the ARs of the analyzed sample.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 1","pages":"67 - 79"},"PeriodicalIF":0.6,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140964523","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 Spectral Studies of a Group of Wolf-Rayet Galactic Stars. II. WC and WO Sequences","authors":"L. N. Kondratyeva,&nbsp;I. V. Reva,&nbsp;E. K. Denissyuk,&nbsp;S. A. Shomshekova,&nbsp;A. K. Aimanova","doi":"10.1007/s10511-024-09812-7","DOIUrl":"10.1007/s10511-024-09812-7","url":null,"abstract":"<p>Photometric and spectral observations of 7 stars in the WC and WO sequences were made at the Fesenkov Astrophysical Institute in 2021-2022. These observations served as the basis of estimates of the brightness of the objects in BVRc filters and the absolute fluxes of radiation in the emission lines. Changes in the brightness of WR 121 over the limits of 0^m.1-0^m.15 were recorded. Changes in the fluxes of emission lines were detected in the spectra of several of the objects, WR 4, WR 5, WR 121, and WR 128.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 1","pages":"9 - 23"},"PeriodicalIF":0.6,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140964945","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":"Magnetic Field Structures of Chemically Peculiar Stars. II. HD98088, HD182180, HD221218, HD318107","authors":"Yu. V. Glagolevskij","doi":"10.1007/s10511-024-09814-5","DOIUrl":"10.1007/s10511-024-09814-5","url":null,"abstract":"<p>Based on published data on the magnitudes of the magnetic field, models are constructed of several magnetic stars of different types of peculiarity and the parameters of the magnetic field are obtained. Among the hot objects, differences are also discovered in the physical conditions in the regions of the magnetic equators and in the region near the magnetic poles, which are not yet amenable to interpretation.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 1","pages":"35 - 47"},"PeriodicalIF":0.6,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141062255","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}