Astrophysics最新文献_第10页

Classification of Flat Spectrum Radio Quasars by Optical Activity Types 按光学活动类型对平谱射电类星体进行分类

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-05-17 DOI: 10.1007/s10511-024-09811-8

A. M. Mickaelian, H. V. Abrahamyan, G. M. Paronyan, G. A. Mikayelyan, A. G. Sukiasyan, V. K. Mkrtchyan

引用次数: 0

Dust Ion Acoustic Solitary Waves in Plasma with Cairns Distributed Electrons and New Classical Distribution of Ions 等离子体中的尘埃离子声孤波与凯恩斯电子分布和离子的新经典分布

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-05-17 DOI: 10.1007/s10511-024-09819-0

B. C. Kalita, R. Kalita, S. Das

{"title":"Dust Ion Acoustic Solitary Waves in Plasma with Cairns Distributed Electrons and New Classical Distribution of Ions","authors":"B. C. Kalita, R. Kalita, S. Das","doi":"10.1007/s10511-024-09819-0","DOIUrl":"10.1007/s10511-024-09819-0","url":null,"abstract":"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 c. The supersonic (M = 1.4) rarefactive solitons considerably and concavely increase from small amplitude with the increase of the ion to dust density ratio Q for various values of temperature α . The concave but increasing growth of amplitude of the rarefactive solitons for all M (>1) exhibits its distinct character. Smaller the Mach number (e.g., for M = 1.2), smaller is the amplitude of the solitons throughout the range of v0 (ion drift). The amplitudes of the rarefactive supersonic solitons are found to increase at the increase of the nonthermal parameter β for all r ( =ne0 /ni0 ). The dynamical scenario of this model indicates that the mass of the dusts should decrease in the plasma to generate higher amplitude solitons.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 1","pages":"80 - 92"},"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}

引用次数: 0

Mass Loss from the Atmosphere of the Planet TOI-1442 c 行星 TOI-1442 大气层的质量损失 c

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-05-17 DOI: 10.1007/s10511-024-09816-3

E. S. Dmitrienko, I. S. Savanov

{"title":"Mass Loss from the Atmosphere of the Planet TOI-1442 c","authors":"E. S. Dmitrienko, I. S. Savanov","doi":"10.1007/s10511-024-09816-3","DOIUrl":"10.1007/s10511-024-09816-3","url":null,"abstract":"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 P 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 Teq,b = 867 K. 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, Mc sini, is 11.1M ⊕ , and the equilibrium temperature is Teq,c = 661 K. For estimating the radius of TOI-1422 c we have used an empirical M-R relation. It was found that the loss of matter from the atmosphere of the planet TOI-1422 c 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.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 1","pages":"54 - 59"},"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}

引用次数: 0

Activity of the Star TOI-784 and Loss of Atmospheric Mass by Its Planet 恒星 TOI-784 的活动及其行星大气质量的损失

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-05-17 DOI: 10.1007/s10511-024-09815-4

I. S. Savanov

{"title":"Activity of the Star TOI-784 and Loss of Atmospheric Mass by Its Planet","authors":"I. S. Savanov","doi":"10.1007/s10511-024-09815-4","DOIUrl":"10.1007/s10511-024-09815-4","url":null,"abstract":"The properties of the planetary system TOI-784, in which an earth-like planet orbits a low-activity star of solar type, are examined. Archived V-band measurements of the brightness of TOI-784 in the ASAS 4 data base do not yield reliable indications about the variability of the brightness owing to rotation or about the cyclical long-term variability of this object. A possible estimate of the magnitude of the rotation period of the star is Prot/sini = 41.7 ± 11.4 days. The age of the system according to the empirical gyrochronological relations equals 7.8±3.4 billion years. The average value of the atmospheric activity parameter logR′HK = – 4.99 which corresponds to the level of low-activity stars with analogous (B-V) color index is found and is close to that of the sun. The radius of the planet TOI-784 b is equal to 1.93 R⊕, its mass is 9.67 M⊕, and its average density is 7.4 g/cm3 (the planet is rocky). An estimate of the loss of matter from the atmosphere of the planet TOI-784 b was obtained from an approximate formula corresponding to a model of loss by the atmosphere with a limit on energy. Calculations have shown that the rate of loss of matter by the atmosphere of the planet is 4.7 ⋅ 108 g/s. The relatively low rate of loss of matter by the planet’s atmosphere, despite a high effective temperature of the star’s atmosphere and the closeness of the planet to the star, is probably related to a low level of activity of the star.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"67 1","pages":"48 - 53"},"PeriodicalIF":0.6,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140964639","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}

引用次数: 0

Magnetic Field Structures of Chemically Peculiar Stars. I. HD57682, HD81009 化学奇特恒星的磁场结构。I. HD57682, HD81009

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-05-17 DOI: 10.1007/s10511-024-09813-6

Yu. V. Glagolevskij

引用次数: 0

Induced Electromagnetic Radiation from a Charged Cloud in a Plane Gravitational Wave 平面引力波中带电云团的诱导电磁辐射

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-05-17 DOI: 10.1007/s10511-024-09821-6

V. Epp, K. Osterin

引用次数: 0

Novel Planetary Signatures from the Dark Universe 来自黑暗宇宙的新奇行星信号

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-01-16 DOI: 10.1007/s10511-024-09809-2

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

{"title":"Novel Planetary Signatures from the Dark Universe","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":"10.1007/s10511-024-09809-2","DOIUrl":"10.1007/s10511-024-09809-2","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","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"550 - 558"},"PeriodicalIF":0.6,"publicationDate":"2024-01-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139483377","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}

引用次数: 0

The First Photometric Study of the Binary System CSS J003106.8+313347 首次对双星系统 CSS J003106.8+313347 进行光度研究

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-01-16 DOI: 10.1007/s10511-024-09802-9

E. Paki, S. Baudart, A. Poro

{"title":"The First Photometric Study of the Binary System CSS J003106.8+313347","authors":"E. Paki, S. Baudart, A. Poro","doi":"10.1007/s10511-024-09802-9","DOIUrl":"10.1007/s10511-024-09802-9","url":null,"abstract":"We performed the first photometric study of the CSS J003106.8+313347 W Ursae Majoris (WUMa)-type system based on ground-based observations. We extracted times of minima from our observations and proposed a linear ephemeris based on the increasing incline of the orbital period using a Markov chain Monte Carlo (MCMC) approach. The PHOEBE Python code and the MCMC approach were used for the light curve analysis. This system did not need starspots for the light curve analysis. Mass ratio, fillout factor, and inclination were obtained as 0.699, 0.322, and 60°.6 respectively. We also estimated the absolute parameters of the system using the Gaia DR3 parallax. Therefore, the masses, radii, and luminosities have been determined to be M1 = 1.675, M2 = 1.171, R1 = 1.292, R2 = 1.097, L1 = 1.348, and L2 = 1.221. The orbital angular momentum J0 of the CSS J003106.8+313347 illustrates that this system is located in a region of contact binaries. The positions of the primary and secondary components on the Hertzsprung-Russell (HR) diagram are depicted.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"452 - 462"},"PeriodicalIF":0.6,"publicationDate":"2024-01-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139483422","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}

引用次数: 0

The Digitized First Byurakan Survey Data Base. Late-Type Stars Candidates. New Confirmations. I 数字化的第一次比乌拉坎巡天数据库。晚型恒星候选者。新的确认I

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-01-15 DOI: 10.1007/s10511-024-09804-7

K. S. Gigoyan, K. K. Gigoyan, A. Sarkissian, G. R. Kostandyan, M. Meftah, S. Bekki

{"title":"The Digitized First Byurakan Survey Data Base. Late-Type Stars Candidates. New Confirmations. I","authors":"K. S. Gigoyan, K. K. Gigoyan, A. Sarkissian, G. R. Kostandyan, M. Meftah, S. Bekki","doi":"10.1007/s10511-024-09804-7","DOIUrl":"10.1007/s10511-024-09804-7","url":null,"abstract":"The Digitized First Byurakan Survey (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 UVX-excess (Markarian) galaxies. FBS low-resolution spectral plates have been used for a long time to search and study faint Late-Type Stars (LTS, M-type and C stars) at high Galactic latitudes. A total of 18 lists of the FBS LTS were published between 1990 and 2016. We report newly confirmed C and M giants, and also large amount of M dwarfs based on the Gaia DR3 BP/RP low-resolution spectroscopic data base. Some of the newly confirmed M dwarfs presents binary systems. Some of them are new eclipsing binaries. In our previous studies of the DFBS spectral plates, all were presented as LTS candidates. Gaia high-accuracy astrometric and photometric data and Transiting Exoplanet Survey Satellite (TESS) data are used to characterize these new confirmed LTS. TESS phase-dependent light curves show rotational modulations and flares for many new M dwarfs. This confirmations of the large number of completely new objects represents a very significant extension in the census of M giants, faint N-type Asymptotic Giant Branch C stars, CH-type C giants at high Galactic latitudes, and M dwarfs in the solar vicinity. Some objects are located more than 7 kpc from the Galactic plane. Ultimately, we aim to present value-added catalog and update the FBS LTS catalog. Note that a large amount of the blue stellar objects with UVX-excess and numerous of emission line objects were also detected.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"470 - 484"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139469222","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}

引用次数: 0

Mass Loss from the Atmosphere of the Planet WASP-193 b 行星 WASP-193 b 大气中的质量损失

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-01-15 DOI: 10.1007/s10511-024-09803-8

I. S. Savanov

{"title":"Mass Loss from the Atmosphere of the Planet WASP-193 b","authors":"I. S. Savanov","doi":"10.1007/s10511-024-09803-8","DOIUrl":"10.1007/s10511-024-09803-8","url":null,"abstract":"Results are presented from an analysis of the manifestations of activity of the star WASP-193 of spectral class F9 with a super-neptune-type planet. The gaseous giant WASP-193 b with a mass 0.13 times Jupiter’s mass and almost one and a half times its radius. The planet has a low density ρ = 0.059±0.014 g/cm3 (Kepler 51 d is an analogous object; there are few other exoplanets of this type). The equilibrium temperature of the atmosphere of the planet is high at Teq = 1254±31 K. The results of this study of the star’s activity are used to estimate the loss of matter by the atmosphere of the planet WASP-193 b using an approximation formula corresponding to a model with limited energy. Estimates of the flux of XUV-photons FXUV were made using an analytical relationship relating FXUV and the parameter ({text{log}}{R}_{HK}{prime}) for stars in classes F-M. Calculations showed that the loss of matter from the atmosphere of the exoplanet is quite high (even in the case of a low chromospheric activity of the parent star). The parameter (dot{M}) ranges from 1.8∙1010 g/s to 4.3∙1011 g/s, depending on the assumed level of the flux of XUV-photons (high and low activity). It is probable that the planet is losing its atmosphere intensively. WASP-193 b can be regarded as a high-priority candidate for observations using the JWST space mission (the transmission spectroscopy metric TSM for this object is about 600).","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"463 - 469"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139471102","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}

引用次数: 0