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Структуры магнитного поля химически пекулярных звезд. I. HD 57682, HD81009 化学奇特恒星的磁场结构。I.HD 57682，HD81009

IF 0.5 4区物理与天体物理

Astrophysics Pub Date : 2024-04-08 DOI: 10.54503/0002-3051-2024.77.1-29

Ю. В. Глаголевский

{"title":"Структуры магнитного поля химически пекулярных звезд. I. HD 57682, HD81009","authors":"Ю. В. Глаголевский","doi":"10.54503/0002-3051-2024.77.1-29","DOIUrl":"https://doi.org/10.54503/0002-3051-2024.77.1-29","url":null,"abstract":"На основе литературных данных о величинах магнитного поля построены модели магнитного поля магнитных звезд разных типов пекулярности HD 57682, HD81009 и получены параметры их магнитного поля. У HD 57682, как и у других горячих объектов, обнаруживаются различия физических условий в области магнитных экваторов и в области близ магнитных полюсов, которые пока не поддаются интерпретации. Звезда HD81009 по своим свойствам является типичным представителем магнитных звезд SrCrEu-типа, кроме ее двойственности.\u0000Based on literature data on magnetic field values, models of the magnetic field\u0000of magnetic stars of different types of peculiarity HD57682, HD81009 were\u0000constructed and the parameters of their magnetic field were obtained. HD57682,\u0000like other hot objects, exhibits differences in physical conditions in the region of\u0000the magnetic equators and in the region near the magnetic poles, which are not\u0000yet amenable to interpretation. The star HD81009 in its properties is a typical\u0000representative of SrCrEu-type magnetic stars, except for it's the binar system.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2024-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140728855","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

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分布电子和离子的新经典分布

IF 0.5 4区物理与天体物理

Astrophysics Pub Date : 2024-04-08 DOI: 10.54503/0002-3051-2024.77.1-91

B. 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. Kalita, R. Kalita, S. Das","doi":"10.54503/0002-3051-2024.77.1-91","DOIUrl":"https://doi.org/10.54503/0002-3051-2024.77.1-91","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  . 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 0 (ion drift). The amplitudes of the rarefactive supersonic solitons are found to increase at the increase of the non-thermal parameter  for all r ( 0 0 / e i n n ). The dynamical scenario of this model indicates that the mass of the dusts should decrease in the plasma to generate higher amplitude solitons. В плазме с отрицательным пылевым зарядом с новым классическим распределением нетепловых ионов и электронов с распределением Кэрнса, как сверхзвуковых, так и дозвуковых, существуют только разреженные солитоны. По-видимому, можно сделать вывод, что солитоны перестают существовать при увеличении c. Сверхзвуковые (M = 1.4) разреженные солитоны с малой амплитудой значительно и полого увеличиваются с ростом отношения плотности ионов к плотности пыли Q для различных температур  . Пологый рост амплитуды разреженных солитонов для всех M (>1) имеет свой отчетливый характер. Чем меньше число Маха (например, при М=1.2), тем меньше амплитуда солитонов во всем диапазоне 0 (дрейф ионов). Обнаружено, что амплитуды разреженных сверхзвуковых солитонов растут с увеличением нетеплового параметра  для всех r (  ne0 ni0 ). Динамический сценарий этой модели указывает на то, что масса пыли должна уменьшаться в плазме для генерации солитонов более высокой амплитуды.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2024-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140730661","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

Поперечные градиенты продольного магнитного поля в активных областях с разным уровнем вспышечной продуктивности. II. Статистический анализ 不同闪光产生水平的活动区的纵向磁场横向梯度。II.统计分析

IF 0.5 4区物理与天体物理

Astrophysics Pub Date : 2024-04-08 DOI: 10.54503/0002-3051-2024.77.1-77

Ю. А. Фурсяк

{"title":"Поперечные градиенты продольного магнитного поля в активных областях с разным уровнем вспышечной продуктивности. II. Статистический анализ","authors":"Ю. А. Фурсяк","doi":"10.54503/0002-3051-2024.77.1-77","DOIUrl":"https://doi.org/10.54503/0002-3051-2024.77.1-77","url":null,"abstract":"Работа является частью исследования, посвященного изучению градиентов продольного магнитного поля в активных областях (АО) с разным уровнем вспышечной продуктивности. Выполнен статистический анализ параметров, описывающих поперечную составляющую градиента продольного магнитного поля z B   в АО: средней по области величины поперечной составляющей градиента продольного магнитного поля z B   , средней величины z B   в окрестности точки с максимальным его значением max Bz , максимального значения z B   между парами пятен в АО z sp max ( B )   . Для вычисления обозначенных параметров использованы магнитограммы z B -компоненты вектора магнитного поля на уровне фотосферы Солнца, получаемые инструментом Helioseismic and Magnetic Imager (HMI) на борту Solar Dynamics Observatory (SDO). Статистическая выборка содержит в себе данные о 75 АО. Усредненные за время мониторинга величины анализируемых параметров сопоставлены с уровнем вспышечной продуктивности АО (вспышечным индексом, FI). Показано, что: 1. Зависимость z B   - FI (чертой сверху обозначено усреднение по времени мониторинга АО) квадратичная с коэффициентом корреляции k = 0.54, а разброс значений величины z B   небольшой (для подавляющего большинства исследуемых областей находится в пределах 0.08-0.12 Гс км-1) и крайне мало различается для областей с низкой и высокой вспышечной продуктивностью, что можно объяснить зависимостью величины z B   от площади АО. 2. Зависимость z B  max - FI квазилинейная с коэффициентом корреляции k = 0.61. 3. Зависимость z sp max ( B )   - FI линейная с коэффициентом корреляции k = 0.63. 4. Выявлены пороговые значения анализируемых параметров: для величины B 0.078 z    Гс км-1, для величины max B 0.983 z    Гс км-1, для параметра max ( B ) 0.118 z sp    Гс км-1. При более низких значениях анализируемых параметров ни в одной из областей выборки вспышек рентгеновских классов Х не фиксировалось.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2024-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140729475","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

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":null,"pages":null},"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":null,"pages":null},"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":null,"pages":null},"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":null,"pages":null},"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

Viscous Ricci Dark Energy Cosmological Models in Brans-Dicke Theory 布兰斯-迪克理论中的粘性里奇暗能量宇宙学模型

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-01-15 DOI: 10.1007/s10511-024-09810-9

M. Vijaya Santhi, T. Chinnappalanaidu, S. Srivani Madhu

{"title":"Viscous Ricci Dark Energy Cosmological Models in Brans-Dicke Theory","authors":"M. Vijaya Santhi, T. Chinnappalanaidu, S. Srivani Madhu","doi":"10.1007/s10511-024-09810-9","DOIUrl":"10.1007/s10511-024-09810-9","url":null,"abstract":"The whole article deals with the analysis of the cosmic model of Ruban’s space-time in the context of a bulk viscosity impact in the form of Ricci dark energy within the framework Brans-Dicke theory. We believe that outer space is filled with dark matter and viscous Ricci dark energy (VRDE) under the pressureless situation. The velocity and rate at which the Universe is expanding are presumed to be proportional to the coefficient of total bulk viscosity, is in the form, ({upxi }_{0}+{upxi }_{1}dot{a}/a+{upxi }_{2}ddot{a}/a,) where ({upxi }_{0},{upxi }_{1}) and ({upxi }_{2}) are the constants. To solve the RDE model's field equations, we utilize the relation among the metric potentials and also the power-law relation among the average scale factor a(t) and scalar field ϕ. To examine the evolutionary dynamics of the Universe, we investigate the deceleration parameter q, jerk parameter j, EoS parameter ({upomega }_{de},) Om(z) , stability of the obtained models through the square speed of the sound ({v}_{s}^{2},{upomega }_{de}-{omega }_{de}{prime}) plane, statefinder parameter planes (r, s) and (q, r) and presented via graphical representation. By the end of the discussion, VRDE model was found to be compatible with the present accelerated expansion of the Universe.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139471051","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

Structure of the Magnetic Field of the Star HD133880 (Si) HD133880 星（硅）的磁场结构

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-01-15 DOI: 10.1007/s10511-024-09806-5

Yu. V. Glagolevskij

引用次数: 0

Periodicity of Flare Frequency of Active Flare Stars Detected by Tess 苔丝探测到的活动耀斑恒星的耀斑频率周期性

IF 0.6 4区物理与天体物理

Astrophysics Pub Date : 2024-01-15 DOI: 10.1007/s10511-024-09807-4

A. A. Akopian

{"title":"Periodicity of Flare Frequency of Active Flare Stars Detected by Tess","authors":"A. A. Akopian","doi":"10.1007/s10511-024-09807-4","DOIUrl":"10.1007/s10511-024-09807-4","url":null,"abstract":"Data from the TESS orbital observatory are used to study the most active flare stars indicating 100 or more flares during the period from July 2018 through October 2020. The main objectives of this study were: (a) analysis of the light curves, determination of the axial rotation periods, and identification of physical features in individual stars, (b) determination of the parameters of the periodic/cyclical variability of the flare frequencies of flare stars owing to axial/orbital rotations. The corresponding periods of the flare frequency functions were obtained and compared with the axial rotation periods of the stars. The periods of the frequency functions of the flares turned out to be close to the axial rotation periods of the stars. Theoretical phase distributions of the flares are constructed and compared with analogous observations of the flares for the given period. For all the stars without exception, a comparison with the aid of the χ2 criterion confirms the periodicity of the flare frequency. It is proposed that the distribution of spots over the longitude of flare stars can be represented by an angular von Mises distribution, for which the parameters are determined by the corresponding parameters of the flare frequency function. The binarity of the star CD-56 1032 is discussed in detail.","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139469135","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