Astrophysics最新文献

{"title":"Потеря массы атмосферы планеты WASP-193 b","authors":"И. С. Саванов","doi":"10.54503/0571-7132-2023.66.4-497","DOIUrl":"https://doi.org/10.54503/0571-7132-2023.66.4-497","url":null,"abstract":"Представлены результаты анализа проявлений активности звезды WASP-193 спектрального класса F9 с планетой типа супер-нептун. Газовый гигант WASP- 193 b при массе 0.13 массы Юпитера почти в полтора раза больше него по радиусу. Планета имеет низкую плотность p= 0.059 ± 0.014 г/см3 (аналогичным объектом является Kepler 51 d, число других таких экзопланет мало). Равновесная температура атмосферы планеты высока - Teq = 1254±31 К. Полученные результаты изучения активности звезды использованы для оценки потери вещества атмосферы планеты WASP-193 b по аппроксимационной формуле, соответствующей модели потери атмосферы с ограничением по энергии. Оценки величины потока XUVфотонов FXUV были установлены по аналитической зависимости, связывающей FXUV и параметр logRШHK для звезд спектральных классов F - M. Расчеты показали, что потеря вещества атмосферы экзопланеты достаточно велика (даже в случае малой хромосферной активности ее родительской звезды). Диапазон изменений параметра M составляет от 1.8 •10 10 г/с до 4.3 •10 11 г/с в зависимости от принимаемого уровня потока XUV-фотонов (высокая и низкая активность). Вероятно, что планета интенсивно теряет свою атмосферу. WASP-193 b можно рассматривать в качестве высокоприоритетного кандидата для наблюдений с помощью космических миссий (метрика трансмиссионной спектроскопии TSM для объекта составляет около 600).\u0000The results of the analysis of the activity manifestations of the star WASP-193 with spectral class F9 with a super-neptune-type planet are presented. The gas giant WASP-193 b with a mass of 0.13 Jupiter's mass is almost one and a half times Jupiter's radius. The planet has a low density of p= 0.059 ± 0.014 g/cm3 (a similar object is Kepler 51 d, the number of other exoplanets of this type is small). The equilibrium temperature of the planet's atmosphere is high - Teq = 1254 ± 31 K. The obtained results of investigations of the activity of the star were used to estimate the mass loss from the atmosphere of the planet WASP-193 b using an approximation formula corresponding to the energy-limited model. The flux of XUV photons were established by the analytical relation linking FXUV and logR'HK parameter for stars of spectral classes F - M. Calculations have shown that the mass loss from the exoplanet atmosphere is quite large (even in the case of low chromospheric activity of the star). The range of the parameter M is from 1.8 •1010 g/s to 4.3•1011 g/s, depending on the received level of the flux of XUV photons (high and low activity). It is likely that the planet is intensively losing its atmosphere. WASP-193 b can be considered as a high-priority candidate for observations using JWST space mission (the transmission spectroscopy metric TSM for the object is about 600).","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2024-06-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141344399","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":"Новые \"планетарные следы\" темной вселенной","authors":"K. Zioutas, V. Anastassopoulos, A. Argiriou, G. Cantatore, S. Cetin, A. Gardikiotis, H. Haralambous, M. Karuza, A. Kryemadhi, M. Maroudas, A. Mastronikolis, C. Oikonomou, K. Ozbozduman, Y. K. Semertzidis, M. Tsagri, I. Tsagris","doi":"10.54503/0571-7132-2023.66.4-591","DOIUrl":"https://doi.org/10.54503/0571-7132-2023.66.4-591","url":null,"abstract":"\"Dunkle Materie\" (DM) came from unexpected cosmological observations. Nowadays within our solar system, diverse observations also defy conventional explanations, like the main physical process(es) underlying the heating of the different solar atmospheric layers. Streaming DM offers a viable common scenario following gravitational focusing by the solar system bodies. This fits as the underlying process behind the solar cycle, which was the first signature suggesting a planetary dependency. The challenge, since 1859, is to find a remote planetary impact, beyond the extremely feeble planetary tidal force. We stress the possible involvement of an external impact by some overlooked \"streaming invisible matter\", which reconciles all investigated mysterious observations mimicking a not extant remote planetary force. Unexpected planetary relationships exist for both the dynamic Sun and Earth, reflecting multiple signatures for streaming DM. The local reasoning à la Zwicky is also suggestive for searches including puzzling biomedical phenomena. Favourite DM candidates are anti-quark-nuggets, magnetic monopoles, dark photons, or the composite \"pearls\". Then, anomalies within the solar system are the manifestation of the dark Universe. The tentative streaming DM scenario enhances spatiotemporally the DM flux favouring conditions for direct DM detection or extracting energy from the not-so-invisible as anticipated dark sector.\u0000Понятие темной материи (DM) введено для объяснения неожиданных результатов космологических наблюдений. В настоящее время разные явления, наблюдаемые в нашей солнечной системе, также не поддаются традиционным объяснениям, например, основные физические процессы, лежащие в основе нагрева различных слоев солнечной атмосферы. Концепция потоков DM с их последующей гравитационной фокусировкой телами Солнечной системы предлагает жизнеспособный общий сценарий для понимания таких явлений. Возможно это основной процесс, ответственный за солнечные циклы, у которых были обнаружены первыe признаки зависимости от параметров планет. Уже в 1859г. была поставлена задача найти удаленное планетарное воздействие, отличное от чрезвычайно слабой планетарной приливной силы. Мы подчеркиваем возможную причастность внешнего воздействия неучтенного \"потока невидимой материи\", что согласуется со всеми загадочными наблюдениями, ранее исследованными с привлeчением несуществующей удаленной планетарной силы. Множество следов \"потоковой\" ТМ проявляются в разного рода неожиданных связах, как динамического Солнца, так и и Земли. В частности, рассуждение в духе Цвикки наводит на размышления о поиске загадочных биомедицинских явлений. Предпочтительными носителями ТМ являются - крупицы антикварковой материи, магнитные монополи, темные фотоны или составные \"жемчужины\". Таким образом, аномалии внутри Солнечной системы являются проявлениями темной Вселенной. Неявный сценарий потока темной материи расширяет пространственно- временное распределение темной материи, создавая лучши","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2024-06-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141342508","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":null,"pages":null},"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":"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":null,"pages":null},"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":"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":null,"pages":null},"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}

{"title":"Physical Acceptability of the Renyi Holographic Dark Energy Model Under the Hubble's Cutoff in f (T, B) Gravity","authors":"N. T. Karte,&nbsp;Kaplana Pawar,&nbsp;A. K. Dabre","doi":"10.1007/s10511-024-09820-7","DOIUrl":"10.1007/s10511-024-09820-7","url":null,"abstract":"<p>The paper deals with the investigations of the behaviour and physical acceptability of the spatially homogeneous and isotropic FLRW space-time filled with pressureless matter and Rényi holographic dark energy under the Hubble's IR-cutoff in the framework of f (T, B) gravity. We have calculated some cosmological parameters to study the astrophysical consequences of the constructed model. We discussed their behaviour during the cosmic evolution, in particular, the statefinder and EoS parameters. It is found that the constructed Rényi holographic dark energy model travels from Phantom, ΛCDM, and lastly enters &amp; remains in Quintessence dark energy era with the increase in redshift.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.6,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141062302","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 Digitized First Byurakan Survey Database Late-Type Stars Candidates. New Confirmations. II","authors":"K. K. Gigoyan,&nbsp;K. S. Gigoyan,&nbsp;A. Sarkissian,&nbsp;M. Meftah,&nbsp;S. Bekki,&nbsp;E. Karapetyan,&nbsp;F. Rahmatullaeva,&nbsp;G. R. Kostandyan","doi":"10.1007/s10511-024-09817-2","DOIUrl":"10.1007/s10511-024-09817-2","url":null,"abstract":"<p>Three new carbon C stars was confirmed among the sample of the Late-Type Stars candidates, selected on the Digitized First Byurakan Survey (DFBS) spectral plates. The DFBS is the digitized version of the First Byurakan Survey (FBS, or Markarian survey). The FBS was the first systematic survey of the extragalactic sky. This objective-prism survey was carried out in 1965-1980 by B.E.Markarian and his colleagues using the 1 m Schmidt telescope of the Byurakan Astrophysical Observatory and resulted in discovery of 1517 UV-excess (Markarian) galaxies. FBS spectral plates have been used long period to search and study faint LTS (C-type and M-type stars) at high Galactic latitudes. In this work we present Gaia DR3 photometric data, spectra, light curves, distances, high above/below Galactic plane, radial velocities (RV), and other important physical characteristics from the modern astronomical catalogues for three new confirmed DFBS C stars. The confirmation is based on Gaia DR3 BP/RP low-resolution spectral database. In our previous studies of the DFBS plates, these objects were presented as LTS candidates. One of the new confirmed objects is N-type C star, which is a Mira-type variable. Two remaining objects, are early CH-type giants at high Galactic latitudes. Most probably they present binary systems.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.6,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141064126","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 Flat Spectrum Radio Quasars 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/s10511-024-09811-8","DOIUrl":"10.1007/s10511-024-09811-8","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 Flat Spectrum Radio Quasars (FSRQ) candidates, designated in the catalogue as BZQ 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 1909 BZQ objects, 618 having SDSS spectra were classified, resulting in 445 broad-line QSOs, 19 narrow-line QSOs, 138 broad-line Seyferts, 8 narrow-line Seyferts, and 2 Emission-line galaxies without a proper classification. We have calculated the absolute magnitudes and luminosities for all objects to distinguish QSOs from Seyferts, as defined by the Catalogue of QSOs and Active Galaxies, -22^m.25 separation limit. This way 148 objects changed their BZCAT subtypes between BZQ to BZG, and also 6 BZQ objects to BZU.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.6,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141062256","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":"Dust Ion Acoustic Solitary Waves in Plasma with Cairns Distributed Electrons and New Classical Distribution of Ions","authors":"B. C. Kalita,&nbsp;R. Kalita,&nbsp;S. Das","doi":"10.1007/s10511-024-09819-0","DOIUrl":"10.1007/s10511-024-09819-0","url":null,"abstract":"<p>In this composition of plasma with negative dust charge, new classical distribution of nonthermal ions and Cairns distributed electrons, both supersonic and subsonic only rarefactive solitons are found to exist. It appears to conclude that the solitons cease to exist at the increase of <i>c</i>. The supersonic (<i>M</i> = 1.4) rarefactive solitons considerably and concavely increase from small amplitude with the increase of the ion to dust density ratio <i>Q</i> for various values of temperature α . The concave but increasing growth of amplitude of the rarefactive solitons for all <i>M</i> (&gt;1) exhibits its distinct character. Smaller the Mach number (e.g., for <i>M</i> = 1.2), smaller is the amplitude of the solitons throughout the range of <i>v</i>₀ (ion drift). The amplitudes of the rarefactive supersonic solitons are found to increase at the increase of the nonthermal parameter β for all <i>r</i> ( =<i>n</i>_<i>e</i>0 /<i>n</i>_<i>i</i>0 ). The dynamical scenario of this model indicates that the mass of the dusts should decrease in the plasma to generate higher amplitude solitons.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.6,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141064067","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":"Mass Loss from the Atmosphere of the Planet TOI-1442 c","authors":"E. S. Dmitrienko,&nbsp;I. S. Savanov","doi":"10.1007/s10511-024-09816-3","DOIUrl":"10.1007/s10511-024-09816-3","url":null,"abstract":"<p>The properties of the planetary system TOI-1422, in which two planets of a neptune type orbit around a low-activity star of solar type with an age of about 5 billion years, are examined. We have previously analyzed activity of the star TOI-1422, found indications of the existence of possible activity cycles, and considered estimates of the orbital rotation period <i>P</i> of the star. The inner planet TOI-1422 b belongs to the hot-neptune types; it rotates with an orbit of period about 13 days and has an equilibrium temperature of <i>Teq,b</i> = 867 <i>K</i>. Calculations using a model of atmospheric loss with an energy limit for TOI-1422 b yielded 9.4·10⁸ g/s of matter from the atmosphere. The outer planet of the system TOI-1422 c can also be regarded as a hot neptune; it has an orbital period of 29.3 days, its minimal mass, <i>Mc</i> sin<i>i</i>, is 11.1M _⊕ , and the equilibrium temperature is <i>Teq</i>,<i>c</i> = 661 <i>K</i>. For estimating the radius of TOI-1422 <i>c</i> we have used an empirical M-R relation. It was found that the loss of matter from the atmosphere of the planet TOI-1422 <i>c</i> is 7.8·10⁷ g/s and, given the error in the parameters, it may lie within a range from 6.1·10⁷ g/s to 9.7·10⁷ g/s.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.6,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140963965","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}